Testing 2D temperature models in Bayesian retrievals of atmospheric properties from hot Jupiter phase curves [EPA]

http://arxiv.org/abs/2305.10249


Spectroscopic phase curves of transiting hot Jupiters are spectral measurements at multiple orbital phases, giving a set of disc-averaged spectra that probe multiple hemispheres. By fitting model phase curves to observations, we can constrain the atmospheric properties of hot Jupiters such as molecular abundance, aerosol distribution and thermal structure, which offer insights into their dynamics, chemistry, and formation. In this work, we propose a novel 2D temperature scheme consisting of a dayside and a nightside to retrieve information from near-infrared phase curves, and apply the scheme to phase curves of WASP-43b observed by HST/WFC3 and Spitzer/IRAC. In our scheme, temperature is constant on isobars on the nightside and varies with cos$^n$(longitude/$\epsilon$) on isobars on the dayside, where $n$ and $\epsilon$ are free parameters. We fit all orbital phases simultaneously using the radiative transfer code NEMESISPY coupled to a Bayesian inference code. We first validate the performance of our retrieval scheme with synthetic phase curves generated from a GCM, and find our 2D scheme can accurately retrieve the latitudinally-averaged thermal structure and constrain the abundance of H$_2$O and CH$_4$. We then apply our 2D scheme to the observed phase curves of WASP-43b and find: (1) the dayside temperature-pressure profiles do not vary strongly with longitude and are non-inverted; (2) the retrieved nightside temperatures are extremely low, suggesting significant nightside cloud coverage; (3) the H$_2$O volume mixing ratio is constrained to $5.6\times10^{-5}$–$4.0\times10^{-4}$, and we retrieve an upper bound for CH$_4$ at $\sim$10$^{-6}$.

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J. Yang, P. Irwin and J. Barstow
Thu, 18 May 23
49/67

Comments: 16 pages. 14 figures. Submitted to MNRAS. Comments welcome!

Effects of the Hunga Tonga-Hunga Ha'apai Volcanic Eruption on Observations at Paranal Observatory [IMA]

http://arxiv.org/abs/2305.08620


The Hunga Tonga-Hunga Ha’apai volcano erupted on 15 January 2022 with an energy equivalent to around 61 megatons of TNT. The explosion was bigger than any other volcanic eruption so far in the 21st century. Huge quantities of particles, including dust and water vapour, were released into the atmosphere. We present the results of a preliminary study of the effects of the explosion on observations taken at Paranal Observatory using a range of instruments. These effects were not immediately transitory in nature, and a year later stunning sunsets are still being seen at Paranal.

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R. Rosa, A. Otarola, T. Szeifert, et. al.
Tue, 16 May 23
29/83

Comments: 4 pages, 5 figures, published in ESO Messenger vol. 190

The pure-rotational and rotational-vibrational Raman spectrum of the atmosphere at an altitude of 23 km [IMA]

http://arxiv.org/abs/2304.13747


Ground-based optical astronomical observations supported by or in the vicinity of laser guide-star systems can be contaminated by Raman-scattered laser photons. Anticipating, alleviating, and correcting for the impact of this self-inflicted contamination requires a detailed knowledge of the pure-rotational and rotational-vibrational spectrum of the molecules in our atmosphere. We present a 15.3hr-deep combined spectrum of the 4LGSF’s 589nm $\approx$ 509THz sodium laser beams of Paranal observatory, acquired with the ESPRESSO spectrograph at a resolution $\lambda/\Delta\lambda\cong140’000\approx0.12$ cm$^{-1}$ and an altitude of 23 km above mean sea level. We identify 865 Raman lines over the spectral range of [3770; 7900]{\AA}$\approx$[+9540; -4315] cm$^{-1}$, with relative intensities spanning ~5 orders of magnitudes. These lines are associated to the most abundant molecules of dry air, including their isotopes: 14N14N, 14N15N, 16O16O, 16O17O, 16O18O, and 12C16O16O. The signal-to-noise of these observations implies that professional observatories can treat the resulting catalogue of Raman lines as exhaustive (for the detected molecules, over the observed Raman shift range) for the purpose of predicting/correcting/exploiting Raman lines in astronomical data.
Our observations also reveal that the four laser units of the 4LGSF do not all lase at the same central wavelength. […] The [measured] offsets […] are larger than the observed 4LGSF spectral stability of $\pm$3 MHz over hours. They remain well within the operational requirements for creating artificial laser guide-stars, but hinder the assessment of the radial velocity accuracy of ESPRESSO at the required level of 10 m/s. Altogether, our observations demonstrate how Raman lines can be exploited by professional observatories as highly-accurate, on-sky wavelength references.

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F. Vogt, A. Mehner, P. Figueira, et. al.
Fri, 28 Apr 23
35/68

Comments: 33 pages incl. appendices, 10 figures, 5 tables. Accepted for publication in Physical Review Research

Avoiding methane emission rate underestimates when using the divergence method [CL]

http://arxiv.org/abs/2304.10303


Methane is a powerful greenhouse gas, and a primary target for mitigating climate change in the short-term future due to its relatively short atmospheric lifetime and greater ability to trap heat in Earth’s atmosphere compared to carbon dioxide. Top-down observations of atmospheric methane are possible via drone and aircraft surveys as well as satellites such as the TROPOspheric Monitoring Instrument (TROPOMI). Recent work has begun to apply the divergence method to produce regional methane emission rate estimates. Here we show that spatially incomplete observations of methane can produce negatively biased time-averaged regional emission rate estimates via the divergence method, but that this effect can be counteracted by adopting a procedure in which daily advective fluxes of methane are time-averaged before the divergence method is applied. Using such a procedure with TROPOMI methane observations, we calculate yearly Permian emission rates of 3.1, 2.4 and 2.7 million tonnes per year for the years 2019 through 2021. We also show that highly-resolved plumes of methane can have negatively biased estimated emission rates by the divergence method due to the presence of turbulent diffusion in the plume, but this is unlikely to affect regional methane emission budgets constructed from TROPOMI observations of methane. The results from this work are expected to provide useful guidance for future implementations of the divergence method for emission rate estimation from satellite data – be it for methane or other gaseous species in the atmosphere.

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C. Roberts, R. IJzermans, D. Randell, et. al.
Fri, 21 Apr 23
1/60

Comments: 17 pages, 10 figures, submitted to Environmental Research Letters

Earth shaped by primordial H$_2$ atmospheres [EPA]

http://arxiv.org/abs/2304.07845


Earth’s water, intrinsic oxidation state, and metal core density are fundamental chemical features of our planet. Studies of exoplanets provide a useful context for elucidating the source of these chemical traits. Planet formation and evolution models demonstrate that rocky exoplanets commonly formed with hydrogen-rich envelopes that were lost over time. These findings suggest that Earth may also have formed from bodies with H$_2$-rich primary atmospheres. Here we use a self-consistent thermodynamic model to show that Earth’s water, core density, and overall oxidation state can all be sourced to equilibrium between H$_2$-rich primary atmospheres and underlying magma oceans in its progenitor planetary embryos. Water is produced from dry starting materials resembling enstatite chondrites as oxygen from magma oceans reacts with hydrogen. Hydrogen derived from the atmosphere enters the magma ocean and eventually the metal core at equilibrium, causing metal density deficits matching that of Earth. Oxidation of the silicate rocks from solar-like to Earth-like oxygen fugacities also ensues as Si, along with H and O, alloys with Fe in the cores. Reaction with hydrogen atmospheres and metal-silicate equilibrium thus provides a simple explanation for fundamental features of Earth’s geochemistry that is consistent with rocky planet formation across the galaxy.

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E. Young, A. Shahar and H. Schlichting
Tue, 18 Apr 23
32/80

Comments: 3 main figures, 5 auxiliary figures

Climatologies of Various OH Lines From About 90,000 X-shooter Spectra [CL]

http://arxiv.org/abs/2304.08206


The nocturnal mesopause region of the Earth’s atmosphere radiates chemiluminescent emission from various roto-vibrational bands of hydroxyl (OH), which is therefore a good tracer of the chemistry and dynamics at the emission altitudes. Intensity variations can, e.g., be caused by the general circulation, gravity waves, tides, planetary waves, and the solar activity. While the basic OH response to the different dynamical influences has been studied quite frequently, detailed comparisons of the various individual lines are still rare. Such studies can improve our understanding of the OH-related variations as each line shows a different emission profile. We have therefore used about 90,000 spectra of the X-shooter spectrograph of the Very Large Telescope at Cerro Paranal in Chile in order to study 10 years of variations of 298 OH lines. The analysis focuses on climatologies of intensity, solar cycle effect, and residual variability (especially with respect to time scales of hours and about 2 days) for day of year and local time. For a better understanding of the resulting variability patterns and the line-specific differences, we applied decomposition techniques, studied the variability depending on time scale, and calculated correlations. As a result, the mixing of thermalized and nonthermalized OH level populations clearly influences the amplitude of the variations. Moreover, the local times of the variability features shift depending on the effective line emission height, which can mainly be explained by the propagation of the migrating diurnal tide. This behavior also contributes to remarkable differences in the effective solar cycle effect.

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S. Noll, C. Schmidt, W. Kausch, et. al.
Tue, 18 Apr 23
70/80

Comments: 35 single-column pages and 12 figures; accepted for publication in J. Geophys. Res. Atmos

How the Moon Impacts Subsea Communication Cables [CL]

http://arxiv.org/abs/2304.06905


We report tidal-induced latency variations on a transpacific subsea cable. Week-long recordings with a precision phase meter suggest length changes in the sub-meter range caused by the Poisson effect. The described method adds to the toolbox for the new field >>optical oceanic seismology<<.

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L. Moeller
Mon, 17 Apr 23
2/51

Comments: N/A

The radiation environment over the African continent at aviation altitudes: First results of the RPiRENA-based dosimeter [CL]

http://arxiv.org/abs/2303.15452


The radiation environment over the African continent, at aviation altitudes, remains mostly uncharacterized and unregulated. In this paper we present initial measurements made by a newly developed active dosimeter on-board long-haul flights between South Africa and Germany. Based on these initial tests, we believe that this low-cost and open-source dosimeter is suitable for continued operation over the Africa continent and can provide valuable long-term measurements to test dosimteric models and inform aviation policy

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M. Mosotho, R. Strauss, S. S.Bottcher, et. al.
Wed, 29 Mar 23
68/73

Comments: Accepted to appear in Journal of Space Weather and Space Climate

Redox evolution of the crystallizing terrestrial magma ocean and its influence on atmosphere outgassing [EPA]

http://arxiv.org/abs/2301.07505


Magma oceans are episodes of large-scale melting of the mantle of terrestrial planets. The energy delivered by the Moon-forming impact induced a deep magma ocean on the young Earth, corresponding to the last episode of core-mantle equilibration. The crystallization of this magma ocean led to the outgassing of volatiles initially present in the Earth’s mantle, resulting in the formation of a secondary atmosphere. During outgassing, the magma ocean acts as a chemical buffer for the atmosphere via the oxygen fugacity, set by the equilibrium between ferrous- and ferric-iron oxides in the silicate melts. By tracking the evolution of the oxygen fugacity during magma ocean solidification, we model the evolving composition of a C-O-H atmosphere. We use the atmosphere composition to calculate its thermal structure and radiative flux. This allows us to calculate the lifetime of the terrestrial magma ocean. We find that, upon crystallizing, the magma ocean evolves from a mildly reducing to a highly oxidized redox state, thereby transiting from a CO- and H2-dominated atmosphere to a CO2- and H2O-dominated one. We find the overall duration of the magma ocean crystallization to depend mostly on the bulk H content of the mantle, and to remain below 1.5 millions years for up to 9 Earth’s water oceans’ worth of H. Our model also suggests that reduced atmospheres emit lower infrared radiation than oxidized ones, despite of the lower greenhouse effect of reduced species, resulting in a longer magma ocean lifetime in the former case. Although developed for a deep magma ocean on Earth, the framework applies to all terrestrial planet and exoplanet magma oceans, depending on their volatile budgets.

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M. Maurice, R. Dasgupta and P. Hassanzadeh
Thu, 19 Jan 23
80/100

Comments: 31 pages, 9+2 figures, accepted for publication in PSJ

Terrestrial Effects of Nearby Supernovae: Updated Modeling [EPA]

http://arxiv.org/abs/2301.05757


We have re-evaluated recent studies of effects on Earth by cosmic rays (CRs) from nearby supernovae (SNe) at 100 pc and 50 pc, in the diffusive transport CR case, here including an early time suppression at lower CR energies neglected in the previous work. Inclusion of this suppression leads to lower overall CR flux at early times, lower atmospheric ionization, smaller resulting ozone depletion, and lower sea-level muon radiation dose. Differences in atmospheric impacts are most pronounced for the 100 pc case with less significant differences in the 50 pc case. We find a greater discrepancy in the modeled sea-level muon radiation dose, with significantly smaller dose values in the 50 pc case; our results indicate it is unlikely that muon radiation is a significant threat to the biosphere for SNe beyond at least 20 pc. We have also performed new modeling of effects by SNe at 20 pc and 10 pc. Overall, our results indicate that, considering only effects of SN CRs, the “lethal” SN distance may be closer to 20 pc rather than the typically quoted 8-10 pc.

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B. Thomas and A. Yelland
Wed, 18 Jan 23
102/133

Comments: 21 pages, 6 figures; submitted to ApJ

Moist convection is most vigorous at intermediate atmospheric humidity [EPA]

http://arxiv.org/abs/2301.03669


In Earth’s current climate, moist convective updraft speeds increase with surface warming. This trend suggests that very vigorous convection might be the norm in extremely hot and humid atmospheres, such as those undergoing a runaway greenhouse transition. However, theoretical and numerical evidence suggests that convection is actually gentle in water vapor-dominated atmospheres, implying that convective vigor may peak at some intermediate humidity level. Here, we perform small-domain convection-resolving simulations of an Earth-like atmosphere over a wide range of surface temperatures and confirm that there is indeed a peak in convective vigor, which we show occurs near T_s ~ 330 K. We show that a similar peak in convective vigor exists when the relative abundance of water vapor is changed by varying the amount of background (non-condensing) gas at fixed T_s, which may have implications for Earth’s climate and atmospheric chemistry during the Hadean and Archean. We also show that Titan-like thermodynamics (i.e., a thick nitrogen atmosphere with condensing methane and low gravity) produce a peak in convective vigor at T_s ~ 95 K, which is curiously close to the current surface temperature of Titan. Plotted as functions of the saturation specific humidity at cloud base, metrics of convective vigor from both Earth-like and Titan-like experiments all peak when cloud-base air contains roughly 10% of the condensible gas by mass. Our results point to a potentially common phenomenon in terrestrial atmospheres: that moist convection is most vigorous when the condensible component is between dilute and non-dilute abundance.

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J. Seeley and R. Wordsworth
Wed, 11 Jan 23
15/80

Comments: N/A

Deep Learning for Space Weather Prediction: Bridging the Gap between Heliophysics Data and Theory [IMA]

http://arxiv.org/abs/2212.13328


Traditionally, data analysis and theory have been viewed as separate disciplines, each feeding into fundamentally different types of models. Modern deep learning technology is beginning to unify these two disciplines and will produce a new class of predictively powerful space weather models that combine the physical insights gained by data and theory. We call on NASA to invest in the research and infrastructure necessary for the heliophysics’ community to take advantage of these advances.

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J. Dorelli, C. Bard, T. Chen, et. al.
Thu, 29 Dec 22
8/47

Comments: Heliophysics 2050 White Paper

Daily detection and quantification of methane leaks using Sentinel-3: a tiered satellite observation approach with Sentinel-2 and Sentinel-5p [CL]

http://arxiv.org/abs/2212.11318


The twin Sentinel-3 satellites have multi-band radiometers which observe at methane-sensitive shortwave infrared bands with daily global coverage and 500 m ground pixel resolution. We investigate the methane observation capability of Sentinel-3 and how its coverage-resolution combination fits between Sentinel-5p and Sentinel-2. We show that methane plume enhancements can be retrieved from the shortwave infrared bands of Sentinel-3. We report a lowest emission detection by Sentinel-3 of 9 t/h under favorable detection conditions of low wind speeds and high surface albedo. We demonstrate Sentinel-3-based identification and monitoring of methane leaks using two case studies. Near Moscow, Sentinel-3 shows that two major short-term leaks separated by 30 km occurred simultaneously at a gas pipeline and appear as a single methane plume in Sentinel-5p data. For a major Sentinel-5p leak detection near the Hassi Messaoud oil/gas field in Algeria, Sentinel-3 identifies the leaking facility emitting continuously for 6 days, and Sentinel-2 pinpoints the source of the leak at an oil/gas well. Sentinel-2 and Sentinel-3 also show the 6-day leak was followed by a four-month period of burning of the leaking gas, suggesting a gas well blowout to be the cause of the leak. We find similar source rate quantifications from plume detections by Sentinel-3 and Sentinel-2 for these leaks, demonstrating utility of Sentinel-3 for emission quantification. These case studies show that zooming in with Sentinel-3 and Sentinel-2 in synergy allows precise identification and quantification as well as monitoring of the sources corresponding to methane anomalies observed in global scans of Sentinel-5p.

