Tag Archives: Nuclear Experiment

Astrophysics in the Laboratory: The CBM Experiment at FAIR [CL]

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http://arxiv.org/abs/2004.11214


The future Facility for Antiproton and Ion Research (FAIR) is an accelerator-based international center for fundamental and applied research, which presently is under construction in Darmstadt, Germany. An important part of the program is devoted to questions related to astrophysics, including the origin of elements in the universe and the properties of strongly interacting matter under extreme conditions, which are relevant for our understanding of the structure of neutron stars and the dynamics of supernova explosions and neutron star mergers. The Compressed Baryonic Matter (CBM) experiment at FAIR is designed to measure promising observables in high-energy heavy-ion collisions, which are expected to be sensitive to the high-density equation-of-state (EOS) of nuclear matter and to new phases of QCD matter at high densities. The CBM physics program, the relevant observables and the experimental setup will be discussed.

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P. Senger
Fri, 24 Apr 20
49/63

Comments: 16 pages, 9 figures, Selected Papers from The Modern Physics of Compact Stars and Relativistic Gravity 2019

Direct measurement of the terrestrial $^7$Be $L/K$ capture ratio in cryogenic tantalum [CL]

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http://arxiv.org/abs/2003.04921


We report a high-statistics measurement of the $L/K$ orbital electron capture (EC) ratio in $^7$Be embedded in cryogenic Ta. The thin Ta film formed part of a high-resolution superconducting tunnel junction (STJ) radiation detector that was used to identify the signals from different decay channels. The measured $L/K$ capture ratio of 0.070(7) is significantly larger than the only previous measurement of this quantity and the theoretical predictions that include in-medium effects. This result brings into question the accuracy of the extrapolated $L/K$ ratio currently used in calculations of the $^7$Be destruction rate in astrophysical environments relevant to solar and galactic neutrino modeling, and the cosmological lithium problem. This Letter presents the first experiment that uses STJs for nuclear-recoil detection, opening a new experimental avenue for low-energy precision measurements with rare isotopes.

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S. Fretwell, K. Leach, C. Bray, et. al.
Thu, 12 Mar 20
21/49

Comments: 5 pages, 3 figures. Submitted to Physical Review Letters

Energy resolution and linearity in the keV to MeV range measured in XENON1T [CL]

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http://arxiv.org/abs/2003.03825


Xenon dual-phase time projection chambers designed to search for Weakly Interacting Massive Particles have so far shown a relative energy resolution which degrades with energy above $\sim$200 keV. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of $^{136}$Xe at its $Q$-value, $Q_{\beta\beta}\simeq$ 2.46 MeV. For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at 1 $\sigma/\mu$ is as low as (0.79$\pm$0.02) % in its one-ton fiducial mass, and for single-site interactions at $Q_{\beta\beta}$. We achieve this by using a signal correction method to rectify the saturation effects of the signal readout system. The very good energy resolution from keV to MeV energies demonstrated in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events.

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E. Aprile, J. Aalbers, F. Agostini, et. al.
Tue, 10 Mar 20
55/63

Comments: 9 pages, 7 figures

Three-Nucleon Forces: Implementation and Applications to Atomic Nuclei and Dense Matter [CL]

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http://arxiv.org/abs/2002.09548


Recent advances in nuclear structure theory have significantly enlarged the accessible part of the nuclear landscape via ab initio many-body calculations. These developments open new ways for microscopic studies of light, medium-mass and heavy nuclei as well as nuclear matter and represent an important step towards a systematic and comprehensive understanding of atomic nuclei across the nuclear chart. While remarkable agreement has been found between different many-body methods for a given nuclear Hamiltonian, the comparison with experiment and the understanding of theoretical uncertainties are still important open questions. The observed discrepancies to experiment indicate deficiencies in presently used nuclear interactions and operators. Chiral effective field theory (EFT) allows to systematically derive contributions to nucleon-nucleon (NN), three-nucleon (3N) and higher-body interactions including estimates of theoretical uncertainties. While the treatment of NN interactions in many-body calculations is well established, the calculation of 3N interactions and their incorporation in ab initio frameworks is still a frontier.
This work reviews in detail recent and current developments on the derivation and implementation of improved 3N interactions and provides a comprehensive introduction to fundamental methods for their practical calculation and representation. We further give an overview of novel and established methods that facilitate the inclusion and treatment of 3N interactions in ab initio nuclear structure frameworks and present a selection of the latest calculations of atomic nuclei as well as nuclear matter based on state-of-the-art nuclear NN and 3N interactions derived within chiral EFT. Finally, we discuss ongoing efforts, open questions and future directions.

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K. Hebeler
Wed, 26 Feb 20
11/72

Comments: 134 pages, 69 figures, 7 tables

Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars [CL]

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http://arxiv.org/abs/2002.10884


The symmetry energy obtained with the effective Skyrme energy density functional is related to the values of isoscalar effective mass and isovector effective mass, which is also indirectly related to the incompressibility of symmetric nuclear matter. In this work, we analyze the values of symmetry energy and its related nuclear matter parameters in five-dimensional parameter space by describing the heavy ion collision data, such as isospin diffusion data at 35 MeV/u and 50 MeV/u, neutron skin of $^{208}$Pb, and tidal deformability and maximum mass of neutron star. We obtain the parameter sets which can describe the isospin diffusion, neutron skin, tidal deformability and maximum mass of neutron star, and give the incompressibility $K_0$=250.23$\pm$20.16 MeV, symmetry energy coefficient $S_0$=31.35$\pm$2.08 MeV, the slope of symmetry energy $L$=59.57$\pm$10.06 MeV, isoscalar effective mass $m_s^*/m$=0.75$\pm$0.05 and quantity related to effective mass splitting $f_I$=0.005$\pm$0.170. At two times normal density, the symmetry energy we obtained is in 35-55 MeV. To reduce the large uncertainties of $f_I$, more critical works in heavy ion collisions at different beam energies are needed.