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S. Pandey, M. Nistelrooij, J. Maasakkers, et. al.
Fri, 23 Dec 22
25/58

Comments: N/A

The effect of interior heat flux on the atmospheric circulation of hot and ultra-hot Jupiters [EPA]

http://arxiv.org/abs/2212.03833


Many hot and ultra-hot Jupiters have inflated radii, implying that their interiors retain significant entropy from formation. These hot interiors lead to an enhanced internal heat flux that impinges upon the atmosphere from below. In this work, we study the effect of this hot interior on the atmospheric circulation and thermal structure of hot and ultra-hot Jupiters. To do so, we incorporate the population-level predictions from evolutionary models of hot and ultra-hot Jupiters as input for a suite of General Circulation Models (GCMs) of their atmospheric circulation with varying semi-major axis and surface gravity. We conduct simulations with and without a hot interior, and find that there are significant local differences in temperature of up to hundreds of Kelvin and in wind speeds of hundreds of m s$^{-1}$ or more across the observable atmosphere. These differences persist throughout the parameter regime studied, and are dependent on surface gravity through the impact on photosphere pressure. These results imply that the internal evolution and atmospheric thermal structure and dynamics of hot and ultra-hot Jupiters are coupled. As a result, a joint approach including both evolutionary models and GCMs may be required to make robust predictions for the atmospheric circulation of hot and ultra-hot Jupiters.

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T. Komacek, P. Gao, D. Thorngren, et. al.
Thu, 8 Dec 22
35/63

Comments: Accepted at ApJL, 17 pages, 8 figures

Dynamics of the Great Oxidation Event from a 3D photochemical-climate model [EPA]

http://arxiv.org/abs/2212.01389


From the Archean toward the Proterozoic, the Earth’s atmosphere underwent a major shift from anoxic to oxic conditions, around 2.4 to 2.1 Gyr, known as the Great Oxidation Event (GOE). This rapid transition may be related to an atmospheric instability caused by the formation of the ozone layer. Previous works were all based on 1D photochemical models. Here, we revisit the GOE with a 3D photochemical-climate model to investigate the possible impact of the atmospheric circulation and the coupling between the climate and the dynamics of the oxidation. We show that the diurnal, seasonal and transport variations do not bring significant changes compared to 1D models. Nevertheless, we highlight a temperature dependence for atmospheric photochemical losses. A cooling during the late Archean could then have favored the triggering of the oxygenation. In addition, we show that the Huronian glaciations, which took place during the GOE, could have introduced a fluctuation in the evolution of the oxygen level. Finally, we show that the oxygen overshoot which is expected to have occurred just after the GOE, was likely accompanied by a methane overshoot. Such high methane concentrations could have had climatic consequences and could have played a role in the dynamics of the Huronian glaciations.

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A. Jaziri, B. Charnay, F. Selsis, et. al.
Tue, 6 Dec 22
27/87

Comments: N/A

Effective Emission Heights of Various OH Lines From X-shooter and SABER Observations of a Passing Quasi-2-Day Wave [CL]

http://arxiv.org/abs/2211.17043


Chemiluminescent radiation of the vibrationally and rotationally excited OH radical, which dominates the nighttime near-infrared emission of the Earth’s atmosphere in wide wavelength regions, is an important tracer of the chemical and dynamical state of the mesopause region between 80 and 100 km. As radiative lifetimes and rate coefficients for collision-related transitions depend on the OH energy level, line-dependent emission profiles are expected. However, except for some height differences for whole bands mostly revealed by satellite-based measurements, there is a lack of data for individual lines. We succeeded in deriving effective emission heights for 298 OH lines thanks to the joint observation of a strong quasi-2-day wave (Q2DW) in eight nights in 2017 with the medium-resolution spectrograph X-shooter at the Very Large Telescope at Cerro Paranal in Chile and the limb-sounding SABER radiometer on the TIMED satellite. Our fitting procedure revealed the most convincing results for a single wave with a period of about 44 h and a vertical wavelength of about 32 km. The line-dependent as well as altitude-resolved phases of the Q2DW then resulted in effective heights which differ by up to 8 km and tend to increase with increasing vibrational and rotational excitation. The measured dependence of emission heights and wave amplitudes (which were strongest after midnight) on the line parameters implies the presence of a cold thermalized and a hot non-thermalized population for each vibrational level.

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S. Noll, C. Schmidt, W. Kausch, et. al.
Thu, 1 Dec 22
58/85

Comments: 33 single-column pages, 1 table, and 11 figures; accepted for publication in J. Geophys. Res. Atmos

Observability of signatures of transport-induced chemistry in clear atmospheres of hot gas giant exoplanets [EPA]

http://arxiv.org/abs/2211.09071


Transport-induced quenching, i.e., the homogenisation of chemical abundances by atmospheric advection, is thought to occur in the atmospheres of hot gas giant exoplanets. While some numerical modelling of this process exists, the three-dimensional nature of transport-induced chemistry is underexplored. Here we present results of 3D cloud- and haze-free simulations of the atmospheres of HAT-P-11b, HD 189733b, HD 209458b, and WASP-17b including coupled hydrodynamics, radiative transfer and chemistry. Our simulations were performed with two chemical schemes: a chemical kinetics scheme, which is capable of capturing transport-induced quenching, and a simpler, more widely used chemical equilibrium scheme. We find that transport-induced quenching is predicted to occur in atmospheres of all planets in our sample; however, the extent to which it affects their synthetic spectra and phase curves varies from planet to planet. This implies that there is a “sweet spot” for the observability of signatures of transport-induced quenching, which is controlled by the interplay between the dynamics and chemistry.

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M. Zamyatina, &. Hébrard, B. Drummond, et. al.
Thu, 17 Nov 22
22/63

Comments: accepted to MNRAS, 27 pages, 8+7 figures

Spectropolarimetry as a Means to Address Cloud Composition and Habitability for a Cloudy Exoplanetary Atmosphere in the Habitable Zone [EPA]

http://arxiv.org/abs/2211.06450


In our solar system, the densely cloud-covered atmosphere of Venus stands out as an example of how polarimetry can be used to gain information on cloud composition and particle mean radius. With current interest running high on discovering and characterizing extrasolar planets in the habitable zone where water exists in the liquid state, making use of spectropolarimetric measurements of directly-imaged exoplanets could provide key information unobtainable through other means. In principle, spectropolarimetric measurements can determine if acidity causes water activities in the clouds to be too low for life. To this end, we show that a spectropolarimeter measurement over the range 400 nm – 1000 nm would need to resolve linear polarization to a precision of about 1% or better for reflected starlight from an optically thick cloud-enshrouded exoplanet. We assess the likelihood of achieving this goal by simulating measurements from a notional spectropolarimeter as part of a starshade configuration for a large space telescope (a HabEx design, but for a 6 m diameter primary mirror). Our simulations include consideration of noise from a variety of sources. We provide guidance on limits that would need to be levied on instrumental polarization to address the science issues we discuss. For photon-limited noise, integration times would need to be of order one hour for a large radius (10 Earth radii) planet to more than 100 hours for smaller exoplanets depending on the star-planet separation, planet radius, phase angle and desired uncertainty. We discuss implications for surface chemistry and habitability.

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R. West, P. Dumont, R. Hu, et. al.
Tue, 15 Nov 22
5/103

Comments: ApJ, accepted

AEROS: Oceanographic Hyperspectral Imaging and Argos-Tracking CubeSat [CL]

http://arxiv.org/abs/2211.05124


AEROS is a 3U CubeSat pathfinder toward a future ocean-observing constellation, targeting the Portuguese Atlantic region. AEROS features a miniaturized, high-resolution Hyperspectral Imager (HSI), a 5MP RGB camera, and a Software Defined Radio (SDR). The sensor generated data will be processed and aggregated for end-users in a new web-based Data Analysis Center (DAC). The HSI has 150 spectrally contiguous bands covering visible to near-infrared with 10 nm bandwidth. The HSI collects ocean color data to support studies of oceanographic characteristics known to influence the spatio-temporal distribution and movement behavior of marine organisms. Usage of an SDR expands AEROS’s operational and communication range and allows for remote reconfiguration. The SDR receives, demodulates, and retransmits short duration messages, from sources including tagged marine organisms, autonomous vehicles, subsurface floats, and buoys. The future DAC will collect, store, process, and analyze acquired data, taking advantage of its ability to disseminate data across the stakeholders and the scientific network. Correlation of animal-borne Argos platform locations and oceanographic data will advance fisheries management, ecosystem-based management, monitoring of marine protected areas, and bio-oceanographic research in the face of a rapidly changing environment. For example, correlation of oceanographic data collected by the HSI, geolocated with supplementary images from the RGB camera and fish locations, will provide researchers with near real-time estimates of essential oceanographic variables within areas selected by species of interest.

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S. Prendergast, C. Payne, M. Lifson, et. al.
Fri, 11 Nov 22
19/58

Comments: 13 pages, 16 figures, Manuscript presented at the 73rd International Astronautical Congress, IAC 2022, Paris, France, 18 – 22 September 2022

The AEROS ocean observation mission and its CubeSat pathfinder [CL]

http://arxiv.org/abs/2211.05008


AEROS aims to develop a nanosatellite as a precursor of a future system of systems, which will include assets and capabilities of both new and existing platforms operating in the Ocean and Space, equipped with state-of-the-art sensors and technologies, all connected through a communication network linked to a data gathering, processing and dissemination system. This constellation leverages scientific and economic synergies emerging from New Space and the opportunities in prospecting, monitoring, and valuing the Ocean in a sustainable manner, addressing the demand for improved spatial, temporal, and spectral coverage in areas such as coastal ecosystems management and climate change assessment and mitigation. Currently, novel sensors and systems, including a miniaturized hyperspectral imager and a flexible software-defined communication system, are being developed and integrated into a new versatile satellite structure, supported by an innovative on-board software. Additional sensors, like the LoRaWAN protocol and a wider field of view RGB camera, are under study. To cope with data needs, a Data Analysis Centre, including a cloud-based data and telemetry dashboard and a back-end layer, to receive and process acquired and ingested data, is being implemented to provide tailored-to-use remote sensing products for a wide range of applications for private and institutional stakeholders.

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R. Santos, O. Bertolami, E. Castanho, et. al.
Thu, 10 Nov 22
73/78

Comments: 15 pages, 9 figures, Manuscript presented at the 4S Symposium 2022, Vilamoura, Portugal, 16 – 20 May 2022

3D modelling of the impact of stellar activity on tidally locked terrestrial exoplanets: atmospheric composition and habitability [EPA]

http://arxiv.org/abs/2210.13257


Stellar flares present challenges to the potential habitability of terrestrial planets orbiting M dwarf stars through inducing changes in the atmospheric composition and irradiating the planet’s surface in large amounts of ultraviolet light. To examine their impact, we have coupled a general circulation model with a photochemical kinetics scheme to examine the response and changes of an Earth-like atmosphere to stellar flares and coronal mass ejections. We find that stellar flares increase the amount of ozone in the atmosphere by a factor of 20 compared to a quiescent star. We find that coronal mass ejections abiotically generate significant levels of potential bio-signatures such as N$_2$O. The changes in atmospheric composition cause a moderate decrease in the amount of ultraviolet light that reaches the planets surface, suggesting that while flares are potentially harmful to life, the changes in the atmosphere due to a stellar flare act to reduce the impact of the next stellar flare.

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R. Ridgway, M. Zamyatina, N. Mayne, et. al.
Tue, 25 Oct 22
25/111

Comments: 28 pages, 21 figures, accepted to MNRAS

The Key Factors Controlling the Seasonality of Planetary Climate [CL]

http://arxiv.org/abs/2210.11357


Several different factors influence the seasonal cycle of a planet. This study uses a general circulation model and an energy balance model (EBM) to assess the parameters that govern the seasonal cycle. We define two metrics to describe the seasonal cycle, $\phi_s$, the latitudinal shift of the maximum temperature, and $\Delta T$, the maximum seasonal temperature variation amplitude. We show that alongside the expected dependence on the obliquity and orbital period, where seasonality generally strengthens with an increase in these parameters, the seasonality depends in a nontrivial way on the rotation rate. While the seasonal amplitude decreases as the rotation rate slows down, the latitudinal shift, $\phi_s$, shifts poleward. A similar result occurs in a diffusive EBM with increasing diffusivity. These results suggest that the influence of the rotation rate on the seasonal cycle stems from the effect of the rotation rate on the atmospheric heat transport.

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I. Guendelman and Y. Kaspi
Fri, 21 Oct 22
9/76

Comments: N/A

Optical turbulence forecast over short timescales using machine learning techniques [IMA]

http://arxiv.org/abs/2210.11236


Forecast of optical turbulence and atmospheric parameters relevant for ground-based astronomy is becoming an important goal for telescope planning and AO instruments optimization in several major telescope. Such detailed and accurate forecast is typically performed with numerical atmospheric models. Recently short-term forecasts (a few hours in advance) are also being provided (ALTA project) using a technique based on an autoregression approach, as part of a strategy that aims to increase the forecast accuracy. It has been proved that such a technique is able to achieve unprecedented performances so far. Such short-term predictions make use of the numerical model forecast and real-time observations. In recent years machine learning (ML) techniques also started to be used to provide an atmospheric and turbulence forecast. Preliminary results indicate however an accuracy not really competitive with respect to the autoregressive method or even prediction by persistence. This technique might be applicable joint to atmospheric model. It is therefore interesting to investigate the main features of their performances and characteristics (also because there is a great number of algorithms potentially accessible) to understand if results achieved so far can be further improved using ML. In this study we focus on a purely machine learning application to short term forecast (1-2 hours) of astroclimatic and other atmospheric parameters above VLT.

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A. Turchi, E. Masciadri and L. Fini
Fri, 21 Oct 22
76/76

Comments: 11 pages, 6 figures

Inferring changes to the global carbon cycle with WOMBAT v2.0, a hierarchical flux-inversion framework [CL]

http://arxiv.org/abs/2210.10479


The natural cycles of the surface-to-atmosphere fluxes of carbon dioxide (CO$_2$) and other important greenhouse gases are changing in response to human influences. These changes need to be quantified to understand climate change and its impacts, but this is difficult to do because natural fluxes occur over large spatial and temporal scales. To infer trends in fluxes and identify phase shifts and amplitude changes in flux seasonal cycles, we construct a flux-inversion system that uses a novel spatially varying time-series decomposition of the fluxes, while also accommodating physical constraints on the fluxes. We incorporate these features into the Wollongong Methodology for Bayesian Assimilation of Trace-gases (WOMBAT, Zammit-Mangion et al., Geosci. Model Dev., 15, 2022), a hierarchical flux-inversion framework that yields posterior distributions for all unknowns in the underlying model. We apply the new method, which we call WOMBAT v2.0, to a mix of satellite observations of CO$_2$ mole fraction from the Orbiting Carbon Observatory-2 (OCO-2) satellite and direct measurements of CO$_2$ mole fraction from a variety of sources. We estimate the changes to CO$_2$ fluxes that occurred from January 2015 to December 2020, and compare our posterior estimates to those from an alternative method based on a bottom-up understanding of the physical processes involved. We find substantial trends in the fluxes, including that tropical ecosystems trended from being a net source to a net sink of CO$_2$ over the study period. We also find that the amplitude of the global seasonal cycle of ecosystem CO$_2$ fluxes increased over the study period by 0.11 PgC/month (an increase of 8%), and that the seasonal cycle of ecosystem CO$_2$ fluxes in the northern temperate and northern boreal regions shifted earlier in the year by 0.4-0.7 and 0.4-0.9 days, respectively (2.5th to 97.5th posterior percentiles).

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M. Bertolacci, A. Zammit-Mangion, A. Schuh, et. al.
Thu, 20 Oct 22
71/74

Comments: N/A

Characterization of the Thermospheric Mean Winds and Circulation during Solstice using ICON/MIGHTI Observations [CL]

http://arxiv.org/abs/2210.09407


Using the horizontal neutral wind observations from the MIGHTI instrument onboard NASA’s ICON (Ionospheric Connection Explorer) spacecraft with continuous coverage, we determine the climatology of the mean zonal and meridional winds and the associated mean circulation at low- to middle latitudes ($10^\circ$S-40$^{\circ}$N) for Northern Hemisphere {summer} solstice conditions between 90 km and 200 km altitudes, specifically on 20 June 2020 solstice as well as for a one-month period from 8 June-7 July 2020 {and for Northern winter season from 16 December 2019-31 January 2020, which spans a 47-day period, providing full local time coverage}. The data are averaged within appropriate altitude, longitude, latitude, solar zenith angle, and local time bins to produce mean wind distributions. The geographical distributions and local time variations of the mean horizontal circulation are evaluated. The instantaneous horizontal winds exhibit a significant degree of spatiotemporal variability often exceeding $\pm 150 $ m s$^{-1}$. The daily averaged zonal mean winds demonstrate day-to-day variability. Eastward zonal winds and northward (winter-to-summer) meridional winds are prevalent in the lower thermosphere, which provides indirect observational evidence of the eastward momentum deposition by small-scale gravity waves. The mean neutral winds and circulation exhibit smaller scale structures in the lower thermosphere (90-120 km), while they are more homogeneous in the upper thermosphere, indicating the increasingly dissipative nature of the thermosphere. The mean wind and circulation patterns inferred from ICON/MIGHTI measurements can be used to constrain and validate general circulation models, as well as input for numerical wave models.

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E. Yiğit, M. Dhadly, A. Medvedev, et. al.
Wed, 19 Oct 22
24/87

Comments: Accepted for publication in Journal of Geophysical Research – Space Physics

Long-term trends of light pollution assessed from SQM measurements and an empirical atmospheric model [IMA]

http://arxiv.org/abs/2210.09177


We present long-term (4-10 years) trends of light pollution observed at 26 locations, covering rural, intermediate and urban sites, including the three major European metropolitan areas of Stockholm, Berlin and Vienna. Our analysis is based on i) night sky brightness (NSB) measurements obtained with Sky Quality Meters (SQMs) and ii) a rich set of atmospheric data products provided by the European Centre for Medium-Range Weather Forecasts. We describe the SQM data reduction routine in which we filter for moon- and clear-sky data and correct for the SQM “aging” effect using an updated version of the twilight method of Puschnig et al. (2021). Our clear-sky, aging-corrected data reveals short- and long-term (seasonal) variations due to atmospheric changes. To assess long-term anthropogenic NSB trends, we establish an empirical atmospheric model via multi-variate penalized linear regression. Our modeling approach allows to quantitatively investigate the importance of different atmospheric parameters, revealing that surface albedo and vegetation have by far the largest impact on zenithal NSB. Additionally, the NSB is sensitive to black carbon and organic matter aerosols at urban and rural sites respectively. Snow depth was found to be important for some sites, while the total column of ozone leaves impact on some rural places. The average increase in light pollution at our 11 rural sites is 1.7 percent per year. At our nine urban sites we measure an increase of 1.8 percent per year and for the remaining six intermediate sites we find an average increase of 3.7 percent per year. These numbers correspond to doubling times of 41, 39 and 19 years. We estimate that our method is capable of detecting trend slopes shallower/steeper than 1.5 percent per year.

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J. Puschnig, S. Wallner, A. Schwope, et. al.
Tue, 18 Oct 22
75/99

Comments: accepted for publication in MNRAS

21st Century Global and Regional Surface Temperature Projections [CL]

http://arxiv.org/abs/2210.03245


Many regions across the globe broke their surface temperature records in recent years, further sparking concerns about the impending arrival of “tipping points” later in the 21st century. This study analyzes observed global surface temperature trends in three target latitudinal regions: the Arctic Circle, the Tropics, and the Antarctic Circle. We show that global warming is accelerating unevenly across the planet, with the Arctic warming at approximately three times the average rate of our world. We further analyzed the reliability of latitude-dependent surface temperature simulations from a suite of Coupled Model Intercomparison Project Phase 6 models and their multi-model mean. We found that GISS-E2-1-G and FGOALS-g3 were the best-performing models based on their statistical abilities to reproduce observational, latitude-dependent data. Surface temperatures were projected from ensemble simulations of the Shared Socioeconomic Pathway 2-4.5 (SSP2-4.5). We estimate when the climate will warm by 1.5, 2.0, and 2.5 degrees C relative to the preindustrial period, globally and regionally. GISS-E2-1-G projects that global surface temperature anomalies would reach 1.5, 2.0, and 2.5 degrees C in 2024 (+/-1.34), 2039 (+/-2.83), and 2057 (+/-5.03) respectively, while FGOALS-g3 predicts these “tipping points” would arrive in 2024 (+/-2.50), 2054 (+/-7.90), and 2087 (+/-10.55) respectively. Our results reaffirm a dramatic, upward trend in projected climate warming acceleration, with upward concavity in 21st century projections of the Arctic, which could lead to catastrophic consequences across the Earth. Further studies are necessary to determine the most efficient solutions to reduce global warming acceleration and maintain a low SSP, both globally and regionally.

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N. Ma, J. Jiang, K. Hou, et. al.
Mon, 10 Oct 22
18/59

Comments: N/A

Air-sea interactions on Titan: effect of radiative transfer on the lake evaporation and atmospheric circulation [EPA]

http://arxiv.org/abs/2210.03278


Titan’s northern high latitudes host many large hydrocarbon lakes. Like water lakes on Earth, Titan’s lakes are constantly subject to evaporation. This process strongly affects the atmospheric methane abundance, the atmospheric temperature, the lake mixed layer temperature, and the local wind circulation. In this work we use a 2D atmospheric mesoscale model coupled to a slab lake model to investigate the effect of solar and infrared radiation on the exchange of energy and methane between Titan’s lakes and atmosphere. The magnitude of solar radiation reaching the surface of Titan through its thick atmosphere is only a few W/m2. However, we find that this small energy input is important and is comparable in absolute magnitude to the latent and sensible heat fluxes, as suggested in the prior study by S. Rafkin and A. Soto (Icarus, 2020).
The implementation of a gray radiative scheme in the model confirms the importance of radiation when studying lakes at the surface of Titan. Solar and infrared radiation change the energy balance of the system leading to an enhancement of the methane evaporation rate, an increase of the equilibrium lake temperature almost completely determined by its environment (humidity, insolation, and background wind), and a strengthening of the local sea breeze, which undergoes diurnal variations. The sea breeze efficiently transports methane vapor horizontally, from the lake to the land, and vertically due to rising motion along the sea breeze front and due to radiation-induced turbulence over the land.

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A. Chatain, S. Rafkin, A. Soto, et. al.
Mon, 10 Oct 22
53/59

Comments: Accepted in The Planetary Science Journal (08/2022)

An ab initio study of the rovibronic spectrum of sulphur monoxide (SO): diabatic vs. adiabatic representation [CL]

http://arxiv.org/abs/2210.02800


We present an ab initio study of the rovibronic spectra of sulfur monoxide ($^{32}$S$^{16}$O) using internally contracted multireference confoguration interaction (ic-MRCI) method and aug-cc-pV5Z basis sets. It covers 13 electronic states $X^{3}\Sigma^{-}$, $a^{1}\Delta$, $b^{1}\Sigma^{+}$, $c^{1}\Sigma^{-}$, $A^{\prime\prime 3}\Sigma^{+}$, $A^{\prime 3}\Delta$, $A^{3}\Pi$, $B^{3}\Sigma^{-}$, $C^{3}\Pi$, $d^{1}\Pi$, $e^{1}\Pi$, $C^{\prime 3}\Pi$, and $(3)^{1}\Pi$ ranging up to 66800 cm$^{-1}$. The ab initio spectroscopic model includes 13 potential energy curves, 23 dipole and transition dipole moment curves, 23 spin-orbit curves, and 14 electronic angular momentum curves. A diabatic representation is built by removing the avoided crossings between the spatially degenerate pairs $C^{3}\Pi – C^{\prime 3}\Pi$ and $e^{1}\Pi – (3)^{1}\Pi$ through a property-based diabatisation method. We also present non-adiabatic couplings and diabatic couplings for these avoided crossing systems. All phases for our coupling curves are defined, and consistent, providing the first fully reproducible spectroscopic model of SO covering the wavelength range longer than 147 nm. Finally, an ab initio rovibronic spectrum of SO is computed.

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R. Brady, S. Yurchenko, G. Kim, et. al.
Fri, 7 Oct 22
22/62

Comments: 15 pages, 14 figures

Cross-Wave Profiles of Altitude and Particle Size of Noctilucent Clouds in the Case of One-Dimensional Small-Scale Gravity Wave Pattern [CL]

http://arxiv.org/abs/2210.00431


This paper describes the wide-field three-color observations of an expanded field of noctilucent clouds modulated by a one-dimensional gravity wave. Long wave crests were aligned by a small angle to the solar vertical in the sky. This made possible separate determination of altitude and particle size at different wave phases based on three-color photometry of noctilucent clouds. Thereby, it is possible to use simple optical imaging to record the changes in the parameters of noctilucent clouds when a short-period gravity wave passes by.

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O. Ugolnikov
Tue, 4 Oct 22
70/71

Comments: 8 pages, 6 figures, submitted to Planetary and Space Science

GENESIS: Co-location of Geodetic Techniques in Space [CL]

http://arxiv.org/abs/2209.15298


Improving and homogenizing time and space reference systems on Earth and, more directly, realizing the Terrestrial Reference Frame (TRF) with an accuracy of 1mm and a long-term stability of 0.1mm/year are relevant for many scientific and societal endeavors. The knowledge of the TRF is fundamental for Earth and navigation sciences. For instance, quantifying sea level change strongly depends on an accurate determination of the geocenter motion but also of the positions of continental and island reference stations, as well as the ground stations of tracking networks. Also, numerous applications in geophysics require absolute millimeter precision from the reference frame, as for example monitoring tectonic motion or crustal deformation for predicting natural hazards. The TRF accuracy to be achieved represents the consensus of various authorities which has enunciated geodesy requirements for Earth sciences.
Today we are still far from these ambitious accuracy and stability goals for the realization of the TRF. However, a combination and co-location of all four space geodetic techniques on one satellite platform can significantly contribute to achieving these goals. This is the purpose of the GENESIS mission, proposed as a component of the FutureNAV program of the European Space Agency. The GENESIS platform will be a dynamic space geodetic observatory carrying all the geodetic instruments referenced to one another through carefully calibrated space ties. The co-location of the techniques in space will solve the inconsistencies and biases between the different geodetic techniques in order to reach the TRF accuracy and stability goals endorsed by the various international authorities and the scientific community. The purpose of this white paper is to review the state-of-the-art and explain the benefits of the GENESIS mission in Earth sciences, navigation sciences and metrology.

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P. Delva, Z. Altamimi, A. Blazquez, et. al.
Mon, 3 Oct 22
38/55

Comments: 31 pages, 9 figures, submitted to Earth, Planets and Space (EPS)

Letter of Interest: Ocean science with the Pacific Ocean Neutrino Experiment [CL]

http://arxiv.org/abs/2209.14710


The Pacific Ocean Neutrino Experiment (P-ONE) is a proposed cubic-kilometer scale neutrino telescope planned to be installed in the deep-sea of the north-east Pacific Ocean. In collaboration with the optical deep-sea data and communications network operated by Ocean Networks Canada, an international collaboration of researchers plans to install an array of kilometer-long mooring lines in a depth of around 2660 m to the relatively flat deep-sea region called Cascadia Basin, around 300 miles West of Vancouver Island. With the design and development ongoing, the P-ONE collaboration is interested to initiate participation of fellow scientists of the oceanographic and marine science communities to provide expertise and experience towards deploying additional or inclusive instrumentation and measurement strategies for doing oceanographic research. In addition to the monitoring of optical bioluminescence and deep-ocean dynamics and thermodynamics, active and passive acoustics can be installed within the P-ONE array. This letter summarizes the P-ONE detector and a non-exhaustive list of potential topics of interest for oceanographic and marine research.

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F. Henningsen and L. Schumacher
Fri, 30 Sep 22
5/71

Comments: N/A

Predicting Swarm Equatorial Plasma Bubbles Via Supervised Machine Learning [CL]

http://arxiv.org/abs/2209.13482


Equatorial Plasma Bubbles (EPBs) are plumes of low density plasma that rise up from the bottomside of the F layer towards the exosphere. EPBs are known causes of radio wave scintillations which can degrade communications with spacecraft. We build a random forest regressor to predict and forecast the probability of an EPB [0-1] detected by the IBI processor on-board the SWARM spacecraft. We use 8-years of Swarm data from 2014 to 2021 and transform the data from a time series into a 5 dimensional space consisting of latitude, longitude, mlt, year, and day-of-the-year. We also add Kp, F10.7cm and solar wind speed. The observations of EPBs with respect to geolocation, local time, season and solar activity mostly agrees with existing work, whilst the link geomagnetic activity is less clear. The prediction has an accuracy of 88% and performs well across the EPB specific spatiotemporal scales. This proves that the XGBoost method is able to successfully capture the climatological and daily variability of SWARM EPBs. Capturing the daily variance has long evaded researchers because of local and stochastic features within the ionosphere. We take advantage of Shapley Values to explain the model and to gain insight into the physics of EPBs. We find that as the solar wind speed increases the probability of an EPB decreases. We also identify a spike in EPB probability around the Earth-Sun perihelion. Both of these insights were derived directly from the XGBoost and Shapley technique.

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S. Reddy, C. Forsyth, A. Aruliah, et. al.
Wed, 28 Sep 22
32/89

Comments: 26 Pages, 18 Figures

Multi-Hour Ahead Dst Index Prediction Using Multi-Fidelity Boosted Neural Networks [CL]

http://arxiv.org/abs/2209.12571


The Disturbance storm time (Dst) index has been widely used as a proxy for the ring current intensity, and therefore as a measure of geomagnetic activity. It is derived by measurements from four ground magnetometers in the geomagnetic equatorial regions.
We present a new model for predicting $Dst$ with a lead time between 1 and 6 hours. The model is first developed using a Gated Recurrent Unit (GRU) network that is trained using solar wind parameters. The uncertainty of the $Dst$ model is then estimated by using the ACCRUE method [Camporeale et al. 2021]. Finally, a multi-fidelity boosting method is developed in order to enhance the accuracy of the model and reduce its associated uncertainty. It is shown that the developed model can predict $Dst$ 6 hours ahead with a root-mean-square-error (RMSE) of 13.54 $\mathrm{nT}$. This is significantly better than the persistence model and a simple GRU model.

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A. Hu, E. Camporeale and B. Swiger
Tue, 27 Sep 22
34/89

Comments: arXiv admin note: text overlap with arXiv:2203.11001

The Role of High Energy Photoelectrons on the Dissociation of Molecular Nitrogen in Earth's Ionosphere [CL]

http://arxiv.org/abs/2209.11185


Soft x-ray radiation from the sun is responsible for the production of high energy photoelectrons in the D and E regions of the ionosphere, where they deposit most of their ionization energy. The photoelectrons created by this process are the main drivers for dissociation of Nitrogen molecule ($N_2$) below 200 km. Furthermore, the dissociation of $N_2$ is one of main mechanisms of the production of Nitric Oxide (NO) at these altitudes. In order to estimate the dissociation rate of $N_2$ we need its dissociation cross-sections. The dissociation cross-sections for $N_2$ by photoelectrons are primarily estimated from the cross-sections of its excitation states using predissociation factors and dissociative ionization channels. Unfortunately, the lack of cross-sections data, particularly at high electron energies and of higher excited states of $N_2$ and $N_2^+$, introduces a lot of uncertainty in the dissociation rate calculation, which subsequently leads to uncertainties in the NO production rate from this source.

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S. Samaddar, K. Venkataramani, J. Yonker, et. al.
Fri, 23 Sep 22
39/70

Comments: N/A

The Role of Solar Soft X-rays Irradiance in Thermospheric Structure [EPA]

http://arxiv.org/abs/2209.10543


We use a new Atmospheric Chemistry and Energetics one-dimensional (ACE1D) thermospheric model to show that the energies deposited by the solar soft x-rays in the lower thermosphere at altitudes between 100 -150 km (Bailey et al. 2000), affects the temperature of the entire Earth’s thermosphere even at altitudes well above 300 km. By turning off the input solar flux in the different wavelength bins of the model iteratively, we are able to demonstrate that the maximum change in exospheric temperature is due to the changes in the soft x-ray solar bins. We also show, using the thermodynamic heat equation, that the molecular diffusion via non-thermal photoelectrons, is the main source of heat transfer to the upper ionosphere/thermosphere and results in the increase of the temperature of the neutral atmosphere. Moreover, these temperature change and heating effects of the solar soft x-rays are comparable to that of the strong HeII 30.4nm emission. Lastly, we show that the uncertainties in the solar flux irradiance at these soft x-rays wavelengths result in corresponding uncertainties in modeled exospheric temperature and the uncertainties increase with increased solar activity.

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S. Samaddar, K. Venkataramani and S. Bailey
Fri, 23 Sep 22
50/70

Comments: N/A

Atmospheric ionization rates during a geomagnetic reversal [CL]

http://arxiv.org/abs/2209.10104


The Matuyama-Brunhes reversal of Earth’s magnetic dipole field took place 0.78 Ma ago, and detailed temporally resolved paleomagnetic data are available for this period. A geomagnetic reversal is expected to impact the cosmic ray flux, which in turn might impact atmospheric ionization rates. In this study a model that yields atmospheric ionization for the entire globe based on an input magnetic field is presented. Taking the time dependent paleomagnetic data as input, a 3D time series of the atmospheric ionization rates during the reversal is produced. We show, that as the dipole field weakens, the atmospheric ionization increases at low latitudes. The increase is ca. 25% at the surface and up to a factor of 5 in the upper atmosphere. Globally, ionization rates increase around 13% at the surface and up to a factor of 2 in the upper atmosphere, whereas polar regions are largely unaffected. Finally, the change in ionization due to the solar 11-year cycle is greatly affected by the reversal. The relative change in atmospheric ionization between solar-minimum and solar-maximum varies between 2 and two orders of magnitude. All atmospheric ionization data is made available for download.