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Y. Zhang, M. Liu, C. Xia, et. al.
Wed, 26 Feb 20
12/72

Comments: 10 pages, 11 figures, 2 tables, accepted by Phys.Rev.C. arXiv admin note: text overlap with arXiv:1911.05380

Study of the $^{25}$Mg(d,p)$^{26}$Mg reaction to constrain the $^{25}$Al(p,$γ$)$^{26}$Si resonant reaction rates in nova burning conditions [CL]

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http://arxiv.org/abs/2002.03934


The rate of the $^{25}$Al($p$,$\gamma$)$^{26}$Si reaction is one of the few key remaining nuclear uncertainties required for predicting the production of the cosmic $\gamma$-ray emitter $^{26}$Al in explosive burning in novae. This reaction rate is dominated by three key resonances ($J^{\pi}=0^{+}$, $1^{+}$ and $3^{+}$) in $^{26}$Si. Only the $3^{+}$ resonance strength has been directly constrained by experiment. A high resolution measurement of the $^{25}$Mg($d$,$p$) reaction was used to determine spectroscopic factors for analog states in the mirror nucleus, $^{26}$Mg. A first spectroscopic factor value is reported for the $0^{+}$ state at 6.256 MeV, and a strict upper limit is set on the value for the $1^{+}$ state at 5.691 MeV, that is incompatible with an earlier ($^{4}$He,$^{3}$He) study. These results are used to estimate proton partial widths, and resonance strengths of analog states in $^{26}$Si contributing to the $^{25}$Al($p$,$\gamma$)$^{26}$Si reaction rate in nova burning conditions.

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C. Hamill, P. Woods, D. Kahl, et. al.
Tue, 11 Feb 20
4/81

Comments: Final version accepted and published. 6 pages and 3 figures

Solar Flare Detection Method using Rn-222 Radioactive Source [SSA]

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http://arxiv.org/abs/2002.02787


Solar neutrino detection is known to be a very challenging task, due to the minuscule absorption cross-section and mass of the neutrino. One research showed that relative large solar-flares affected the decay-rates of Mn-54 in December 2006. Since most the radiation emitted during a solar flare are blocked before reaching the earth surface, it should be assumed that such decay-rate changes could be due to neutrino flux increase from the sun, in which only neutrinos can penetrate the radionuclide. This study employs the Rn-222 radioactive source for the task of solar flare detection, based on the prediction that it will provide a stable gamma ray counting rate. In order to ascertain counting stability, three counting systems were constructed to track the count-rate changes. The signal processing approach was applied in the raw data analysis. The Rn-222 count-rate measurements showed several radiation counting dips, indicating that the radioactive nuclide can be affected by order of magnitude neutrino flux change from the sun. We conclude that using the cooled Radon source obtained the clearest responses, and therefore this is the preferable system for detecting neutrino emissions from a controlled source.

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J. Walg, Y. Zigel, A. Rodnianski, et. al.
Mon, 10 Feb 20
16/59

Comments: arXiv admin note: substantial text overlap with arXiv:1902.10131

Constraining the $^{22}$Ne($α$,$γ$)$^{26}$Mg and $^{22}$Ne($α$,n)$^{25}$Mg reaction rates using sub-Coulomb $α$-transfer reactions [CL]

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http://arxiv.org/abs/2001.08316


The $^{22}$Ne($\alpha$,$\gamma$)$^{26}$Mg and $^{22}$Ne($\alpha$,n)$^{25}$Mg reactions play an important role in astrophysics because they have significant influence on the neutron flux during the weak branch of the s-process. We constrain the astrophysical rates for these reactions by measuring partial $\alpha$-widths of resonances in $^{26}$Mg located in the Gamow window for the $^{22}$Ne+$\alpha$ capture. These resonances were populated using $^{22}$Ne($^6$Li,d)$^{26}$Mg and $^{22}$Ne($^7$Li,t)$^{26}$Mg reactions at energies near the Coulomb barrier. At these low energies $\alpha$-transfer reactions favor population of low spin states and the extracted partial $\alpha$-widths for the observed resonances exhibit only minor dependence on the model parameters. The astrophysical rates for both the $^{22}$Ne($\alpha$,$\gamma$)$^{26}$Mg and the $^{22}$Ne($\alpha$,n)$^{25}$Mg reactions are shown to be significantly lower than the previously suggested values.

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H. Jayatissa, G. Rogachev, V. Goldberg, et. al.
Fri, 24 Jan 20
8/72

Comments: 7 pages, 3 figures, 2 tables, accepted for publication in Physics Letters B

A new possibility for light-quark Dark Matter [CEA]

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http://arxiv.org/abs/2001.08654


Despite many decades of study the physical origin of “dark matter” in the Universe remains elusive. In this letter we calculate the properties of a completely new dark matter candidate – Bose-Einstein condensates formed from a recently discovered bosonic particle in the light-quark sector, the $\mathbf{ d^(2380)}$ hexaquark. In this first study, we show stable $\mathbf{ d^(2380)}$ Bose-Einstein condensates could form in the primordial early universe, with a production rate sufficiently large that they are a plausible new candidate for dark matter. Some possible astronomical signatures of such dark matter are also presented.

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M. Bashkanov and D. Watts
Fri, 24 Jan 20
15/72

Comments: N/A

Decay properties of $^{22}\mathrm{Ne} + α$ resonances and their impact on $s$-process nucleosynthesis [CL]

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http://arxiv.org/abs/2001.08206


The astrophysical $s$-process is one of the two main processes forming elements heavier than iron. A key outstanding uncertainty surrounding $s$-process nucleosynthesis is the neutron flux generated by the ${}^{22}\mathrm{Ne}(\alpha, n){}^{25}\mathrm{Mg}$ reaction during the He-core and C-shell burning phases of massive stars. This reaction, as well as the competing ${}^{22}\mathrm{Ne}(\alpha, \gamma){}^{26}\mathrm{Mg}$ reaction, is not well constrained in the important temperature regime from ${\sim} 0.2$–$0.4$~GK, owing to uncertainties in the nuclear properties of resonances lying within the Gamow window. To address these uncertainties, we have performed a new measurement of the ${}^{22}\mathrm{Ne}({}^{6}\mathrm{Li}, d){}^{26}\mathrm{Mg}$ reaction in inverse kinematics, detecting the outgoing deuterons and ${}^{25,26}\mathrm{Mg}$ recoils in coincidence. We have established a new $n / \gamma$ decay branching ratio of $1.14(26)$ for the key $E_x = 11.32$ MeV resonance in $^{26}\mathrm{Mg}$, which results in a new $(\alpha, n)$ strength for this resonance of $42(11)~\mu$eV when combined with the well-established $(\alpha, \gamma)$ strength of this resonance. We have also determined new upper limits on the $\alpha$ partial widths of neutron-unbound resonances at $E_x = 11.112,$ $11.163$, $11.169$, and $11.171$ MeV. Monte-Carlo calculations of the stellar ${}^{22}\mathrm{Ne}(\alpha, n){}^{25}\mathrm{Mg}$ and ${}^{22}\mathrm{Ne}(\alpha, \gamma){}^{26}\mathrm{Mg}$ rates, which incorporate these results, indicate that both rates are substantially lower than previously thought in the temperature range from ${\sim} 0.2$–$0.4$~GK.