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J. Svensmark
Thu, 22 Sep 22
62/65

Comments: 8 Figures, 1 table

An experimental and theoretical investigation of HCN production in the Hadean Earth atmosphere [EPA]

http://arxiv.org/abs/2209.09257


A critical early stage for the origin of life on Earth may have involved the production of hydrogen cyanide (HCN) in a reducing, predominantly H$_2$ atmosphere. HCN is crucial for the origin of life as it is a possible precursor to several biomolecules that make up RNA and proteins including nucleobases, nucleotides, amino acids, and ribose. In this work, we perform an in depth experimental and theoretical investigation of HCN production in reducing atmospheric conditions (89-95% H$_2$) possibly representing the earliest stages of the Hadean eon, ~4.5-4.3 billion years ago. We make use of cold plasma discharges – a laboratory analog to shortwave UV radiation – to simulate HCN production in the upper layers of the atmosphere for CH$_4$ abundances ranging from 0.1-6.5%. We then combine experimental mass spectrum measurements with our theoretical plasma models to estimate the HCN concentrations produced in our experiments. We find that upper atmospheric HCN production scales linearly with CH$_4$ abundance with the relation [HCN] = 0.13 $\pm$ 0.01[CH$_4$]. Concentrations of HCN near the surface of the Hadean Earth are expected to be about 2-3 orders of magnitude lower. The addition of 1% water to our experiments results in a ~50% reduction in HCN production. We find that four reactions are primarily responsible for HCN production in our experiments: (i) $^4$N + CH$_3$ -> H$_2$CN + H -> HCN + H$_2$, (ii) $^4$N + CH -> CN + H followed by CN + CH$_4$ -> HCN + CH$_3$, (iii) C$_2$H$_4$ + $^4$N -> HCN + CH$_3$, and (iv) $^4$N + $^3$CH$_2$ -> HCN + H. The most prebiotically favorable Hadean atmosphere would have been very rich in CH$_4$ (> 5%), and as a result of greenhouse effects the surface would be likely very hot. In such a prebiotic scenario, it may have been important to incorporate HCN into organic hazes that could later release biomolecules and precursors into the first ponds.

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B. Pearce, C. He and S. Hörst
Wed, 21 Sep 22
16/68

Comments: Accepted for publication in ACS Earth and Space Chemistry, 24 pages, 7 figures, 5 tables, Supporting info

Can we detect deep axisymmetric toroidal magnetic fields in stars? [SSA]

http://arxiv.org/abs/2209.09823


One of the major discoveries of asteroseismology is the signature of a strong extraction of angular momentum (AM) in the radiative zones of stars across the entire Hertzsprung-Russell diagram, resulting in weak core-to-surface rotation contrasts. Despite all efforts, a consistent AM transport theory, which reproduces both the internal rotation and mixing probed thanks to the seismology of stars, remains one of the major open problems in modern stellar astrophysics. A possible key ingredient to figure out this puzzle is magnetic field with its various possible topologies. Among them, strong axisymmetric toroidal fields, which are subject to the so-called Tayler MHD instability, could play a major role. They could trigger a dynamo action in radiative layers while the resulting magnetic torque allows an efficient transport of AM. But is it possible to detect signatures of these deep toroidal magnetic fields? The only way to answer this question is asteroseismology and the best laboratories of study are intermediate-mass and massive stars because of their external radiative envelope. Since most of these are rapid rotators during their main-sequence, we have to study stellar pulsations propagating in stably stratified, rotating, and potentially strongly magnetised radiative zones. For that, we generalise the traditional approximation of rotation, which provides in its classic version a flexible treatment of the adiabatic propagation of gravito-inertial modes, by taking simultaneously general axisymmetric differential rotation and toroidal magnetic fields into account. Using this new non-perturbative formalism, we derive the asymptotic properties of magneto-gravito-inertial modes and we explore the different possible field configurations. We found that the magnetic effects should be detectable for equatorial fields using high-precision asteroseismic data.

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H. Dhouib, S. Mathis, L. Bugnet, et. al.
Wed, 21 Sep 22
52/68

Comments: 4 pages, 2 figures. Proceeding of the Annual meeting of the French Society of Astronomy and Astrophysics (SF2A 2022)

From the Stochastic Weather to a Putative Chaotic Earth System [EPA]

http://arxiv.org/abs/2209.09540


In this brief report we discuss how continuous changes on the physical parameters that determine the weather conditions may lead to long term climate variability. This variability of the weather patterns are a response to continuous random short period weather excitations that are imprinted in the ocean-atmosphere-cryosphere-land system, the Earth System. Given that Earth System is, in the Anthropocene, dominated by the human action, it responds to the intensity and the rate of change of the humankind activities. Thus, we argue, in the context of a specific model of the Earth System, that this rate of change may admit a chaotic-type behaviour.

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O. Bertolami
Wed, 21 Sep 22
57/68

Comments: Based on talk delivered at the Green Marble 2022, “International Meeting on Anthropocene Studies and Ecocriticism: Only One Earth”, June 30th – July 2nd, 2022, Porto, Portugal

Towards photophoretically levitating macroscopic sensors in the stratosphere [CL]

http://arxiv.org/abs/2209.08093


Photophoretic forces could levitate thin 10 centimeter-scale structures in Earth$’$s stratosphere indefinitely. We develop models of the thermal transpiration lofting force on a bilayer sandwich structure under stratospheric conditions driven by radiative fluxes in the thermal-infrared and solar-band. Similar structures have been levitated in the laboratory. Lofting is maximized when the layers are separated by an air gap equal to the mean free path (MFP), when about half of the layers$’$ surface area consists of holes with radii < MFP, and when the top layer is solar-transmissive and infrared-emissive while the bottom layer is solar-absorptive and infrared-transmissive. We describe a preliminary design of a 10 cm diameter device that combines a levitating structure made of two membranes 2 $\mu$m apart with the support structure required for stiffness and orientation control. We limit the design to components that could be fabricated with available methods. Structural analysis suggests that the device would have sufficient strength to withstand forces that might be encountered in transport, deployment, and flight. Our models predict a payload capacity of about 300 mg at 25 km altitude and our analysis suggests it could support bidirectional radio communication at over 10 Mb/s and could have limited navigational abilities. Such devices could be useful for atmospheric science or telecommunications, and similar devices might be useful on Mars. Structures a few times larger might have payloads of a few grams.

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B. Schafer, J. Kim, J. Vlassak, et. al.
Tue, 20 Sep 22
4/81

Comments: Main: 14 pages, 4 figures. Supporting information: 7 pages, 13 figures

Trustworthy modelling of atmospheric formaldehyde powered by deep learning [CL]

http://arxiv.org/abs/2209.07414


Formaldehyde (HCHO) is one one of the most important trace gas in the atmosphere, as it is a pollutant causing respiratory and other diseases. It is also a precursor of tropospheric ozone which damages crops and deteriorates human health. Study of HCHO chemistry and long-term monitoring using satellite data is important from the perspective of human health, food security and air pollution. Dynamic atmospheric chemistry models struggle to simulate atmospheric formaldehyde and often overestimate by up to two times relative to satellite observations and reanalysis. Spatial distribution of modelled HCHO also fail to match satellite observations. Here, we present deep learning approach using a simple super-resolution based convolutional neural network towards simulating fast and reliable atmospheric HCHO. Our approach is an indirect method of HCHO estimation without the need to chemical equations. We find that deep learning outperforms dynamical model simulations which involves complicated atmospheric chemistry representation. Causality establishing the nonlinear relationships of different variables to target formaldehyde is established in our approach by using a variety of precursors from meteorology and chemical reanalysis to target OMI AURA satellite based HCHO predictions. We choose South Asia for testing our implementation as it doesnt have in situ measurements of formaldehyde and there is a need for improved quality data over the region. Moreover, there are spatial and temporal data gaps in the satellite product which can be removed by trustworthy modelling of atmospheric formaldehyde. This study is a novel attempt using computer vision for trustworthy modelling of formaldehyde from remote sensing can lead to cascading societal benefits.

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M. Biswas and M. Singh
Fri, 16 Sep 22
30/84

Comments: N/A

The Oscillatory Motion of Jupiter's Polar Cyclones Results From Vorticity Dynamics [EPA]

http://arxiv.org/abs/2209.00309


The polar cyclone at Jupiter’s south pole and the five cyclones surrounding it oscillate in position and interact. These cyclones, observed since 2016 by NASA’s Juno mission, present a unique opportunity to study vortex dynamics and interactions on long time scales. The cyclones’ position data, acquired by Juno’s JIRAM instrument, is analyzed, showing dominant oscillations with ~12 month periods and amplitudes of ~400 km. Here, the mechanism driving these oscillations is revealed by considering vorticity-gradient forces generated by mutual interactions between the cyclones and the latitudinal variation in planetary vorticity. Data-driven estimation of these forces exhibits a high correlation with the measured acceleration of the cyclones. To further test this mechanism, a model is constructed, simulating how cyclones subject to these forces exhibit similar oscillatory motion.

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N. Gavriel and Y. Kaspi
Fri, 2 Sep 22
60/62

Comments: 9 pages, 5 figures, 11 supplementary pages, 9 supplementary figures

Super-resolution wavefront reconstruction [IMA]

http://arxiv.org/abs/2208.12052


Super-Resolution (SR) is a technique that seeks to upscale the resolution of a set of measured signals. SR retrieves higher-frequency signal content by combining multiple lower resolution sampled data sets. SR is well known both in the temporal and spatial domains. It is widely used in imaging to reduce aliasing and enhance the resolution of coarsely sampled images.This paper applies the SR technique to the bi-dimensional wavefront reconstruction. In particular, we show how SR is intrinsically suited for tomographic multi WaveFront Sensor (WFS) AO systems revealing many of its advantages with minimal design effort. This paper provides a direct space and Fourier-optics description of the wavefront sensing operation and demonstrate how SR can be exploited through signal reconstruction, especially in the framework of Periodic Nonuniform Sampling. Both meta uniform and nonuniform sampling schemes are investigated. Then, the SR bi-dimensional model for a Shack Hartmann (SH) WFS is provided and the characteristics of the sensitivity function are analyzed. The SR concept is finally validated with numerical simulations of representative multi WFS SH AO systems. Our results show that combining several WFS samples in a SR framework grants access to a larger number of modes than the native one offered by a single WFS and that despite the fixed sub-aperture size across samples. Furthermore, we show that the associated noise propagation is not degraded under SR. Finally, the concept is extended to the signal produced by single Pyramid WFS. In conclusion, SR applied to wavefront reconstruction offers a new parameter space to explore as it decouples the size of the subaperture from the desired wavefront sampling resolution. By cutting short with old assumptions, new, more flexible and better performing AO designs become now possible.

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S. Oberti, C. Correia, T. Fusco, et. al.
Fri, 26 Aug 22
43/49

Comments: Astronomy & Astrophysics Section: 13. Astronomical instrumentation AA/2022/43954

Greater climate sensitivity and variability on TRAPPIST-1e than Earth [EPA]

http://arxiv.org/abs/2208.06297


The atmospheres of rocky exoplanets are close to being characterized by astronomical observations, in part due to the commissioning of the James Webb Space Telescope. These observations compel us to understand exoplanetary atmospheres, in the voyage to find habitable planets. With this aim, we investigate the effect that CO$_2$ partial pressure (pCO$_2$) has on exoplanets’ climate variability, by analyzing results from ExoCAM model simulations of the tidally locked TRAPPIST-1e exoplanet, an Earth-like aqua-planet and Earth itself. First, we relate the differences between the planets to their elementary parameters. Then, we compare the sensitivity of the Earth analogue and TRAPPIST-1e’s surface temperature and precipitation to pCO$_2$. Our simulations suggest that the climatology and extremes of TRAPPIST-1e’s temperature are $\sim$1.5 times more sensitive to pCO$_2$ relative to Earth. The precipitation sensitivity strongly depends on the specific region analyzed. Indeed, the precipitation near mid-latitude and equatorial sub-stellar regions of TRAPPIST-1e is more sensitive to pCO$_2$, and the precipitation sensitivity is $\sim$2 times larger in TRAPPIST-1e. A dynamical systems perspective, which provides information about how the atmosphere evolves in phase-space, provides additional insights. Notably, an increase in pCO$_2$, results in an increase in atmospheric persistence on both planets, and the persistence of TRAPPIST-1e is more sensitive to pCO$_2$ than Earth. We conclude that the climate of TRAPPIST-1e may be more sensitive to pCO$_2$, particularly on its dayside. This study documents a new pathway for understanding the effect that varying planetary parameters have on the climate variability of potentially habitable exoplanets and on Earth.

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A. Hochman, P. Luca and T. Komacek
Mon, 15 Aug 22
21/54

Comments: Accepted at ApJ

Gaussian phase autocorrelation as an accurate compensator for FFT-based atmospheric phase screen simulations [IMA]

http://arxiv.org/abs/2208.06060


Accurately simulating the atmospheric turbulence behaviour is always challenging. The well-known FFT based method falls short in correctly predicting both the low and high frequency behaviours. Sub-harmonic compensation aids in low-frequency correction but does not solve the problem for all screen size to outer scale parameter ratios (G/$L_0$). FFT-based simulation gives accurate result only for relatively large screen size to outer scale parameter ratio (G/$L_0$). In this work, we have introduced a Gaussian phase autocorrelation matrix to compensate for any sort of residual errors after applying for a modified subharmonics compensation. With this, we have solved problems such as under sampling at the high-frequency range, unequal sampling/weights for subharmonics addition at low-frequency range and the patch normalization factor. Our approach reduces the maximum error in phase structure-function in the simulation with respect to theoretical prediction to within 1.8\%, G/$L_0$ = 1/1000.

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S. Chhabra, J. Paul, A. Ramaprakash, et. al.
Mon, 15 Aug 22
26/54

Comments: SPIE conference proceedings 2020. arXiv admin note: substantial text overlap with arXiv:2106.01002

Impact of climate change on site characteristics of eight major astronomical observatories using high-resolution global climate projections until 2050 [IMA]

http://arxiv.org/abs/2208.04918


Sites for next-generation telescopes are chosen decades before the first light of a telescope. Site selection is usually based on recent measurements over a period that is too short to account for long-term changes in observing conditions such as those arising from anthropogenic climate change. In this study, we analyse trends in astronomical observing conditions for eight sites. Most sites either already host telescopes that provide in situ measurements of weather parameters or are candidates for hosting next-generation telescopes. For a fine representation of orography, we use the highest resolution global climate model (GCM) ensemble available provided by the high-resolution model intercomparison project and developed as part of the European Union Horizon 2020 PRIMAVERA project. We evaluate atmosphere-only and coupled PRIMAVERA GCM historical simulations against in situ measurements and the fifth generation atmospheric reanalysis (ERA5) of the ECMWF. The projections of changes in current site conditions are then analysed for the period 2015-2050 using PRIMAVERA future climate simulations. Over most sites, we find that PRIMAVERA GCMs show good agreement in temperature, specific humidity, and precipitable water vapour compared to in situ observations and ERA5. The ability of PRIMAVERA to simulate those variables increases confidence in their projections. For those variables, the model ensemble projects an increasing trend for all sites. On the other hand, no significant trends are projected for relative humidity, cloud cover, or astronomical seeing and PRIMAVERA does not simulate these variables well compared to observations and reanalyses. Therefore, there is little confidence in these projections. Our results show that climate change likely increases time lost due to bad site conditions.

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C. Haslebacher, M. Demory, B. Demory, et. al.
Wed, 10 Aug 22
64/66

Comments: 53 pages, 35 figures. accepted for publication in A&A

The Resonant Tidal Evolution of the Earth-Moon Distance [EPA]

http://arxiv.org/abs/2207.00438


Due to tidal interactions in the Earth-Moon system, the spin of the Earth slows down and the Moon drifts away. This recession of the Moon is now measured with great precision, but it has been realized, more than fifty years ago, that simple tidal models extrapolated back in time lead to an age of the Moon that is by far incompatible with the geochronological and geochemical evidence. In order to evade this problem, more elaborate models have been proposed, taking into account the oceanic tidal dissipation. However, these models did not fit both the estimated lunar age and the present rate of lunar recession simultaneously. Here we present a physical model that reconciles these two constraints and yields a unique solution of the tidal history. This solution fits well the available geological proxies for the history of the Earth-Moon system and consolidates the cyclostratigraphic method. The resulting evolution involves multiple crossings of resonances in the oceanic dissipation that are associated with significant and rapid variations in the lunar orbital distance, the Earth’s length of the day, and the Earth’s obliquity.

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M. Farhat, P. Auclair-Desrotour, G. Boué, et. al.
Mon, 4 Jul 22
42/62

Comments: N/A

Changing spatial distribution of water flow charts major change in Mars' greenhouse effect [EPA]

http://arxiv.org/abs/2206.00036


Early Mars had rivers, but the cause of Mars’ wet-to-dry transition remains unknown. Past climate on Mars can be probed using the spatial distribution of climate-sensitive landforms. We analyzed global databases of water-worked landforms and identified changes in the spatial distribution of rivers over time. These changes are simply explained by comparison to a simplified meltwater model driven by an ensemble of global climate model simulations, as the result of $\gtrsim$10 K global cooling, from global average surface temperature (T) $\ge$ 268 K to T $\sim$ 258 K, due to a weaker greenhouse effect. In other words, river-forming climates on Early Mars were warm and wet first, and cold and wet later. Surprisingly, analysis of the greenhouse effect within our ensemble of global climate model simulations suggests that this shift was primarily driven by waning non-CO2 radiative forcing, and not changes in CO2 radiative forcing.

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E. Kite, M. Mischna, B. Fan, et. al.
Thu, 2 Jun 22
37/57

Comments: N/A

2n-Stream Radiative Transfer [CL]

http://arxiv.org/abs/2205.09713


We use 2n streams, where n is an integer, of axially symmetric radiation to solve the equation of transfer for a layered medium. This is a generalization of Schuster’s classic 2 stream model. As is well known, using only the first 2n Legendre polynomials to describe the angular dependence of radiation reduces the equation of transfer to a first order differential equation in a space of 2n dimensions. It is convenient to characterize the radiation as 2n stream intensities propagating at zenith angles having cosines called the 2n Gauss-Legendre cosines defined to be solutions of equating the Legendre polynomial of degree 2n to zero. We show how to efficiently and accurately solve the equation of transfer with vector and matrix methods analogous to those used to solve Schroedinger’s equation of quantum mechanics. To model strong forward scattering, like that of visible light by Earth’s clouds, we have introduced a new family of phase functions. These give the maximum possible forward scattering p(p+1) for a phase function constructed from the first 2p Legendre polynomials, where p is an integer. We show illustrative examples of radiative-transfer phenomena calculated with this new method.