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S. Ota, G. Christian, G. Lotay, et. al.
Thu, 23 Jan 20
23/36

Comments: 17 pages, 4 figures, accepted for publication in Phys. Lett. B

Measurement and analysis of nuclear $γ$-ray production cross sections in proton interactions with Mg, Si and Fe nuclei abundant in astrophysical sites over the incident energy range $E=30-66$ MeV [CL]

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http://arxiv.org/abs/2001.07087


Gamma-ray production cross section excitation functions have been measured for $30$, $42$, $54$ and $66$ MeV proton beams accelerated onto targets of astrophysical interest, $^{nat}$C, C + O (Mylar), $^{nat}$Mg, $^{nat}$Si and $^{56}$Fe, at the Sector Separated Cyclotron (SSC) of iThemba LABS (near Cape Town, South Africa). The AFRODITE array equipped with 8 Compton suppressed HPGe clover detectors was used to record $\gamma$-ray data. For known, intense $\gamma$-ray lines the previously reported experimental data measured up to $E_{p}\simeq$ $25$ MeV at the Washington and Orsay tandem accelerators were extended to higher proton energies. Our experimental data for the last 3 targets are reported here and discussed with respect to previous data and the Murphy \textit{et al.} compilation [ApJS 183, 142 (2009)], as well as to predictions of the nuclear reaction code TALYS. The overall agreement between theory and experiment obtained in first-approach calculations using default input parameters of TALYS has been appreciably improved by using modified optical model potential (OMP), deformation, and level density parameters. The OMP parameters have been extracted from theoretical fits to available experimental elastic/inelastic nucleon scattering angular distribution data by means of the coupled-channels reaction code OPTMAN. Experimental data for several new $\gamma$-ray lines are also reported and discussed. The astrophysical implications of our results are emphasised.

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W. Yahia-Cherif, S. Ouichaoui, J. Kiener, et. al.
Wed, 22 Jan 20
35/116

Comments: 22 pages, 10 figures, five tables; regular article submitted to Phys Rev C

Nuclear effects in high-energy neutrino interactions [CL]

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http://arxiv.org/abs/2001.03677


Neutrino telescopes like IceCube, KM3NeT and Baikal-GVD offer physicists the opportunity to study neutrinos with energies far beyond the reach of terrestrial accelerators. These neutrinos are used to study high-energy neutrino interactions and to probe the Earth through absorption tomography. Current studies of TeV neutrinos use cross sections which are calculated for free nucleons with targets which are assumed to contain equal numbers of protons and neutrons.
Here we consider modifications of high-energy neutrino interactions due to two nuclear effects: modifications of the parton densities in the nucleus, referred to here as shadowing, and the effect of non-isoscalar targets, with unequal numbers of neutrons and protons. Both these effects depend on the interaction medium. Because shadowing is larger for heavier nuclei, such as iron, found in the Earth’s core, it introduces a zenith-angle dependent change in the absorption cross section. These modifications increase the cross sections by 1-2\% at energies below 100 TeV (antishadowing), and reduce it by 3-4\% at higher energies (shadowing).
Nuclear effects also alter the inelasticity distribution of neutrino interactions in water/ice by increasing the number of low inelasticity interactions, with a larger effect for $\nu$ than $\bar\nu$. These effects are particularly large in the energy range below a few TeV. These effects could alter the cross sections inferred from events with tracks originating within the active detector volume as well as the ratio $\nu/\bar\nu$ inferred from inelasticity measurements.
The uncertainties in these nuclear effects are larger than the uncertainties on the free-proton cross sections and will thus limit the systematic precision of future high-precision measurements at neutrino telescopes.

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S. Klein, S. Robertson and R. Vogt
Tue, 14 Jan 20
20/72

Comments: N/A

Bayesian inference of the skewness parameter of supra-dense nuclear matter from energetic heavy-ion reactions [CL]

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http://arxiv.org/abs/2001.03669


Within the Bayesian framework using available constraining bands on the pressure in symmetric nuclear matter (SNM) derived earlier by others in the density range of 1.3$\rho_0$ to 4.5$\rho_0$ from kaon production and nuclear collective flow data in energetic heavy-ion collisions, we infer the posterior probability distribution functions (PDFs) of SNM incompressibility $K_0$ and skewness $J_0$ using uniform prior PDFs for them in the ranges of $220\leq K_0\leq 260$ MeV and $-800\leq J_0\leq 400$ MeV. The 68\% posterior credible boundaries around the most probable values of $K_0$ and $J_0$ are found to be 222$\pm$2 MeV and -215$\pm$20 MeV, respectively, much narrower than their prior ranges widely used currently in the literature and are consistent with the results of a recent Bayesian analysis of neutron star properties constrained by available X-ray and gravitational wave observations.

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W. Xie and B. Li
Tue, 14 Jan 20
49/72

Comments: 20 pages with 4 figures

Gamma-ray emission in alpha-particle reactions with C, Mg, Si, Fe [CL]

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http://arxiv.org/abs/2001.03600


Cross sections for the strongest gamma-ray emission lines produced in alpha-particle reactions with C, Mg, Si, Fe have been measured in the range E_alpha = 50 – 90 MeV at the center for proton therapy at the Helmholtz-Zentrum Berlin. Data for more than 60 different gamma-ray lines were determined, with particular efforts for lines that are in cross section compilations/evaluations with astrophysical purpose, and where data exist at lower projectile energies. The data are compared with predictions of a modern nuclear reaction code and cross-section curves of the latest evaluation for gamma-ray line emission in accelerated-particle interactions in solar flares.

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J. Kiener, J. Bundesmann, I. Deloncle, et. al.
Mon, 13 Jan 20
2/61

Comments: 5 pages, 5 figures, contribution to the XXIII International School on Nuclear Physics, Neutron Physics and Applications, Varna, Bulgaria, September 22-28, 2019

Nuclear physics uncertainties in neutrino-driven, neutron-rich supernova ejecta [CL]

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http://arxiv.org/abs/2001.02085


Neutrino-driven ejecta in core collapse supernovae (CCSNe) offer an interesting astrophysical scenario where lighter heavy elements between Sr and Ag can be synthesized. Previous studies emphasized the important role that ($\alpha,n$) reactions play in the production of these elements, particularly in neutron-rich and alpha-rich environments. In this paper, we have investigated the sensitivity of elemental abundances to specific ($\alpha,n$) reaction-rate uncertainties under different astrophysical conditions. Following a Monte Carlo nucleosynthesis study with over 36 representative astrophysical wind conditions, we have identified the most important reactions based on their impact on the final elemental abundances. Experimental studies of these reactions will reduce the nucleosynthesis uncertainties and make it possible to use observations to understand the origin of lighter heavy elements and the astrophysical conditions where they are formed.

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J. Bliss, A. Arcones, F. Montes, et. al.
Wed, 8 Jan 20
55/64

Comments: N/A

Nucleosynthesis of "Light" Heavy Nuclei in Neutrino-driven Winds. Role of ($α,n$) reactions [SSA]

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http://arxiv.org/abs/2001.00924


Neutrino-driven winds following core collapse supernovae have been proposed as a suitable site where the so-called light heavy elements (between Sr to Ag) can be synthetized. For moderately neutron-rich winds, ($\alpha,n$) reactions play a critical role in the weak r process, becoming the main mechanism to drive nuclear matter towards heavier elements. In this paper we summarize the sensitivity of network-calculated abundances to the astrophysical conditions, and to uncertainties in the ($\alpha,n$) reaction rates. A list of few ($\alpha,n$) reactions were identified to dominate the uncertainty in the calculated elemental abundances. Measurements of these reactions will allow to identify the astrophysical conditions of the weak r process by comparing calculated/observed abundances in r-limited stars.

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J. Pereira, A. Arcones, J. Bliss, et. al.
Mon, 6 Jan 20
30/49

Comments: N/A

Re-analysis of the $^{24}$Mg($α,γ$)$^{28}$Si reaction rate at stellar temperatures [CL]

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http://arxiv.org/abs/1912.11826


The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction influences the production of magnesium and silicon isotopes during carbon burning and is one of eight reaction rates found to significantly impact the shape of calculated X-ray burst light curves. The reaction rate is based on measured resonance strengths and known properties of levels in $^{28}$Si. The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction rate has been re-evaluated including recent additional indirect data. The reaction rate is substantially unchanged from previously calculated rates, especially at astrophysically important temperatures. Increases in the reaction rate could occur at lower temperatures due to as-yet unmeasured resonances but these increases have little astrophysical impact. The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction rate at temperatures relevant to carbon burning and Type I X-ray bursts is well constrained by the available experimental data. This removes one reaction from the list of eight previously found to be important for X-ray burst light curve model-observation comparisons.

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P. Adsley, A. Laird and Z. Meisel
Mon, 30 Dec 19
32/51

Comments: 5 pages, 5 figures

Re-analysis of the $^{24}$Mg($α,γ$)$^{28}$Si reaction rate at stellar temperatures [CL]

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http://arxiv.org/abs/1912.11826


The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction influences the production of magnesium and silicon isotopes during carbon burning and is one of eight reaction rates found to significantly impact the shape of calculated X-ray burst light curves. The reaction rate is based on measured resonance strengths and known properties of levels in $^{28}$Si. The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction rate has been re-evaluated including recent additional indirect data. The reaction rate is substantially unchanged from previously calculated rates, especially at astrophysically important temperatures. Increases in the reaction rate could occur at lower temperatures due to as-yet unmeasured resonances but these increases have little astrophysical impact. The $^{24}$Mg($\alpha,\gamma$)$^{28}$Si reaction rate at temperatures relevant to carbon burning and Type I X-ray bursts is well constrained by the available experimental data. This removes one reaction from the list of eight previously found to be important for X-ray burst light curve model-observation comparisons.

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P. Adsley, A. Laird and Z. Meisel
Mon, 30 Dec 19
30/51

Comments: 5 pages, 5 figures

Covariant Density Functional Theory in Nuclear Physics and Astrophysics [CL]

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http://arxiv.org/abs/1912.11112


How does subatomic matter organize itself? Neutron stars are cosmic laboratories uniquely poised to answer this fundamental question that lies at the heart of nuclear science. Newly commissioned rare isotope facilities, telescopes operating across the entire electromagnetic spectrum, and ever more sensitive gravitational wave detectors will probe the properties of neutron-rich matter with unprecedented precision over an enormous range of densities. Yet, a coordinated effort between observation, experiment, and theoretical research is of paramount importance for realizing the full potential of these investments. Theoretical nuclear physics provides valuable insights into the properties of neutron-rich matter in regimes that are not presently accessible to experiment or observation. In particular, nuclear density functional theory is likely the only tractable framework that can bridge the entire nuclear landscape by connecting finite nuclei to neutron stars. This compelling connection is the main scope of the present review.

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J. Yang and J. Piekarewicz
Wed, 25 Dec 19
15/31

Comments: 23 pages, 5 figures. When citing this paper, please use the following: Yang J, Piekarewicz J. Covariant Density Functional Theory in Nuclear Physics and Astrophysics. Annual Review of Nuclear and Particle Science Volume 70: Submitted. DOI: 10.1146/annurev-nucl-101918-023608

Covariant Density Functional Theory in Nuclear Physics and Astrophysics [CL]

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http://arxiv.org/abs/1912.11112


How does subatomic matter organize itself? Neutron stars are cosmic laboratories uniquely poised to answer this fundamental question that lies at the heart of nuclear science. Newly commissioned rare isotope facilities, telescopes operating across the entire electromagnetic spectrum, and ever more sensitive gravitational wave detectors will probe the properties of neutron-rich matter with unprecedented precision over an enormous range of densities. Yet, a coordinated effort between observation, experiment, and theoretical research is of paramount importance for realizing the full potential of these investments. Theoretical nuclear physics provides valuable insights into the properties of neutron-rich matter in regimes that are not presently accessible to experiment or observation. In particular, nuclear density functional theory is likely the only tractable framework that can bridge the entire nuclear landscape by connecting finite nuclei to neutron stars. This compelling connection is the main scope of the present review.