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W. Wijngaarden and W. Happer
Fri, 20 May 22
11/65

Comments: 59 pages, 20 figures

Patchy nightside clouds on ultra-hot Jupiters: General Circulation Model simulations with radiatively active cloud tracers [EPA]

http://arxiv.org/abs/2205.07834


The atmospheres of ultra-hot Jupiters have been characterized in detail through recent phase curve and low- and high-resolution emission and transmission spectroscopic observations. Previous numerical studies have analyzed the effect of the localized recombination of hydrogen on the atmospheric dynamics and heat transport of ultra-hot Jupiters, finding that hydrogen dissociation and recombination lead to a reduction in the day-to-night contrasts of ultra-hot Jupiters relative to previous expectations. In this work, we add to previous efforts by also considering the localized condensation of clouds in the atmospheres of ultra-hot Jupiters, their resulting transport by the atmospheric circulation, and the radiative feedback of clouds on the atmospheric dynamics. To do so, we include radiatively active cloud tracers into the existing MITgcm framework for simulating the atmospheric dynamics of ultra-hot Jupiters. We take cloud condensate properties appropriate for the high-temperature condensate corundum from CARMA cloud microphysics models. We conduct a suite of GCM simulations with varying cloud microphysical and radiative properties, and we find that partial cloud coverage is a ubiquitous outcome of our simulations. This patchy cloud distribution is inherently set by atmospheric dynamics in addition to equilibrium cloud condensation, and causes a cloud greenhouse effect that warms the atmosphere below the cloud deck. Nightside clouds are further sequestered at depth due to a dynamically induced high-altitude thermal inversion. We post-process our GCMs with the Monte Carlo radiative transfer code gCMCRT and find that the patchy clouds on ultra-hot Jupiters do not significantly impact transmission spectra but can affect their phase-dependent emission spectra.

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T. Komacek, X. Tan, P. Gao, et. al.
Tue, 17 May 22
4/95

Comments: 41 pages, 23 figures, 2 tables. Re-submitted to ApJ. Co-first authors

The Effect of Ocean Salinity on Climate and Its Implications for Earth's Habitability [EPA]

http://arxiv.org/abs/2205.06785


The influence of atmospheric composition on the climates of present-day and early Earth has been studied extensively, but the role of ocean composition has received less attention. We use the ROCKE-3D ocean-atmosphere general circulation model to investigate the response of Earth’s present-day and Archean climate system to low vs. high ocean salinity. We find that saltier oceans yield warmer climates in large part due to changes in ocean dynamics. Increasing ocean salinity from 20 g/kg to 50 g/kg results in a 71% reduction in sea ice cover in our present-day Earth scenario. This same salinity change also halves the pCO$_2$ threshold at which Snowball glaciation occurs in our Archean scenarios. In combination with higher levels of greenhouse gases such as CO$_2$ and CH$_4$, a saltier ocean may allow for a warm Archean Earth with only seasonal ice at the poles despite receiving 20% less energy from the Sun.

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S. Olson, M. Jansen, D. Abbot, et. al.
Mon, 16 May 22
31/42

Comments: Accepted for publication in Geophysical Research Letters 04/19/22

First High-speed Camera Observations of the Optical Counterpart of a Terrestrial Gamma-ray Flash [CL]

http://arxiv.org/abs/2205.05115


In this paper, we present the first observation of optical emission of a downward-directed terrestrial gamma ray flash (TGF). The optical emission was observed by a high-speed video camera Phantom v2012 in conjunction with the Telescope Array (TA) surface detector, lightning mapping array, interferrometer, fast antenna, and the national lightning detection network. The suite of gamma and lightning instruments, timing resolution, and source proximity offers us an unprecedented look at the TGF phenomena. On September 11 of 2021 we observed a storm above the TA detector. The storm resulted in six extremely energetic TGF events that were produced by flashes with return stroke peak currents up to 223 kA. The observed TGFs were found to correlate directly to the initial burst pulse signal of the lightning flash while producing an intense optical signature. Results from this study allow us to furthers the understanding regarding the initiation mechanism of TGFs.

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R. Abbasi, J. J.W.Belz, M. Saba, et. al.
Thu, 12 May 22
12/63

Comments: N/A

Ocean signatures in the total flux and polarization spectra of Earth-like exoplanets [EPA]

http://arxiv.org/abs/2205.05669


Numerical simulations of starlight that is reflected by Earth-like exoplanets predict habitability signatures that can be searched for with future telescopes. We explore signatures of water oceans in the flux and polarization spectra of this reflected light. With an adding-doubling algorithm, we compute the total flux F, polarized flux Q and degree of polarization P of starlight reflected by dry and ocean model planets with Earth-like atmospheres and patchy clouds. The oceans consist of Fresnel reflecting surfaces with wind-ruffled waves, foam and wave shadows, above natural blue seawater. Our results are presented as functions of wavelength (from 300 to 2500 nm with 1 nm resolution) and as functions of the planetary phase angle from 90 to 170 degrees. The ocean glint increases F, |Q| and P with increasing phase angle at non-absorbing wavelengths, and causes the spectra of F and |Q| for the various phase angles to intersect. In the near-infrared, Q is negative, i.e. the direction of polarization is perpendicular to the plane through the star, planet, and observer. In the P-spectra, the glint leaves dips (instead of peaks) in gaseous absorption bands. All those signatures are missing in the spectra of dry planets. The dips in P, and the negative Q in the near-infrared, can be searched for at a phase angle of 90 degrees, where the planet-star separation is largest. Those ocean signatures in polarized light do not suffer from false positive glint signals that could be due to clouds or reflecting dry surfaces. For heavily cloudy planets, ocean detection is possible when the glint is (partially) cloud-free. When modelling signals of planets with oceans, using horizontally inhomogeneous cloud covers is thus crucial. Observations spread over time would increase the probability of catching a cloud-free glint and detecting an ocean.

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V. Trees and D. Stam
Thu, 12 May 22
29/63

Comments: Accepted for publication in Astronomy & Astrophysics

On Sea-Level Change in Coastal Areas [CL]

http://arxiv.org/abs/2205.03895


Variations in sea-level, based on tide gauge data (GSLTG) and on combining tide gauges and satellite data (GSLl) are subjected to singular spectrum analysis (SSA), to determine their trends and periodic or quasi-periodic components. GLSTG increases by 90 mm from 1860 to 2020, a contribution of 0.56 mm/yr to the mean rise rate. Annual to multi-decadal periods of ~90/80, 60, 30, 20, 10/11, and 4/5 years are found in both GSLTG and GSLl. These periods are commensurable periods of the Jovian planets, combinations of the periods of Neptune (165 yr), Uranus (84 yr), Saturn (29 yr) and Jupiter (12 yr). These same periods are encountered in sea-level changes, motion of the rotation pole RP and evolution of global pressure GP, suggesting physical links. The first SSA components comprise most of the signal variance: 95% for GSLTG, 89% for GSLI, 98% for GP, 75% for RP. Laplace derived the Liouville-Euler equations that govern the rotation and translation of the rotation axis of any celestial body. He emphasized that one must consider the orbital kinetic moments of all planets in addition to gravitational attractions and concluded that the Earth’s rotation axis should undergo motions that carry the combinations of periods of the Sun, Moon and planets. Almost all the periods found in the SSA components of sea-level (GSLl and GSLTG), global pressure (GP) and polar motion (RP), of their modulations and their derivatives can be associated with the Jovian planets. It would be of interest to search for data series with longer time spans, that could allow one to test whether the trends themselves could be segments of components with still longer periodicities (e.g. 175 yr Jose cycle).

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V. Courtillot, J. Mouël and F. Lopes
Tue, 10 May 22
48/70

Comments: N/A

Critical Balance and Scaling of Stably Stratified Turbulence at Low Prandtl Number [CL]

http://arxiv.org/abs/2205.01540


We extend the scaling relations of stably stratified turbulence from the geophysical regime of unity Prandtl number to the astrophysical regime of extremely small Prandtl number applicable to stably stratified regions of stars and gas giants. A transition to a new turbulent regime is found to occur when the Prandtl number drops below the inverse of the buoyancy Reynolds number, i.e. $PrRb<1$, which signals a shift of the dominant balance in the buoyancy equation. Application of critical balance arguments then derives new predictions for the anisotropic energy spectrum and dominant balance of the Boussinesq equations in the $PrRb\ll1$ regime. We find that all the standard scaling relations from the unity $Pr$ limit of stably stratified turbulence simply carry over if the Froude number, $Fr$, is replaced by a modified Froude number, $Fr_M\equiv Fr/(PrRb)^{1/4}$. The geophysical and astrophysical regimes are thus smoothly connected across the $PrRb=1$ transition. Applications to vertical transport in stellar radiative zones and modification to the instability criterion for the small-scale dynamo are discussed.

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V. Skoutnev
Wed, 4 May 22
34/48

Comments: N/A

Avoiding the "Great Filter": An Assessment of Climate Change Solutions and Combinations for Effective Implementation [CL]

http://arxiv.org/abs/2205.00133


Climate change is the long-term shift in global weather patterns, largely caused by anthropogenic activity of greenhouse gas emissions. Global climate temperatures have unmistakably risen and naturally-occurring climate variability alone cannot account for this trend. Human activities are estimated to have caused about 1.0 {\deg}C of global warming above the pre-industrial baseline and if left unchecked, will continue to drastically damage the Earth and its inhabitants. Globally, natural disasters and subsequent economic losses have become increasingly impactful as a result of climate change. Both wildlife ecosystems and human habitats have been negatively impacted, from rising sea levels to alarming frequency of severe weather events around the world. Attempts towards alleviating the effects of global warming have often been at odds and remain divided among a multitude of strategies, reducing the overall effectiveness of these efforts. It is evident that collaborative action is required for avoiding the most severe consequences of climate change. This paper evaluates the main strategies (industrial/energy, political, economic, agricultural, atmospheric, geological, coastal, and social) towards both mitigating and adapting to climate change. As well, it provides an optimal combination of seven solutions which can be implemented simultaneously, working in tandem to limit and otherwise accommodate the harmful effects of climate change. Previous legislation and deployment techniques are also discussed as guides for future endeavors.

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J. Zhang, K. Zhang, M. Zhang, et. al.
Tue, 3 May 22
16/82

Comments: N/A

Layer formation in a stably-stratified fluid cooled from above. Towards an analog for Jupiter and other gas giants [EPA]

http://arxiv.org/abs/2204.12643


It is theorized that in gas giants, an outer convection zone advances into the interior as the surface cools, and multiple convective layers form beneath that convective front. To study layer formation below an outer convection zone in a similar scenario, we investigate the evolution of a stably-stratified fluid with a linear composition gradient that is constantly being cooled from above. We use the Boussinesq approximation in a series of 2D simulations at low and high Prandtl numbers ($\mathrm{Pr} = 0.5$ and 7), initialized with different temperature stratifications, and cooled at different rates. We find that simulations initialized with an isothermal temperature profile form multiple convective layers at $\mathrm{Pr} = 7$. These layers result from an instability of a diffusive thermal boundary layer below the outer convection zone. At low Pr, layers do not form. Double-diffusive instabilities drive the fluid below the outer convection zone into a state of turbulent diffusion rather than layered convection. Changing the initial distribution of temperature to decrease linearly with depth results in lower values of the inverse density ratio $R^{-1}\equiv S_{z}/T_{z}$ (given the normalization in this work), and consequently, the spontaneous formation of multiple convective layers at low Pr. For the stratifications used in this study, on the long-term the composition gradient is an ineffective barrier against the propagation of the outer convection zone and the entire fluid becomes fully-mixed, whether layers form or not. Our results challenge 1D evolutionary models of gas giant planets, which predict that layers are long-lived and that the outer convective envelope stops advancing inwards. We discuss what is needed for future work to build more realistic models.

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J. Fuentes, A. Cumming and E. Anders
Thu, 28 Apr 22
51/70

Comments: Submitted to PR Fluids, comments are welcome 🙂

Chaotic Behaviour of the Earth System in the Anthropocene [EPA]

http://arxiv.org/abs/2204.08955


It is shown that the Earth System (ES) can, due to the impact of human activities, behave in a chaotic fashion. Our arguments are based on the assumption that the ES can be described by a Landau-Ginzburg model, which on its own allows for predicting that the ES evolves, through regular trajectories in the phase space, towards a Hothouse Earth scenario for a finite amount of human-driven impact. Furthermore, we find that the equilibrium point for temperature fluctuations can exhibit bifurcations and a chaotic pattern if the human impact follows a logistic map.

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A. Bernardini, O. Bertolami and F. Francisco
Wed, 20 Apr 22
27/62

Comments: 18 pages, 6 figures. arXiv admin note: text overlap with arXiv:1811.05543

Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets [EPA]

http://arxiv.org/abs/2204.06503


Observations of time-resolved thermal emission from tidally locked exoplanets can tell us about their atmospheric temperature structure. Telescopes such as JWST and ARIEL will improve the quality and availability of these measurements. This motivates an improved understanding of the processes that determine atmospheric temperature structure, particularly atmospheric circulation. The circulation is important in determining atmospheric temperatures, not only through its ability to transport heat, but also because any circulation pattern needs to be balanced by horizontal pressure contrasts, therefore implying a particular temperature structure. In this work, we show how the global temperature field on a tidally locked planet can be decomposed into contributions that are balanced by different components of the atmospheric circulation. These are the superrotating jet, stationary Rossby waves, and the divergent circulation. To achieve this, we partition the geopotential field into components balanced by the divergent circulation and the rotational circulation, with the latter comprising the jet and Rossby waves. The partitioned geopotential then implies a corresponding partitioning of the temperature via the hydrostatic relation. We apply these diagnostics to idealised general circulation model simulations, to show how the separate rotational and divergent circulations together make up the total three-dimensional atmospheric temperature structure. We also show how each component contributes distinct signatures to the thermal phase curve of a tidally locked planet. We conclude that this decomposition is a physically meaningful separation of the temperature field that explains its global structure, and can be used to fit observations of thermal emission.

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N. Lewis and M. Hammond
Thu, 14 Apr 22
49/62

Comments: Submitted to AAS journals. Comments welcome and appreciated

Computation of Optical Refractive Index Structure Parameter from its Statistical Definition Using Radiosonde Data [CL]

http://arxiv.org/abs/2204.00349


Knowledge of the optical refractive index structure parameter $C_n^2$ is of interest for Free Space Optics (FSO) and ground-based optical astronomy, as it depicts the strength of the expected scintillation on the received optical waves. Focus is given here to models using meteorological quantities coming from radiosonde measurements as inputs to estimate the $C_n^2$ profile in the atmosphere. A model relying on the $C_n^2$ statistical definition is presented and applied to recent high-density radiosonde profiles at Trappes (France) and Hilo, HI (USA). It is also compared to thermosonde measurements coming from the T-REX campaign. This model enables to obtain site-specific average profiles and to identify isolated turbulent layers using only pressure and temperature measurements, paving the way for optical site selection.

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F. Quatresooz, D. Vanhoenacker-Janvier and C. Oestges
Mon, 4 Apr 22
36/50

Comments: N/A

COWS all tHE way Down (COWSHED) I: Could cow based planetoids support methane atmospheres? [EPA]

http://arxiv.org/abs/2203.16609


More often than not a lunch time conversation will veer off into bizarre and uncharted territories. In rare instances these frontiers of conversation can lead to deep insights about the Universe we inhabit. This paper details the fruits of one such conversation. In this paper we will answer the question: How many cows do you need to form a planetoid entirely comprised of cows, which will support a methane atmoosphere produced by the planetary herd? We will not only present the necessary assumptions and theory underpinning the cow-culations, but also present a thorough (and rather robust) discussion of the viability of, and implications for accomplishing, such a feat.

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W. Roper, T. Cook, V. Korbina, et. al.
Fri, 1 Apr 22
6/85

Comments: N/A

Adiabatic lapse rate of real gases [CL]

http://arxiv.org/abs/2203.12040


We derive a formula for the dry adiabatic lapse rate of atmospheres composed of real gases. We restrict our study to those described by a family of two-parameter cubic equations of state and the recent Guevara non-cubic equation. Since our formula depends on the adiabatic curves, we compute them all at once considering molecules that can move, rotate, and vibrate, for any equation of state. To illustrate our results, we estimate the lapse rate of the troposphere of Titan, obtaining a better approximation to the observed data in some instances, when compared to the estimation provided by the virial expansion up to third order.

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B. Díaz, M. Ariza and J. Ramírez
Thu, 24 Mar 22
7/56

Comments: N/A

Geophysical Evolution During Rocky Planet Formation [EPA]

http://arxiv.org/abs/2203.10023


Progressive astronomical characterization of planet-forming disks and rocky exoplanets highlight the need for increasing interdisciplinary efforts to understand the birth and life cycle of terrestrial worlds in a unified picture. Here, we review major geophysical and geochemical processes that shape the evolution of rocky planets and their precursor planetesimals during planetary formation and early evolution, and how these map onto the astrophysical timeline and varying accretion environments of planetary growth. The evolution of the coupled core-mantle-atmosphere system of growing protoplanets diverges in thermal, compositional, and structural states to first order, and ultimately shapes key planetary characteristics that can discern planets harboring clement surface conditions from those that do not. Astronomical campaigns seeking to investigate rocky exoplanets will require significant advances in laboratory characterization of planetary materials and time- and spatially-resolved theoretical models of planetary evolution, to extend planetary science beyond the Solar System and constrain the origins and frequency of habitable worlds like our own.