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J. Yang and J. Piekarewicz
Wed, 25 Dec 19
12/31

Comments: 23 pages, 5 figures. When citing this paper, please use the following: Yang J, Piekarewicz J. Covariant Density Functional Theory in Nuclear Physics and Astrophysics. Annual Review of Nuclear and Particle Science Volume 70: Submitted. DOI: 10.1146/annurev-nucl-101918-023608

Covariant Density Functional Theory in Nuclear Physics and Astrophysics [CL]

Posted on by

http://arxiv.org/abs/1912.11112


How does subatomic matter organize itself? Neutron stars are cosmic laboratories uniquely poised to answer this fundamental question that lies at the heart of nuclear science. Newly commissioned rare isotope facilities, telescopes operating across the entire electromagnetic spectrum, and ever more sensitive gravitational wave detectors will probe the properties of neutron-rich matter with unprecedented precision over an enormous range of densities. Yet, a coordinated effort between observation, experiment, and theoretical research is of paramount importance for realizing the full potential of these investments. Theoretical nuclear physics provides valuable insights into the properties of neutron-rich matter in regimes that are not presently accessible to experiment or observation. In particular, nuclear density functional theory is likely the only tractable framework that can bridge the entire nuclear landscape by connecting finite nuclei to neutron stars. This compelling connection is the main scope of the present review.

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J. Yang and J. Piekarewicz
Wed, 25 Dec 19
23/31

Comments: 23 pages, 5 figures. When citing this paper, please use the following: Yang J, Piekarewicz J. Covariant Density Functional Theory in Nuclear Physics and Astrophysics. Annual Review of Nuclear and Particle Science Volume 70: Submitted. DOI: 10.1146/annurev-nucl-101918-023608

Nuclear and neutron-star matter from local chiral interactions [CL]

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http://arxiv.org/abs/1912.09411


We report the first quantum Monte Carlo calculation of the equation of state of symmetric nuclear matter using local interactions derived from chiral effective field theory up to next-to-next-to-leading order fit to few-body observables only. The empirical saturation density and energy are well reproduced within statistical and systematic uncertainties. We have also derived the symmetry energy as a function of the density, finding good agreement with available experimentally derived constraints at saturation and twice saturation density. We find that the corresponding pressure is also in excellent agreement with recent constraints extracted from gravitational waves of the neutron-star merger GW170817 by the LIGO-Virgo detection.

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D. Lonardoni, I. Tews, S. Gandolfi, et. al.
Fri, 20 Dec 19
12/63

Comments: 7 pages, 3 figures, 3 tables

123-321 Models of Classical Novae [SSA]

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http://arxiv.org/abs/1912.08443


High-resolution spectroscopy has revealed large concentrations of CNO and sometimes other intermediate-mass elements in the shells ejected during nova outbursts, suggesting that the solar composition material transferred from the secondary mixes with the outermost layers of the underlying white dwarf during the thermonuclear runaway. Multidimensional simulations have shown that Kelvin-Helmholtz instabilities provide self-enrichment of the accreted envelope with material from the outermost layers of the white dwarf, at levels that agree with observations. However, the Eulerian and time-explicit nature of most multidimensional codes used to date and the overwhelming computational load have limited their applicability, and no multidimensional simulation has been conducted for a full nova cycle. This paper explores a new methodology that combines 1-D and 3-D simulations. The early stages of the explosion (i.e., mass-accretion and initiation of the runaway) have been computed with the 1-D hydrodynamic code SHIVA. When convection extends throughout the entire envelope, the structures for each model were mapped into 3-D Cartesian grids and were subsequently followed with the multidimensional code FLASH. Two key physical quantities were extracted from the 3-D simulations and subsequently implemented into SHIVA, which was used to complete the simulation through the late expansion and ejection stages: the time-dependent amount of mass dredged-up from the outer white dwarf layers, and the time-dependent convective velocity profile throughout the envelope. More massive envelopes than those reported from previous models with pre-enrichment have been found. This results in more violent outbursts, characterized by higher peak temperatures and greater ejected masses, with metallicity enhancements in agreement with observations.

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J. Jose, S. Shore and J. Casanova
Thu, 19 Dec 19
29/82

Comments: 8 pages, accepted for publication in Astronomy & Astrophysics

Scintillation balloon for liquid scintillator base Neutrinoless double beta decay search experiments [CL]

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http://arxiv.org/abs/1912.08067


A liquid scintillator base experiment KamLAND-Zen has set a lower limit on neutrinoless double beta decay half-life, and upgrade project KamLAND-Zen 800 has started in 2019. Unfortunately, this project expects some backgrounds, and one of the main backgrounds is beta/gamma-ray from 214Bi in container of xenon loaded liquid scintillator (mini-balloon). In order to reject the background, we suggest using scintillation film for the future mini-balloon. If we can tag alpha-ray from 214Po by scintillation detection, we can eliminate 214Bi events by delayed coincidence analysis. Recently, it was reported that polyethylene naphthalate (PEN) can be used as a scintillator with blue photon emission. PEN has chemical compatibility for strong solvent, thus it has a possibility to use in liquid scintillator. In this presentation, we will mention the results for feasibility studies about transparency and emission spectra, light yield, radioactivity, strength of film etc.. We also show the test-sized scintillation balloon with an 800-mm diameter and discussions about how to use the scintillation balloon in KamLAND.

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S. S.Obara, Y. Y.Gando and K. K.Ishidoshiro
Wed, 18 Dec 19
70/71

Comments: 3 pages, 4 figures, Proceedings of the 16th International Conference on Topics in Astroparticle and Underground Physics (TAUP 2019), September 9-13, 2019, Toyama, Japan

Generalized Lomb-Scargle analysis of $\rm{^{36}Cl}$ decay rate measurements at PTB and BNL [HEAP]

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http://arxiv.org/abs/1912.06970


Recently, Pomme et al did an analysis of $\rm{^{36}Cl} $ radioactive decay data from measurements at the Physikalisch-Technische Bundesanstalt (PTB), in order to verify the claims by Sturrock and collaborators of an influence on beta-decay rates measured at Brookehaven National Lab (BNL) due to the rotation-induced modulation of the solar neutrino flux. Their analysis excluded any sinusoidal modulations in the frequency range from 0.2-20/year. We carry out an independent analysis of the same PTB and BNL data using the generalized Lomb-Scargle periodogram, to look for any statistically significant peaks in the range from 0 to 14 per year, and by evaluating the significance of every peak using multiple methods. Our results for the PTB data are in agreement with those by Pomme et al. For BNL data, we do find peaks at some of the same frequencies as Sturrock et al, but the significance is much lower. All our analysis codes and datasets have been made publicly available.

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A. Dhaygude and S. Desai
Tue, 17 Dec 19
85/89

Comments: 6 pages, 4 figures

A Low Energy Rare Event Search with the Majorana Demonstrator [CL]

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http://arxiv.org/abs/1912.06181


The MAJORANA DEMONSTRATOR is sensitive to rare events near its energy threshold, including bosonic dark matter, solar axions, and lightly ionizing particles. In this analysis, a novel training set of low energy small-angle Compton scatter events is used to determine the efficiency of pulse shape analysis cuts, and we present updated bosonic dark matter and solar axion results from an 11.17 kg-y dataset using a 5 keV analysis threshold.

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M. Collaboration, C. Wiseman, I. Arnquist, et. al.
Mon, 16 Dec 19
8/62

Comments: 4 pages, 4 figures. Proceedings of the 16th International Conference on Topics in Astroparticle and Underground Physics (TAUP 2019), September 9-13, 2019, Toyama, Japan

Big-Bang Nucleosynthesis After Planck [CEA]

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http://arxiv.org/abs/1912.01132


We assess the status of big-bang nucleosynthesis (BBN) in light of the final Planck data release and other recent developments, and in anticipation of future measurements. Planck data fix the cosmic baryon density to 0.9% precision, and determine the helium abundance and effective number of neutrinos with precision approaching that of astronomical and BBN determinations respectively. In addition, new high-redshift measurements give D/H to better precision than theoretical predictions, and new Li/H data reconfirm the lithium problem. We present new ${}^{7}{\rm Be}(n,p){}^{7}{\rm Li}$ rates using new neutron capture measurements; we have also examined the effect of proposed changes in the $d(p,\gamma){}^{3}{\rm He}$ rates. Using these results we perform a series of likelihood analyses. We assess BBN/CMB consistency, with attention to how our results depend on the choice of Planck data, as well as how the results depend on the choice of non-BBN, non-Planck data sets. Most importantly the lithium problem remains, and indeed is more acute given the very tight D/H observational constraints; new neutron capture data reveals systematics that somewhat increases uncertainty and thus slightly reduces but does not essentially change the problem. We confirm that $d(p,\gamma){}^{3}{\rm He}$ theoretical rates brings D/H out of agreement and slightly increases 7Li; new experimental data are needed at BBN energies. Setting the lithium problem aside, we find the effective number of neutrino species at BBN is $N_\nu = 2.86 \pm 0.15$. Future CMB Stage-4 measurements promise substantial improvements in BBN parameters: helium abundance determinations will be competitive with the best astronomical determinations, and $N_{\rm eff}$ will approach sensitivities capable of detecting the effects of Standard Model neutrino heating of the primordial plasma. (Abridged)

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B. Fields, K. Olive, T. Yeh, et. al.
Wed, 4 Dec 19
34/58

Comments: 63 pages, 22 figures. Comments welcome

Search for dark matter induced de-excitation of $^{180}$Ta$\rm ^m$ [CEA]

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http://arxiv.org/abs/1911.07865


Weak-scale dark matter particles, in collisions with nuclei, can mediate transitions between different nuclear energy levels. In particular, owing to sizeable momentum exchange, dark matter particles can enable de-excitation of nuclear isomers that are extremely long lived with respect to regular radioactive decays. In this paper, we utilize data from a past experiment with $^{180}$Ta$\rm ^m$ to search for $\gamma$-lines that would accompany dark matter induced de-excitation of this isomer. Non-observation of such transitions above background yields the first direct constraint on the lifetime of $^{180}$Ta$\rm ^m$ against DM-initiated transitions: $T_{1/2}>1.3\times 10^{14}$~a at 90\% C.I. Using this result, we derive novel constraints on dark matter models with strongly interacting relics, and on models with inelastic dark matter particles. Existing constraints are strengthened by this independent new method. The obtained limits are also valid for the Standard Model $\gamma$-decay of $^{180}$Ta$\rm ^m$.

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B. Lehnert, H. Ramani, M. Hult, et. al.
Wed, 20 Nov 19
19/73

Comments: N/A

Indirect methods in nuclear astrophysics with relativistic radioactive beams [CL]

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http://arxiv.org/abs/1910.14094


Reactions with radioactive nuclear beams at relativistic energies have opened new doors to clarify the mechanisms of stellar evolution and cataclysmic events in stars and during the big bang epoch. Numerous nuclear reactions of astrophysical interest cannot be assessed directly in laboratory experiments. In this contribution, we make a short review of the limitations of experiments and of the theoretical methods needed to understand the physics of stars, adding to the knowledge inferred from astronomical observations. We continue by introducing a more detailed description of how the use of relativistic radioactive beams can help to solve astrophysical puzzles and several successful experimental methods. State-of-the-art theories are discussed at some length with the purpose of helping us understand the experimental results reported. The review is not complete and we have focused most of it to traditional methods aiming at the determination of the equation of state of symmetric and asymmetric nuclear matter and the role of the symmetry energy. Whenever possible, under the limitations of our present understanding of experimental data and theory, we try to pinpoint the information still missing to further understand how stars evolve, explode, and how their internal structure might be. We try to convey the idea that in order to improve microscopic theories for many-body calculations, nuclear structure, nuclear reactions, and astrophysics, and in order to constrain and allow for convergence of our understanding of stars, we still need considerable improvements in terms of accuracy of experiments and the development of new and dedicated nuclear facilities to study relativistic reactions with radioactive beams.