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T. Lichtenberg, L. Schaefer, M. Nakajima, et. al.
Mon, 21 Mar 22
1/60

Comments: 37 pages, 10 figures; under review for publication as a chapter in Protostars and Planets VII, University of Arizona Press; comments welcome; figures available at this https URL

The Pierre Auger Exotic Events and Axion Quark Nuggets [CL]

http://arxiv.org/abs/2203.08160


The Pierre Auger Observatory have reported [1-3] observation of several exotic events (EE) which apparently related to thunderstorms. These events are much larger in size than conventional cosmic ray (CR) events, and they have very distinct timing features. A possible nature of the observed phenomenon is still a matter of active research and debates as many unusual features of these exotic events are hard to explain. In particular, the frequency of appearance of these EE is very low (less than 2 events/year), in huge contrast with a typical rate of a conventional lightning strikes in the area. We propose that the observed EE can be explained within the so-called axion quark nugget (AQN) dark matter model. The idea is that the AQNs may trigger and initiate a special and unique class of lightning strikes during a thunderstorm as a result of ionization of the atmospheric molecules along its path. The corresponding AQN-induced lighting flashes may show some specific features not shared by typical and much more frequent conventional flashes. We support this proposal by demonstrating that the observations[1-3], including the frequency of appearance and time duration are consistent with observations. We also comment on possible relation of AUGER EEs with the Telescope Array bursts and the terrestrial gamma ray flashes (TGF). We list a number of features of the AQN-induced EE (such as specific radio pulses synchronized with these events) which can be directly tested by future experiments. We also suggest to use distributed acoustic sensing (DAS) instruments to detect the acoustic pulses which must be synchronized with AUGER EEs.

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A. Zhitnitsky
Thu, 17 Mar 22
56/66

Comments: 17 pages

A novel method for adaptive control of deformable mirrors [CL]

http://arxiv.org/abs/2203.04915


For sufficiently wide ranges of applied control signals (control voltages), MEMS and piezoelectric Deformable Mirrors (DMs), exhibit nonlinear behavior. The nonlinear behavior manifests itself in nonlinear actuator couplings, nonlinear actuator deformation characteristics, and in the case of piezoelectric DMs, hysteresis. Furthermore, in a number of situations, DM behavior can change over time, and this requires a procedure for updating the DM models on the basis of the observed data. If not properly modeled and if not taken into account when designing control algorithms, nonlinearities, and time-varying DM behavior, can significantly degrade the achievable closed-loop performance of Adaptive Optics (AO) systems. Widely used approaches for DM control are based on pre-estimated linear time-invariant DM models in the form of influence matrices. Often, these models are not being updated during system operation. Consequently, when the nonlinear DM behavior is excited by control signals with wide operating ranges, or when the DM behavior changes over time, the state-of-the-art DM control approaches relying upon linear control methods, might not be able to produce a satisfactory closed-loop performance of an AO system. Motivated by these key facts, we present a novel method for data-driven DM control. Our approach combines a simple open-loop control method with a recursive least squares method for dynamically updating the DM model. The DM model is constantly being updated on the basis of the dynamically changing DM operating points. That is, the proposed method updates both the control actions and the DM model during the system operation. We experimentally verify this approach on a Boston Micromachines MEMS DM with 140 actuators. Preliminary experimental results reported in this manuscript demonstrate good potential for using the developed method for DM control.

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A. Haber
Thu, 10 Mar 22
30/60

Comments: SPIE Proceedings, SPIE BiOS, 2022, San Francisco, California, United States, Proceedings Volume 11969, Adaptive Optics and Wavefront Control for Biological Systems VIII; 1196902

Scaling and phase diagrams of planetary sediment transport [EPA]

http://arxiv.org/abs/2203.00562


Sediment transport by atmospheric winds shapes the surface and affects the climates of planetary bodies. Reliably predicting the occurrence and rate of sediment transport in the Solar System has been notoriously difficult because fluid density, grain size and soil cohesiveness vary across many orders of magnitude. Here, we use recent advances in analytical and numerical sediment transport modeling to derive general scaling relations for planetary transport. In particular, we show that the equations of motion of rebounding grains predict that the minimum threshold fluid shear velocity needed to sustain transport (transport cessation threshold) scales with the particle-fluid-density ratio ($s$) as $s^{1/3}$, in contrast to the $s^{1/2}$-scaling exhibited by the threshold for transport initiation. The grain size corresponding to this minimum is in the range $80{-}290~\mu\mathrm{m}$ for Solar System bodies. Our results, summarized in phase diagrams for the cessation threshold, mean transport rate and dust emission potential, explain the observed eastward propagation of Titan’s dunes, in spite of a predominantly westward wind circulation, indicate active dust cycles on Earth, Mars and Titan, and suggest marginal but active atmospheric transport on Venus, Triton and Pluto.

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T. Pähtz, O. Duŕan and F. Comola
Wed, 2 Mar 22
36/54

Comments: N/A

Amateur Observers Witness the Return of Venus' Cloud Discontinuity [EPA]

http://arxiv.org/abs/2202.12601


Firstly identified in images from JAXA’s orbiter Akatsuki, the cloud discontinuity of Venus is a planetary-scale phenomenon known to be recurrent since, at least, the 1980s. Interpreted as a new type of Kelvin wave, this disruption is associated to dramatic changes in the clouds’ opacity and distribution of aerosols, and it may constitute a critical piece for our understanding of the thermal balance and atmospheric circulation of Venus. Here, we report its reappearance on the dayside middle clouds four years after its last detection with Akatsuki/IR1, and for the first time, we characterize its main properties using exclusively near-infrared images from amateur observations. In agreement with previous reports, the discontinuity exhibited temporal variations in its zonal speed, orientation, length, and its effect over the clouds’ albedo during the 2019/2020 eastern elongation. Finally, a comparison with simultaneous observations by Akatsuki UVI and LIR confirmed that the discontinuity is not visible on the upper clouds’ albedo or thermal emission, while zonal speeds are slower than winds at the clouds’ top and faster than at the middle clouds, evidencing that this Kelvin wave might be transporting momentum up to upper clouds.

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K. E., P. J., M. G., et. al.
Mon, 28 Feb 22
37/38

Comments: 19 pages, 6 figures, 2 tables

Detecting deep axisymmetric toroidal magnetic fields in stars. The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimutal magnetic field [SSA]

http://arxiv.org/abs/2202.10026


Asteroseismology has revealed small core-to-the-surface rotation contrasts in stars in the whole HR diagram. This is the signature of strong transport of angular momentum (AM) in stellar interiors. One of the plausible candidates to efficiently carry AM is magnetic fields with various topologies that could be present in stellar radiative zones. Among them, strong axisymmetric azimuthal magnetic fields have received a lot of interest. Indeed, if they are subject to the so-called Tayler instability, the accompanying triggered Maxwell stresses can transport AM efficiently. In addition, the electromotive force induced by the fluctuations of magnetic and velocity fields could potentially sustain a dynamo action that leads to the regeneration of the initial strong axisymmetric azimuthal magnetic field. The key question we aim to answer is: can we detect signatures of these deep strong azimuthal magnetic fields? The only way to answer this question is asteroseismology and the best laboratories of study are intermediate-mass and massive stars. Most of these are rapid rotators during their main-sequence. Therefore, we have to study stellar pulsations propagating in stably stratified, rotating, and potentially strongly magnetised radiative zones. We generalise the traditional approximation of rotation by taking simultaneously general axisymmetric differential rotation and azimuthal magnetic fields into account in a non-perturbative way. Using this new formalism, we derive the asymptotic properties of magneto-gravito-inertial (MGI) waves and their period spacings. We find that toroidal magnetic fields induce a shift in the period spacings of MGI modes. An equatorial azimuthal magnetic field with an amplitude of the order of $10^5\,\rm G$ leads to signatures that can be detectable thanks to modern space photometry. More complex hemispheric configurations are more difficult to observe.

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H. Dhouib, S. Mathis, L. Bugnet, et. al.
Tue, 22 Feb 22
42/77

Comments: 21 pages, 15 figures, 3 tables, abstract shortened for arXiv. Accepted for publication in A&A

Superrotation of Titan's stratosphere driven by the radiative heating of the haze layer [EPA]

http://arxiv.org/abs/2202.08397


Titan’s stratosphere has been observed in a superrotation state, where the atmosphere rotates many times faster than the surface does. Another characteristics of Titan’s atmosphere is the presence of thick haze layer. In this paper, we performed numerical experiments using a General Circulation Model (GCM), to explore the effects of the haze layer on the stratospheric superrotation. We employed a semi-gray radiation model of Titan’s atmosphere following McKay et al. (1999), which takes account of the sunlight absorption by haze particles. The phase change of methane or the seasonal changes were not taken into account. Our model with the radiation parameters tuned for Titan yielded the global eastward wind around the equator with larger velocities at higher altitudes except at around 70 km after $10^5$ Earth days. Although the atmosphere is not in an equilibrium state, the zonal wind profiles is approximately consistent with the observed one. Analysis on our experiments suggests that the quasi-stationary stratospheric superrotation is maintained by the balance between the meridional circulation decoupled from the surface, and the eddies that transport angular momentum equatorward. This is different from, but similar to, the so-called Gierasch mechanism, in which momentum is supplied from the surface. This structure may explain the no-wind region at about $80$ km in altitude.

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M. Sumi, S. Takehiro, W. Ohfuchi, et. al.
Fri, 18 Feb 22
44/63

Comments: 24 pages, 14 figures, accepted to the Astrophysical Journal

Dynamical regimes of polar vortices on terrestrial planets with a seasonal cycle [EPA]

http://arxiv.org/abs/2202.06270


Polar vortices are common planetary flows that encircle the pole in the middle or high latitudes, and are observed on most of the solar systems’ planetary atmospheres. The polar vortices on Earth, Mars, and Titan are dynamically related to the mean meridional circulation and exhibits a significant seasonal cycle. However, the polar vortex’s characteristics vary between the three planets. To understand the mechanisms that influence the polar vortex’s dynamics and dependence on planetary parameters, we use an idealized general circulation model with a seasonal cycle in which we varied the obliquity, rotation rate, and orbital period. We find that there are distinct regimes for the polar vortex seasonal cycle across the parameter space. Some regimes have similarities to the observed polar vortices, including a weakening of the polar vortex during midwinter at slow rotation rates, similar to Titan’s polar vortex. However, other regimes found within the parameter space have no counterpart in the solar system. In addition, we show that for a significant fraction of the parameter space, the vortex’s potential vorticity latitudinal structure is annular, similar to the observed structure of the polar vortex on Mars and Titan. We also find a suppression of storm activity during midwinter that resembles the suppression observed on Mars and Earth, which occurs in simulations where the jet speed is greater than ~60 ms$^{-1}$. This wide variety of polar vortex dynamical regimes that shares similarities to observed polar vortices suggests that among exoplanets, there can be a wide variability of polar vortices.

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I. Guendelman, D. Waugh and Y. Kaspi
Tue, 15 Feb 22
10/75

Comments: Accepted for publication in the Planetary Science Journal

A nitrogen-rich atmosphere on ancient Mars consistent with isotopic evolution models [EPA]

http://arxiv.org/abs/2202.04825


The ratio of nitrogen isotopes in the Martian atmosphere is a key constraint on the planet’s atmospheric evolution. However, enrichment of the heavy isotope expected due to atmospheric loss from sputtering and photochemical processes is greater than measurements. A massive, multi-bar early CO2-dominated atmosphere and recent volcanic outgassing have been proposed to explain this discrepancy, and many previous models have assumed atmospheric nitrogen rapidly reached a steady state where loss to space balanced volcanic outgassing. Here we show using time-dependent models that the abundance and isotopic composition of nitrogen in the Martian atmosphere can be explained by a family of evolutionary scenarios in which the initial partial pressure of nitrogen is sufficiently high that a steady state is not reached and nitrogen levels gradually decline to present-day values over 4 billion years. Our solutions do not require a multi-bar early CO2 atmosphere and are consistent with volcanic outgassing indicated by both geologic mapping and the atmospheric 36Ar/38Ar ratio. Monte Carlo simulations that include these scenarios estimate that the partial pressure of N2 was 60 – 740 mbar (90% confidence, with a median value of 310 mbar) at 3.8 billion years ago when the valley networks formed. We suggest that such a high nitrogen partial pressure could have contributed substantially to warming on early Mars.

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R. Hu and T. Thomas
Fri, 11 Feb 22
71/71

Comments: Nature Geoscience, published online on February 10, 2022, this https URL

Upward lightning at tall structures: Atmospheric drivers for trigger mechanisms and flash type [CL]

http://arxiv.org/abs/2201.05663


Despite its scarcity, upward lightning initiated from tall structures causes more damage than common downward lightning. One particular subtype with a continuous current only is not detectable by conventional lightning location systems (LLS) causing a significantly reduced detection efficiency. Upward lightning has become a major concern due to the recent push in the field of renewable wind energy generation . The growing number of tall wind turbines increased lightning related damages. Upward lightning may be initiated by the tall structure triggering the flash itself (self-triggered) or by a flash striking close by (other-triggered).
The major objective of this study is to find the driving atmospheric conditions influencing whether an upward flash is self-triggered or other-triggered and whether it is of the undetectable subtype. We explore upward flashes directly measured at the Gaisberg Tower in Salzburg (Austria) between 2000 and 2015. These upward flashes are combined with atmospheric reanalysis data stratified into five main meteorological groups: cloud physics, mass field, moisture field, surface exchange and wind field. We use classification methods based on tree-structured ensembles in form of conditional random forests. From these random forests we assess the meteorological influence and find the most important atmospheric drivers for one event or the other, respectively.

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I. Stucke, D. Morgenstern, A. Zeileis, et. al.
Wed, 19 Jan 22
54/121

Comments: N/A

Martian Dust Storms and Gravity Waves: Disentangling Water Transport to the Upper Atmosphere [EPA]

http://arxiv.org/abs/2201.05081


Simulations with the Max Planck Institute Martian general circulation model for Martian years 28 and 34 reveal details of the water “pump” mechanism and the role of gravity wave (GW) forcing. Water is advected to the upper atmosphere mainly by upward branches of the meridional circulation: in low latitudes during equinoxes and over the south pole during solstices. Molecular diffusion plays little role in water transport in the middle atmosphere and across the mesopause. GWs modulate the circulation and temperature during global dust storms, thus changing the timing and intensity of the transport. At equinoxes, they facilitate water accumulation in the polar warming regions in the middle atmosphere followed by stronger upwelling over the equator. As equinoctial storms decay, GWs tend to accelerate the reduction of water in the thermosphere. GWs delay the onset of the transport during solstitial storms and change the globally averaged amount of water in the upper atmosphere by 10-25%.

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D. Shaposhnikov, A. Medvedev, A. Rodin, et. al.
Fri, 14 Jan 22
17/52

Comments: N/A

Modeling the hydrological cycle in the atmosphere of Mars: Influence of a bimodal size distribution of aerosol nucleation particles [EPA]

http://arxiv.org/abs/2201.05086


We present a new implementation of the hydrological cycle scheme into a general circulation model of the Martian atmosphere. The model includes a semi-Lagrangian transport scheme for water vapor and ice, and accounts for microphysics of phase transitions between them. The hydrological scheme includes processes of saturation, nucleation, particle growth, sublimation and sedimentation under the assumption of a variable size distribution. The scheme has been implemented into the Max Planck Institute Martian general circulation model (MPI–MGCM) and tested assuming mono- and bimodal log-normal distributions of ice condensation nuclei. We present a comparison of the simulated annual variations, horizontal and vertical distributions of water vapor and ice clouds with the available observations from instruments onboard Mars orbiters. The accounting for bi-modality of aerosol particle distribution improves the simulations of the annual hydrological cycle, including predicted ice clouds mass, opacity, number density, particle radii. The increased number density and lower nucleation rates brings the simulated cloud opacities closer to observations. Simulations show a weak effect of the excess of small aerosol particles on the simulated water vapor distributions.

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D. Shaposhnikov, A. Rodin, A. Medvedev, et. al.
Fri, 14 Jan 22
20/52

Comments: N/A

An Energy Balance Model for Rapidly and Synchronously Rotating Terrestrial Planets [EPA]

http://arxiv.org/abs/2201.02685


This paper describes the Habitable Energy balance model for eXoplaneT ObseRvations (HEXTOR), which is a model for calculating latitudinal temperature profiles on Earth and other rapidly rotating planets. HEXTOR includes a lookup table method for calculating the outgoing infrared radiative flux and planetary albedo, which provides improvements over other approaches at parameterizing radiative transfer in an energy balance model. Validation cases are presented for present-day Earth and other Earth-sized planets with aquaplanet and land planet conditions from 0 to 45 degrees obliquity. A tidally locked coordinate system is also implemented in the energy balance model, which enables calculation of the horizontal temperature profile for planets in synchronous rotation around low mass stars. This coordinate transformed model is applied to cases for TRAPPIST-1e as defined by the TRAPPIST Habitable Atmosphere Intercomparison protocol, which demonstrates better agreement with general circulation models compared to the latitudinal energy balance model. Advances in applying energy balance models to exoplanets can be made by using general circulation models as a benchmark for tuning as well as by conducting intercomparisions between energy balance models with different physical parameterizations.