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T. Aumann and C. Bertulani
Fri, 1 Nov 19
39/54

Comments: 70 pages, 66 figures, 458 references. Comments are welcome

Highlights of EPS HEP 2019 [CL]

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http://arxiv.org/abs/1910.12768


An opinionated and informal recap of highlights from the EPS HEP 2019 conference in Ghent, including some aspects of flavour physics, neutrinos, high-density QCD, astrophysics and energy frontier collider physics, and some thoughts about the future.

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J. Butterworth
Tue, 29 Oct 19
19/78

Comments: 8 pages

Proceedings of The Magnificent CE$ν$NS Workshop 2018 [CL]

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http://arxiv.org/abs/1910.07450


The Magnificent CE$\nu$NS Workshop (2018) was held November 2 & 3 of 2018 on the University of Chicago campus and brought together theorists, phenomenologists, and experimentalists working in numerous areas but sharing a common interest in the process of coherent elastic neutrino-nucleus scattering (CE$\nu$NS). This is a collection of abstract-like summaries of the talks given at the meeting, including links to the slides presented. This document and the slides from the meeting provide an overview of the field and a snapshot of the robust CE$\nu$NS-related efforts both planned and underway.

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D. Sierra, A. Balantekin, D. Caratelli, et. al.
Thu, 17 Oct 19
21/62

Comments: The Magnificent CEvNS Workshop (2018), Nov 2-3, 2018; Chicago, IL, USA; 44 contributions

Relativistic energy-density functional approach to magnetic-dipole excitation and its sum rule [CL]

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http://arxiv.org/abs/1910.05349


Magnetic-dipole (M1) excitations of $^{18}$O and $^{42}$Ca nuclei are investigated within a relativistic nuclear energy density functional framework. In our last work \cite{2019OP}, these nuclei are found to have unique M1 excitation and its sum rule, because of their characteristic structure: the system consists of the shell-closure core plus two neutrons. For a more systematic investigation of the M1 mode, we have implemented a framework based on the relativistic nuclear energy density functional (RNEDF). For benchmark, we have performed the RNEDF calculations combined with the random-phase approximation (RPA). We evaluate the M1 excitation of $^{18}$O and $^{42}$Ca, whose sum-rule value (SRV) of the M1 transitions can be useful to test the computational implementation \cite{2019OP}. We also apply this RNEDF method to $^{208}$Pb, whose M1 property has been precisely measured \cite{1979Holt,1987Koehler,1988Laszewski,2016Birkhan}. Up to the level of the M1 sum rule, our result is in agreement with the experiments, except the discrepancy related with the quenching factors for $g$ coefficients.

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T. Oishi, G. Kruzic and N. Paar
Tue, 15 Oct 19
24/90

Comments: 6 pages, 2 figures, 1 table, contribution to the conference proceedings for INPC 2019 in Glasgow, UK (29th July – 2nd August, 2019)

$S$-factor and scattering-parameter extractions from ${}^{3}\mathrm{He} +{}^{4}\mathrm{He} \rightarrow {}^{7}\mathrm{Be} + γ$ [CL]

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http://arxiv.org/abs/1909.07287


Previous studies of the reaction ${}^{3}\mathrm{He} +{}^{4}\mathrm{He} \rightarrow {}^{7}\mathrm{Be} + \gamma$ have focused on providing the best central value and error bar for the $S$ factor at solar energies. Measurements of this capture reaction, the ${}^{3}\mathrm{He}$-${}^{4}\mathrm{He}$ scattering phase shifts, as well as properties of ${}^{7}\mathrm{Be}$, have been used to constrain employed theoretical models. Here we show that much more information than was previously appreciated can be extracted from angle-integrated capture data alone. We use the next-to-leading-order (NLO) amplitude in an effective field theory (EFT) for the reaction to perform the extrapolation. At this order the EFT describes the reaction using an s-wave scattering length and effective range, the asymptotic properties of the final bound states, and short-distance contributions to the $E1$ capture amplitude. We extract the multi-dimensional posterior of all these parameters via a Bayesian analysis. We find that properties of the ${}^{7}\mathrm{Be}$ ground and excited states are well constrained. The total $S$ factor $S(0)= 0.578^{+0.015}{-0.016}$ keV~b, while the branching ratio for excited- to ground-state capture at zero energy, $Br(0)=0.406^{+0.013}{-0.011}$, both at 68\% degree of belief. This $S(0)$ is broadly consistent with other recent evaluations, including the previously recommended value $S(0)=0.56 \pm 0.03$ eV b, but has a smaller error bar. We also find significant constraints on the scattering parameters, and we obtain constraints on the $S(E)$’s angular dependence. The path forward seems to lie with better measurements of the scattering phase shift and $S(E)$’s angular dependence, together with better understanding of the asymptotic normalization coefficients of the ${}^7$Be bound states’ wave functions. Data on these could further reduce $S(0)$’s uncertainty.

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X. Zhang, K. Nollett and D. Phillips
Tue, 17 Sep 19
28/98

Comments: 19 pages and 10 figures (including the supplemental materials)

New Results from the Cosmic-Ray Program of the NA61/SHINE facility at the CERN SPS [HEAP]

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http://arxiv.org/abs/1909.07136


The NA61/SHINE experiment at the SPS accelerator at CERN is a unique facility for the study of hadronic interactions at fixed target energies. The data collected with NA61/SHINE is relevant for a broad range of topics in cosmic-ray physics including ultrahigh-energy air showers and the production of secondary nuclei and anti-particles in the Galaxy.
Here we present an update of the measurement of the momentum spectra of anti-protons produced in $\pi^-$+C interactions at 158 and 350 GeV/c and discuss their relevance for the understanding of muons in air showers initiated by ultrahigh-energy cosmic rays.
Furthermore, we report the first results from a three-day pilot run aimed at investigating the capability of our experiment to measure nuclear fragmentation cross sections for the understanding of the propagation of cosmic rays in the Galaxy. We present a preliminary measurement of the production cross section of Boron in C+p interactions at 13.5 AGeV/c and discuss prospects for future data taking to provide the comprehensive and accurate reaction database of nuclear fragmentation needed in the era of high-precision measurements of Galactic cosmic rays.