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J. Haqq-Misra and B. Hayworth
Tue, 11 Jan 22
73/95

Comments: Accepted by the Planetary Science Journal, 14 pages, 6 figures

Towards RNA life on Early Earth: From atmospheric HCN to biomolecule production in warm little ponds [EPA]

http://arxiv.org/abs/2201.00829


The origin of life on Earth involves the early appearance of an information-containing molecule such as RNA. The basic building blocks of RNA could have been delivered by carbon-rich meteorites, or produced in situ by processes beginning with the synthesis of hydrogen cyanide (HCN) in the early Earth’s atmosphere. Here, we construct a robust physical and non-equilibrium chemical model of the early Earth atmosphere. The atmosphere is supplied with hydrogen from impact degassing of meteorites, sourced with water evaporated from the oceans, carbon dioxide from volcanoes, and methane from undersea hydrothermal vents, and in which lightning and external UV-driven chemistry produce HCN. This allows us to calculate the rain-out of HCN into warm little ponds (WLPs). We then use a comprehensive sources and sinks numerical model to compute the resulting abundances of nucleobases, ribose, and nucleotide precursors such as 2-aminooxazole resulting from aqueous and UV-driven chemistry within them. We find that at 4.4 bya (billion years ago) peak adenine concentrations in ponds can be maintained at ~2.8$\mu$M for more than 100 Myr. Meteorite delivery of adenine to WLPs produce similar peaks in concentration, but are destroyed within months by UV photodissociation, seepage, and hydrolysis. The early evolution of the atmosphere is dominated by the decrease of hydrogen due to falling impact rates and atmospheric escape, and the rise of oxygenated species such as OH from H2O photolysis. Our work points to an early origin of RNA on Earth within ~200 Myr of the Moon-forming impact.

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B. Pearce, K. Molaverdikhani, R. Pudritz, et. al.
Wed, 5 Jan 22
14/54

Comments: Accepted to ApJ, 27 pages (14 main text), 11 figures, 9 tables

A study on UV emission from clouds with Mini-EUSO [CL]

http://arxiv.org/abs/2112.11878


Mini-EUSO is the first mission of the JEM-EUSO program located on the International Space Station. One of the main goals of the mission is to provide valuable scientific data in view of future large missions devoted to study Ultra-High Energy Cosmic Rays (UHECRs) from space by exploiting the fluorescence emission generated by Extensive Air Showers (EAS) developing in the atmosphere. A space mission like Mini-EUSO experiences continuous changes in atmospheric conditions, including the cloud presence. The influence of clouds on space-based observation is, therefore, an important topic to investigate as it might alter the instantaneous exposure for EAS detection or deteriorate the quality of the EAS images with consequences on the reconstructed EAS parameters. For this purpose, JEM-EUSO is planning to have an IR camera and a lidar as part of its Atmospheric Monitoring System. At the same time, it would be extremely beneficial if the UV camera itself would be able to detect the presence of clouds, at least in some specific conditions. For this reason, we analyze a few case studies by comparing the pixel count rates from Mini-EUSO during orbits with the cloud cover (as cloud fraction). This quantity is retrieved from the Global Forecast System (GFS) model at different height levels over the Mini-EUSO trajectory. The results of this analysis are reported.

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A. Golzio, M. Battisti, M. Beratina, et. al.
Thu, 23 Dec 21
1/63

Comments: 12 pages, 5 figures, 1 table Proceedings of the 37th International Cosmic Ray Conference (ICRC 2021)

Production of Ammonia Makes Venusian Clouds Habitable and Explains Observed Cloud-Level Chemical Anomalies [EPA]

http://arxiv.org/abs/2112.10850


The atmosphere of Venus remains mysterious, with many outstanding chemical connundra. These include: the unexpected presence of ~10 ppm O2 in the cloud layers; an unknown composition of large particles in the lower cloud layers; and hard to explain measured vertical abundance profiles of SO2 and H2O. We propose a new hypothesis for the chemistry in the clouds that largely addresses all of the above anomalies. We include ammonia (NH3), a key component that has been tentatively detected both by the Venera 8 and Pioneer Venus probes. NH3 dissolves in some of the sulfuric acid cloud droplets, effectively neutralizing the acid and trapping dissolved SO2 as ammonium sulfite salts. This trapping of SO2 in the clouds together with the release of SO2 below the clouds as the droplets settle out to higher temperatures, explains the vertical SO2 abundance anomaly. A consequence of the presence of NH3 is that some Venus cloud droplets must be semi-solid ammonium salt slurries, with a pH~1, which matches Earth acidophile environments, rather than concentrated sulfuric acid. The source of NH3 is unknown, but could involve biological production; if so, then the most energy-efficient NH3-producing reaction also creates O2, explaining the detection of O2 in the cloud layers. Our model therefore predicts that the clouds are more habitable than previously thought, and may be inhabited. Unlike prior atmospheric models, ours does not require forced chemical constraints to match the data. Our hypothesis, guided by existing observations, can be tested by new Venus in situ measurements.

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W. Bains, J. Petkowski, P. Rimmer, et. al.
Wed, 22 Dec 21
26/67

Comments: N/A

Monte Carlo Simulation of CRAND Protons Trapped at Low Earth Orbits [EPA]

http://arxiv.org/abs/2112.08677


The Cosmic Ray Albedo Neutron Decay (CRAND) is believed to be the principal mechanism for the formation of inner proton radiation belt — at least for relatively higher energy particles. We implement this mechanism in a Monte Carlo simulation procedure to calculate the trapped proton radiation at the low Earth orbits, through event-by-event interaction of the cosmic ray particles in the Earth’s atmosphere and their transportation in the magnetosphere. We consider the generation of protons from subsequent decay of the secondary neutrons from the cosmic ray interaction in the atmosphere and their transport (and/or trapping) in the geomagnetic field. We address the computational challenges for this type of calculations and develop an optimized algorithm to minimize the computation time. We consider a full 3D description of the Earth’s atmospheric and magnetic-field configurations using the latest available models. We present the spatial and phase-space distribution of the trapped protons considering the adiabatic invariants and other parameters at the low Earth orbits. We compare the simulation results with the trapped proton flux measurements made by PAMELA experiment at low Earth orbit and explain certain features observed by the measurement.

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R. Sarkar and A. Roy
Fri, 17 Dec 21
63/72

Comments: 28 pages, 11 figures, Accepted for publication in Advances in Space Research

Deliquescence probability maps of Mars and key limiting factors using GCM model calculations [EPA]

http://arxiv.org/abs/2112.08287


There may be a chance of small-scale ephemeral liquid water formation on present day Mars, even though the current climate does not support the existence of larger bodies of water. Through a process called deliquescence, hygroscopic salts can enter solution by absorbing water vapor directly from the atmosphere. Due to the absence of in-situ deliquescence experiments so far, the most reliable way to forecast deliquescence is through atmospherical modeling, however, the locations and times when salty liquid water could emerge are not yet well known. In this paper we present our results of likely brine formation on Mars, their proposed locations and seasons, as well as the possible limiting factors. For our calculations we used the data of Laboratoire de M\’et\’eorologie Dynamique Mars General Circulation Model version 5. The results show that from L$_s$ 35$^\circ$ – L$_s$ 160$^\circ$, between 9 PM and 11 PM there is a good chance for calcium perchlorate deliquescence above 30$^\circ$ N, while in this zone the ideal regions are concentrated mostly to Acidalia Planitia and Utopia Planitia between 1 AM and 3 AM. We found that in the Southern Hemisphere, between L$_s$ 195$^\circ$ and L$_s$ 320$^\circ$, there is a noticeable, but weaker band in the vicinity of 60$^\circ$ S, and both Argyre Planitia and Hellas Planitia show some chance for brine formation. According to our statistics the key limiting factor of deliquescence could be relative humidity in most cases. Our results suggest that during summer — early fall seasons, there could be deliquescence in both hemispheres in specific areas from the late evening until the early morning hours. There are only few studies detailing the geological and temporal distribution of brine formation through deliquescence, thus this work could be used as a good guide for future landing site analysis or in choosing a specific location for further research.

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B. Pál and &. Kereszturi
Thu, 16 Dec 21
76/83

Comments: Accepted for publication in Icarus (arXiv version is Review 1, final version will be online soon on Icarus website)

Local-time Dependence of Chemical Species in the Venusian Mesosphere [EPA]

http://arxiv.org/abs/2112.07037


Observed chemical species in the Venusian mesosphere show local-time variabilities. SO2 at the cloud top exhibits two local maxima over local time, H2O at the cloud top is uniformly distributed, and CO in the upper atmosphere shows a statistical difference between the two terminators. In this study, we investigated these local-time variabilities using a three-dimensional (3D) general circulation model (GCM) in combination with a two-dimensional (2D) chemical transport model (CTM). Our simulation results agree with the observed local-time patterns of SO2, H2O, and CO. The two-maximum pattern of SO2 at the cloud top is caused by the superposition of the semidiurnal thermal tide and the retrograde superrotating zonal (RSZ) flow. SO2 above 85 km shows a large day-night difference resulting from both photochemistry and the sub-solar to anti-solar (SS-AS) circulation. The transition from the RSZ flows to SS-AS circulation can explain the CO difference between two terminators and the displacement of the CO local-time maximum with respect to the anti-solar point. H2O is long-lived and exhibits very uniform distribution over space. We also present the local-time variations of HCl, ClO, OCS and SO simulated by our model and compare to the sparse observations of these species. This study highlights the importance of multidimensional CTMs for understanding the interaction between chemistry and dynamics in the Venusian mesosphere.

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W. Shao, X. Zhang, J. Mendonça, et. al.
Wed, 15 Dec 21
25/85

Comments: 51 pages, 19 figures, accepted by Planetary Science Journal

Convection modeling of pure-steam atmospheres [EPA]

http://arxiv.org/abs/2111.15265


Condensable species are crucial in shaping planetary climate. A wide range of planetary climate systems involve understanding non-dilute condensable substances and their influence on climate dynamics. There has been progress on large-scale dynamical effects and on 1D convection parameterization, but resolved 3D moist convection remains unexplored in non-dilute conditions, though it can have a profound impact on temperature/humidity profiles and cloud structure. We tackle this problem for pure-steam atmospheres using three-dimensional, high-resolution numerical simulations of convection in post-runaway atmospheres where the water reservoir at the surface has been exhausted. We show that the atmosphere is comprised of two characteristic regions, an upper condensing region dominated by gravity waves and a lower noncondensing region characterized by convective overturning cells. Velocities in the condensing region are much smaller than those in the lower noncondensing region, and the horizontal temperature variation is small overall. Condensation in the thermal photosphere is largely driven by radiative cooling and tends to be statistically homogeneous. Some condensation also happens deeper, near the boundary of the condensing region, due to triggering by gravity waves and convective penetrations and exhibit random patchiness. This qualitative structure is insensitive to varying model parameters, but quantitative details may differ. Our results confirm theoretical expectations that atmospheres close to the pure-steam limit do not have organized deep convective plumes in the condensing region. The generalized convective parameterization scheme discussed in Ding & Pierrehumbert (2016) is appropriate to handle the basic structure of atmospheres near the pure-steam limit but is difficult to capture gravity waves and their mixing that appear in 3D convection-resolving models.

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X. Tan, M. Lefevre and R. Pierrehumbert
Wed, 1 Dec 21
97/110

Comments: 10 pages, 4 figures, accepted to ApJL

Longitudinally asymmetric stratospheric oscillation on a tidally locked exoplanet [EPA]

http://arxiv.org/abs/2111.11281


Using a three-dimensional general circulation model, we show that the atmospheric dynamics on a tidally locked Earth-like exoplanet, simulated with the planetary and orbital parameters of Proxima Centauri b, support a longitudinally asymmetric stratospheric wind oscillation (LASO), analogous to Earth’s quasi-biennial oscillation (QBO). In our simulations, the LASO has a vertical extent of 35–55 km, a period of 5–6.5 months, and a peak-to-peak wind speed amplitude of -70 to +130 m/s with a maximum at an altitude of 41 km. Unlike the QBO, the LASO displays longitudinal asymmetries related to the asymmetric thermal forcing of the planet and to interactions with the resulting stationary Rossby waves. The equatorial gravity wave sources driving the LASO are localised in the deep convection region at the substellar point and in a jet exit region near the western terminator, unlike the QBO, for which these sources are distributed uniformly around the planet. Longitudinally, the western terminator experiences the highest wind speeds and undergoes reversals earlier than other longitudes. The antistellar point only experiences a weak oscillation with a very brief, low-speed westward phase. The QBO on Earth is associated with fluctuations in the abundances of water vapour and trace gases such as ozone which are also likely to occur on exoplanets if these gases are present. Strong fluctuations in temperature and the abundances of atmospheric species at the terminators will need to be considered when interpreting atmospheric observations of tidally locked exoplanets.

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M. Cohen, M. Bollasina, P. Palmer, et. al.
Tue, 23 Nov 21
10/84

Comments: 18 pages, 7 figures

Observation of Variations in Cosmic Ray Single Count Rates During Thunderstorms and Implications for Large-Scale Electric Field Changes [HEAP]

http://arxiv.org/abs/2111.09962


We present the first observation by the Telescope Array Surface Detector (TASD) of the effect of thunderstorms on the development of cosmic ray single count rate intensity over a 700 km$^{2}$ area. Observations of variations in the secondary low-energy cosmic ray counting rate, using the TASD, allow us to study the electric field inside thunderstorms, on a large scale, as it progresses on top of the 700 km$^{2}$ detector, without dealing with the limitation of narrow exposure in time and space using balloons and aircraft detectors. In this work, variations in the cosmic ray intensity (single count rate) using the TASD, were studied and found to be on average at the $\sim(0.5-1)\%$ and up to 2\% level. These observations were found to be both in excess and in deficit. They were also found to be correlated with lightning in addition to thunderstorms. These variations lasted for tens of minutes; their footprint on the ground ranged from 6 to 24 km in diameter and moved in the same direction as the thunderstorm. With the use of simple electric field models inside the cloud and between cloud to ground, the observed variations in the cosmic ray single count rate were recreated using CORSIKA simulations. Depending on the electric field model used and the direction of the electric field in that model, the electric field magnitude that reproduces the observed low-energy cosmic ray single count rate variations was found to be approximately between 0.2-0.4 GV. This in turn allows us to get a reasonable insight on the electric field and its effect on cosmic ray air showers inside thunderstorms.

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R. Abbasi, T. Abu-Zayyad, M. Allen, et. al.
Mon, 22 Nov 21
2/53

Comments: N/A

Near ground horizontal high resolution $C_n^2$ profiling from Shack-Hartmann slope and scintillation data [IMA]

http://arxiv.org/abs/2111.08003


CO-SLIDAR is a very promising technique for the metrology of near ground $C_n^2$ profiles. It exploits both phase and scintillation measurements obtained with a dedicated wavefront sensor and allows profiling on the full line of sight between pupil and sources. This technique is applied to an associated instrument based on a mid-IR Shack-Hartmann wavefront sensor, coupled to a 0.35 m telescope, which observes two cooperative sources. This paper presents the first comprehensive description of the CO-SLIDAR method in the context of near ground optical turbulence metrology. It includes the presentation of the physics principles underlying the measurements, of our unsupervised $C_n^2$ profile reconstruction strategy together with the error bar estimation on the reconstructed values. The application to data acquired in a heterogeneous rural landscape during an experimental campaign in Lannemezan (France) demonstrates the ability to obtain profiles with a sampling pitch of about 220 m over a 2.7 km line of sight. The retrieved $C_n^2$ profiles are presented and their variability in space and time is discussed.

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C. Sauvage, C. Robert, L. Mugnier, et. al.
Wed, 17 Nov 21
17/64

Comments: N/A

Episodic deluges in simulated hothouse climates [EPA]

http://arxiv.org/abs/2111.03109


Earth’s distant past and potentially its future include extremely warm “hothouse” climate states, but little is known about how the atmosphere behaves in such states. One distinguishing characteristic of hothouse climates is that they feature lower-tropospheric radiative heating, rather than cooling, due to the closing of the water vapor infrared window regions. Previous work has suggested that this could lead to temperature inversions and significant changes in cloud cover, but no previous modeling of the hothouse regime has resolved convective-scale turbulent air motions and cloud cover directly, thus leaving many questions about hothouse radiative heating unanswered. Here, we conduct simulations that explicitly resolve convection and find that lower-tropospheric radiative heating in hothouse climates causes the hydrologic cycle to shift from a quasi-steady regime to a “relaxation oscillator” regime, in which precipitation occurs in short and intense outbursts separated by multi-day dry spells. The transition to the oscillatory regime is accompanied by strongly enhanced local precipitation fluxes, a significant increase in cloud cover, and a transiently positive (unstable) climate feedback parameter. Our results indicate that hothouse climates may feature a novel form of “temporal” convective self-organization, with implications for both cloud coverage and erosion processes.

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J. Seeley and R. Wordsworth
Mon, 8 Nov 21
16/69

Comments: N/A

Trajectory-based simulation of far-infrared CIA profiles of CH$_4-$N$_2$ for modeling Titan's atmosphere [EPA]

http://arxiv.org/abs/2111.02312


We report the results of the trajectory-based simulation of far-infrared collision-induced absorption (CIA) due to CH$_4-$N$_2$ pairs at temperatures between 70 and 400 K. Our analysis utilizes recently calculated high-level potential energy (PES) and induced dipole surfaces (IDS) [Finenko, A. A., Chistikov, D. N., Kalugina, Y. N., Conway E. K., Gordon, I. E., Phys. Chem. Chem. Phys., 2021, doi: 10.1039/d1cp02161c]. Treating collision partners as rigid rotors, the time evolution of interaction-induced dipole is accumulated over a vast ensemble of classical trajectories and subsequently transformed into CIA spectrum via Fourier transform. In our calculations, both bound and unbound states are properly accounted for, and the rigorous theory of lower-order spectral moments is addressed to check the accuracy of simulated profiles. Classically derived trajectory-based profiles are subject to two approximate desymmetrization procedures so that resulting profiles conform to the quantum principle of detailed balance. The simulated profiles are compared to laboratory measurements and employed for modeling Titan’s spectra in the 50-500 cm$^{-1}$ range. Based on the desymmetrized simulated profiles, a new semi-empirical model for CH$_4-$N$_2$ CIA is proposed for modeling Titan’s infrared spectra. Synthetic spectra derived using this model yield an excellent agreement with the data recorded by the Composite Infrared Spectrometer (CIRS) aboard the Cassini spacecraft at low and high emission angles.

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A. Finenko, B. Bézard, I. Gordon, et. al.
Thu, 4 Nov 21
16/73

Comments: 18 pages, 11 figures, accepted for publication in ApJS . The semiempirical CH4-N2 profiles tabulated in the HITRAN CIA format are available on the ApJS website or upon reasonable request

The Scientific Observation Campaign of the Hayabusa-2 Capsule Re-entry [EPA]

http://arxiv.org/abs/2111.02235


On 5th December 2020 at 17:28 UTC, the Japan Aerospace Exploration Agency’s Hayabusa-2 sample return capsule came back to the Earth. It re-entered the atmosphere over South Australia, visible for 53 seconds as a fireball from near the Northern Territory border toward Woomera where it landed in the the Woomera military test range. A scientific observation campaign was planned to observe the optical, seismo-acoustic, radio and high energy particle phenomena associated with the entry of an interplanetary object. A multi-institutional collaboration between Australian and Japanese universities resulted in the deployment of 49 instruments, with a further 13 permanent observation sites. The campaign successfully recorded optical, seismo-acoustic and spectral data for this event which will allow an in depth analysis of the effects produced by interplanetary objects impacting the Earth’s atmosphere. This will allow future comparison and insights to be made with natural meteoroid objects.

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E. Sansom, H. Devillepoix, M. Yamamoto, et. al.
Thu, 4 Nov 21
52/73

Comments: accepted in Publications of the Astronomical Society of Japan

Self-preserving ice layers on CO2 clathrate particles: implications for Enceladus, Pluto and similar ocean worlds [EPA]

http://arxiv.org/abs/2110.15769


Under both engineering and natural conditions on Earth and in the Universe, some gas hydrates are found to be stabilised outside their window of thermodynamic stability by the formation of an ice layer-a phenomenon termed self-preservation. Low occupancy surface regions on type I CO2 clathrate structures together with the self-preserving ice layer lead to an effective buoyancy for these structures which restricts the size range of particles that float in the ocean on Enceladus, Pluto and similar oceanic worlds. Our goal here is to investigate the implications of Lifshitz forces and low occupancy surface regions on clathrate structures for their self-preservation through ice layer formation, presenting a plausible model based on multilayer interactions through dispersion forces. We predict that the growth of an ice layer between 0.01 and 0.2 $\mu$m thick on CO2 clathrate surfaces depends on the presence of surface regions in the gas hydrates with low occupancy. The effective particle density is estimated delimiting a range of particles that would be buoyant in different oceans. Over geological time, deposition of floating CO2 hydrates could result in the accumulation of kilometre-thick hydrate layers above liquid water reservoirs, and below the water ice crusts of their respective ocean worlds. On Enceladus, destabilisation of near-surface hydrate deposits could lead to increased gas pressures that both drive plumes and entrain stabilised hydrates to be redeposited on the surface of Enceladus or ejected into the E-ring of Saturn. On ocean worlds such as Enceladus and particularly Pluto, the accumulation of thick CO2 hydrate deposits could insulate its ocean against freezing. In preventing the freezing of liquid water reservoirs in ocean worlds, the presence of CO2 hydrate layers could enhance the habitability of ocean worlds in our solar systems and on the exoplanets and exomoons beyond.

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M. Boström, V. Esteso, J. Fiedler, et. al.
Mon, 1 Nov 21
27/58

Comments: N/A

Using the Climate App to learn about Planetary Habitability and Climate Change [CL]

http://arxiv.org/abs/2110.14087


Simple climate models have been around for more than a century but have recently come back into fashion: they are useful for explaining global warming and the habitability of extrasolar planets. The Climate App (https://www.climateapp.ca) is an interactive web-based application that describes the radiative transfer governing planetary climate. The App is currently available in French and English and is suitable for teaching high-school through college students, or public outreach. The beginner version can be used to explore the greenhouse effect and planetary albedo, sufficient for explaining anthropogenic climate change, the Faint Young Sun Paradox, the habitability of TRAPPIST planets and other simple scenarios. There is also an advanced option with more atmospheric layers and incorporating the absorption and scattering of shortwave radiation for students and educators wishing a deeper dive into atmospheric radiative transfer. A number of pedagogical activities are being beta tested and rolled out.

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L. Zhu, A. Courchesne and N. Cowan
Thu, 28 Oct 21
42/76

Comments: 8 pages, 4 figures. A summarized version is included in International Astronomical Union CAP2021 conference proceedings

EOS: Atmospheric Radiative Transfer in Habitable Worlds with HELIOS [EPA]

http://arxiv.org/abs/2110.11702


We present EOS, a procedure for determining the Outgoing Longwave Radiation (OLR) and top-of-atmosphere (TOA) albedo for a wide range of conditions expected to be present in the atmospheres of rocky planets with temperate conditions. EOS is based on HELIOS and HELIOS-K, which are novel and publicly available atmospheric radiative transfer (RT) codes optimized for fast calculations with GPU processors. These codes were originally developed for the study of giant planets. In this paper we present an adaptation for applications to terrestrial-type, habitable planets, adding specific physical recipes for the gas opacity and vertical structure of the atmosphere. To test the reliability of the procedure we assessed the impact of changing line opacity profile, continuum opacity model, atmospheric lapse rate and tropopause position prescriptions on the OLR and the TOA albedo. The results obtained with EOS are in line with those of other RT codes running on traditional CPU processors, while being at least one order of magnitude faster. The adoption of OLR and TOA albedo data generated with EOS in a zonal and seasonal climate model correctly reproduce the fluxes of the present-day Earth measured by the CERES spacecraft. The results of this study disclose the possibility to incorporate fast RT calculations in climate models aimed at characterizing the atmospheres of habitable exoplanets.

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P. Simonetti, G. Vladilo, L. Silva, et. al.
Mon, 25 Oct 21
7/76

Comments: Accepted for publication in ApJ

General Circulation Model Errors are Variable across Exoclimate Parameter Spaces [EPA]

http://arxiv.org/abs/2110.10925


General circulation models are often used to explore exoclimate parameter spaces and classify atmospheric circulation regimes. Models are tuned to give reasonable climate states for standard test cases, such as the Held-Suarez test, and then used to simulate diverse exoclimates by varying input parameters such as rotation rates, instellation, atmospheric optical properties, frictional timescales and so on. In such studies, there is an implicit assumption that the model which works reasonably well for the standard test case will be credible at all points in an arbitrarily wide parameter space. Here, we test this assumption using the open-source general circulation model THOR to simulate atmospheric circulation on tidally locked Earth-like planets with rotation periods of 0.1 to 100 days. We find that the model error, as quantified by the ratio between physical and spurious numerical contributions to the angular momentum balance, is extremely variable across this range of rotation periods with some cases where numerical errors are the dominant component. Increasing model grid resolution does improve errors but using a higher-order numerical diffusion scheme can sometimes magnify errors for finite-volume dynamical solvers. We further show that to minimize error and make the angular momentum balance more physical within our model, the surface friction timescale must be smaller than the rotational timescale.

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P. Kopparla, R. Deitrick, K. Heng, et. al.
Fri, 22 Oct 21
72/133

Comments: 8 pages, 5 figures, accepted by ApJ

The number and location of Jupiter's circumpolar cyclones explained by vorticity dynamics [EPA]

http://arxiv.org/abs/2110.09422


The Juno mission observed that both poles of Jupiter have polar cyclones that are surrounded by a ring of circumpolar cyclones. The North Pole holds eight circumpolar cyclones and the South Pole possesses five, with both circumpolar rings positioned along latitude ~84{\deg} N/S. Here we explain the location, stability, and number of the Jovian circumpolar cyclones by establishing the primary forces that act on them, which develop because of vorticity gradients in the background of a cyclone. In the meridional direction, the background vorticity varies owning to the planetary sphericity and the presence of the polar cyclone. In the zonal direction, the vorticity varies by the presence of adjacent cyclones in the ring. Our analysis successfully predicts the latitude and number of circumpolar cyclones for both poles, according to the size and spin of the respective polar cyclone. Moreover, the analysis successfully predicts that Jupiter can hold circumpolar cyclones while Saturn currently cannot. The match between the theory and observations implies that vortices in the polar regions of the giant planets are largely governed by barotropic dynamics, and that the movement of other vortices at high-latitudes is also driven by interaction with the background vorticity.

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N. Gavriel and Y. Kaspi
Tue, 19 Oct 21
3/98

Comments: 13 Pages, 8 figures

Day-night cloud asymmetry prevents early oceans on Venus but not on Earth [EPA]

http://arxiv.org/abs/2110.08801


Earth has had oceans for nearly four billion years and Mars had lakes and rivers 3.5-3.8 billion years ago. However, it is still unknown whether water has ever condensed on the surface of Venus because the planet – now completely dry – has undergone global resurfacing events that obscure most of its history. The conditions required for water to have initially condensed on the surface of Solar System terrestrial planets are highly uncertain, as they have so far only been studied with one-dimensional numerical climate models that cannot account for the effects of atmospheric circulation and clouds, which are key climate stabilizers. Here we show using three-dimensional global climate model simulations of early Venus and Earth that water clouds – which preferentially form on the nightside, owing to the strong subsolar water vapour absorption – have a strong net warming effect that inhibits surface water condensation even at modest insolations (down to 325 W/m2, that is, 0.95 times the Earth solar constant). This shows that water never condensed and that, consequently, oceans never formed on the surface of Venus. Furthermore, this shows that the formation of Earth’s oceans required much lower insolation than today, which was made possible by the faint young Sun. This also implies the existence of another stability state for present-day Earth: the ‘Steam Earth’, with all the water from the oceans evaporated into the atmosphere.

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M. Turbet, E. Bolmont, G. Chaverot, et. al.
Tue, 19 Oct 21
91/98

Comments: Published in Nature (13 October 2021)

Determination of uncertainty profiles in neutral atmospheric properties measured by radio occultation experiments [EPA]

http://arxiv.org/abs/2110.09448


Radio occultations are commonly used to assess remotely atmospheric properties of planets or satellites within the solar system. The data processing usually involves the so-called Abel inversion method or the numerical ray-tracing technique. Both are now well established, however, they do not allow to easily determine the uncertainty profiles in atmospheric properties, and this makes results difficult to interpret statistically. Recently, a purely analytical approach based on the time transfer functions formalism was proposed for modeling radio occultation data. Using this formulation, we derive uncertainty relationships between the frequency shift and neutral atmosphere properties such as temperature, pressure, and neutral number density. These expressions are relevant for interpreting previous results from past radio occultation experiments and for deriving the system requirements for future missions in a rigorous manner, and consistently with the scientific requirements about the atmospheric properties retrieval.

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A. Bourgoin, E. Gramigna, M. Zannoni, et. al.
Tue, 19 Oct 21
93/98

Comments: 16 pages, 5 figures, 1 table

Seasonal Variability of the Daytime and Nighttime Atmospheric Turbulence Experienced by InSight on Mars [EPA]

http://arxiv.org/abs/2110.06113


The InSight mission, featuring continuous high-frequency high-sensitivity pressure measurements, is in ideal position to study the active atmospheric turbulence of Mars. Data acquired during 1.25 Martian year allows us to study the seasonal evolution of turbulence and its diurnal cycle. We investigate vortices (abrupt pressure drops), local turbulence (frequency range 0.01-2 Hz) and non-local turbulence often caused by convection cells and plumes (frequency range 0.002-0.01 Hz).
Contrary to non-local turbulence, local turbulence is strongly sensitive at all local times and seasons to the ambient wind. We report many remarkable events with the arrival of northern autumn at the InSight landing site: a spectacular burst of daytime vortices, the appearance of nighttime vortices, and the development of nighttime local turbulence as intense as its daytime counterpart. Nighttime turbulence at this dusty season appears as a result of the combination of a stronger low-level jet, producing shear-driven turbulence, and a weaker stability.

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A. Chatain, A. Spiga, D. Banfield, et. al.
Wed, 13 Oct 21
20/80

Comments: 15 pages, 5 figures, revised version of the manuscript submitted to GRL

The traditional approximation of rotation for rapidly rotating stars and planets. II. Deformation and differential rotation [SSA]

http://arxiv.org/abs/2110.03619


We examine the dynamics of low-frequency gravito-inertial waves (GIWs) in differentially rotating deformed radiation zones in stars and planets by generalising the traditional approximation of rotation (TAR). The TAR treatment was built on the assumptions that the star is spherical and uniformly rotating. However, it has been generalised in our previous work by including the effects of the centrifugal deformation using a non-perturbative approach in the uniformly rotating case. We aim to carry out a new generalisation of the TAR treatment to account for the differential rotation and the strong centrifugal deformation simultaneously. We generalise our previous work by taking into account the differential rotation in the derivation of our complete analytical formalism that allows the study of the dynamics of GIWs in differentially and rapidly rotating stars. We derived the complete set of equations that generalises the TAR, simultaneously taking the full centrifugal acceleration and the differential rotation into account. Within the validity domain of the TAR, we derived a generalised Laplace tidal equation for the horizontal eigenfunctions and asymptotic wave periods of the GIWs, which can be used to probe the structure and dynamics of differentially rotating deformed stars with asteroseismology. A new generalisation of the TAR, which simultaneously takes into account the differential rotation and the centrifugal acceleration in a non-perturbative way, was derived. This generalisation allowed us to study the detectability and the signature of the differential rotation on GIWs in rapidly rotating deformed stars and planets. We found that the effects of the differential rotation in early-type deformed stars on GIWs is theoretically largely detectable in modern space photometry using observations from $\textit{Kepler}$ and TESS.

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H. Dhouib, V. Prat, T. Reeth, et. al.
Fri, 8 Oct 21
67/70

Comments: 13 pages, 11 figures, 1 table, abstract shortened for arXiv. Accepted for publication in A&A. arXiv admin note: substantial text overlap with arXiv:2104.09302

Interferometric imaging of Intensely Radiating Negative Leaders [CL]

http://arxiv.org/abs/2110.02547


The common phenomenon of lightning still harbors many secrets and only recently a new propagation mode was observed for negative leaders. While propagating in this `Intensely Radiating Negative Leader’ (IRNL) mode a negative leader emits 100 times more very-high frequency (VHF) and broadband radiation than a more normal negative leader. We have reported that this mode occurs soon after initiation of all lightning flashes we have mapped as well as sometimes long thereafter. Because of the profuse emission of VHF the leader structure is very difficult to image. In this work we report on measurements made with the LOFAR radio telescope, an instrument primarily built for radio-astronomy observations. For this reason, as part of the present work, we have refined our time resolved interferometric 3-Dimensional (TRI-D) imaging to take into account the antenna function. The images from the TRI-D imager show that during an IRNL there is an ionization front with a diameter in excess of 500~m where strong corona bursts occur. This is very different from what is seen for a normal negative leader where the corona bursts happen at the tip, an area of typically 10~m in diameter. The observed massive ionization wave supports the idea that this mode is indicative of a dense charge pocket.

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O. Scholten, B. Hare, J. Dwyer, et. al.
Thu, 7 Oct 21
8/51

Comments: 13 pages, 5 figures

Towards Adaptive Simulations of Dispersive Tsunami Propagation from an Asteroid Impact [CL]

http://arxiv.org/abs/2110.01420


The long-term goal of this work is the development of high-fidelity simulation tools for dispersive tsunami propagation. A dispersive model is especially important for short wavelength phenomena such as an asteroid impact into the ocean, and is also important in modeling other events where the simpler shallow water equations are insufficient. Adaptive simulations are crucial to bridge the scales from deep ocean to inundation, but have difficulties with the implicit system of equations that results from dispersive models. We propose a fractional step scheme that advances the solution on separate patches with different spatial resolutions and time steps. We show a simulation with 7 levels of adaptive meshes and onshore inundation resulting from a simulated asteroid impact off the coast of Washington. Finally, we discuss a number of open research questions that need to be resolved for high quality simulations.

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M. Berger and R. LeVeque
Tue, 5 Oct 21
11/72

Comments: 16 pages, 5 figures, submitted to Proc. International Congress of Mathematicians, 2022