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M. Unger and N. Collaboration
Tue, 17 Sep 19
63/98

Comments: To appear on the proceedings of the 36th International Cosmic Ray Conference (ICRC 2019)

Study of the lateral distribution functions of electron and muon bundles using Trasgo detectors [IMA]

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http://arxiv.org/abs/1909.07035


Some of the main features of the new generation Trasgo detectors are their capability in measuring the incoming direction and the arrival time of secondary cosmic particles. They also offer the identification capability between muon and electrons and a rough calorimetry for electrons. Using ground-based stations, these properties allow for the development of new tools for the measurement of primary cosmic ray fluxes. In order to verify and quantify the suitability of Trasgo detectors, whether a single one or arrays of them, to provide reliable information of the properties (mass, energy, incoming direction) of primary cosmic rays we have started an initiative for the systematic study of the ‘lateral distributions’ displayed by electrons and muons, or by bundles of those particles, using MonteCarlo simulations. In a first approach, electrons and muons were produced in vertical showers from primary H, He, C and Fe nuclei, and with incoming energies limited to a maximum of 10$^{15}$ eV per nucleon. This choice represents a significant component of all secondary particles, which can be measured on Earth’s surface. The lateral distributions study has been done at the two locations of Santiago de Compostela (Spain) and Livingston Island (Antarctica), where Trasgo detectors are either in operation, or will be operative in the near future.

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A. Álvarez-Díaz, P. Cabanelas, Y. Fontenla, et. al.
Tue, 17 Sep 19
72/98

Comments: N/A

Symmetry energy of super-dense neutron-rich matter from integrating barotropic pressures in neutron stars and heavy-ion reactions [CL]

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http://arxiv.org/abs/1909.06616


Within the minimum model of neutron stars (NS) consisting of neutrons, protons and electrons, a new approach is proposed for inferring the symmetry energy of super-dense neutron-rich nucleonic matter above twice the saturation density $\rho_0$ of nuclear matter directly from integrating iteratively barotropic pressures in both neutron stars and heavy-ion reactions. Simultaneously, the proton fraction of NSs at $\beta$ equilibrium is extracted as a function of baryon density from the same procedure. An application of this approach using the NS pressure from GW170817 and the pressure in cold symmetric nuclear matter (SNM) extracted earlier by analyzing nuclear collective flow data in relativistic heavy-ion collisions provides a useful constraining band for the symmetry energy above $2\rho_0$.

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B. Li and W. Xie
Tue, 17 Sep 19
76/98

Comments: 15 pages

Status on $\mathbf{{}^{12}{\rm C}+{}^{12}{\rm C}}$ fusion at deep subbarrier energies: impact of resonances on astrophysical $S^{*}$ factors [CL]

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http://arxiv.org/abs/1909.06021


Since the discovery of molecular resonances in $^{12}$C+$^{12}$C in the early sixties a great deal of research work has been undertaken to study $\alpha$-clustering and resonant effects of the fusion process at sub-Coulomb barrier energies. The astrophysical $S^{*}$ factors of $^{12}$C+$^{12}$C fusion have been extracted from several recent direct fusion measurements at deep subbarrier energies near the Gamov window. They were also obtained by the indirect Trojan horse method (THM). A critical comparison of recent direct measurements and the THM, which elucidates problems in the analysis of the THM, is proposed in this Letter to the Editor.

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C. Beck, A. Mukhamedzhanov and X. Tang
Mon, 16 Sep 19
32/74

Comments: 5 pages, 2 figures

First operation of the KATRIN experiment with tritium [CL]

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http://arxiv.org/abs/1909.06069


The determination of the neutrino mass is one of the major challenges in astroparticle physics today. Direct neutrino mass experiments, based solely on the kinematics of beta-decay, provide a largely model-independent probe to the neutrino mass scale. The Karlsruhe Tritium Neutrino (KATRIN) experiment is designed to directly measure the effective electron antineutrino mass with a sensitivity of 0.2 eV 90% CL. In this work we report on the first operation of KATRIN with tritium which took place in 2018. During this commissioning phase of the tritium circulation system, excellent agreement of the theoretical prediction with the recorded spectra was found and stable conditions over a time period of 13 days could be established. These results are an essential prerequisite for the subsequent neutrino mass measurements with KATRIN in 2019.

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M. Aker, K. Altenmüller, M. Arenz, et. al.
Mon, 16 Sep 19
48/74

Comments: N/A

An improved upper limit on the neutrino mass from a direct kinematic method by KATRIN [CL]

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http://arxiv.org/abs/1909.06048


We report on the neutrino mass measurement result from the first four-week science run of the Karlsruhe Tritium Neutrino experiment KATRIN in spring 2019. Beta-decay electrons from a high-purity gaseous molecular tritium source are energy analyzed by a high-resolution MAC-E filter. A fit of the integrated electron spectrum over a narrow interval around the kinematic endpoint at 18.57 keV gives an effective neutrino mass square value of $(-1.0^{+0.9}_{-1.1})$ eV$^2$. From this we derive an upper limit of 1.1 eV (90$\%$ confidence level) on the absolute mass scale of neutrinos. This value coincides with the KATRIN sensitivity. It improves upon previous mass limits from kinematic measurements by almost a factor of two and provides model-independent input to cosmological studies of structure formation.

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M. Aker, K. Altenmüller, M. Arenz, et. al.
Mon, 16 Sep 19
56/74

Comments: N/A

Impact of Uncertainties in Astrophysical Reaction Rates on Nucleosynthesis in the $νp$ Process [HEAP]

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http://arxiv.org/abs/1909.03235


The $\nu p$ process appears in proton-rich, hot matter which is expanding in a neutrino wind and may be realised in explosive environments such as core-collapse supernovae or in outflows from accretion disks. The impact of uncertainties in nuclear reaction cross sections on the finally produced abundances has been studied by applying Monte Carlo variation of all astrophysical reaction rates in a large reaction network. As the detailed astrophysical conditions of the $\nu p$ process still are unknown, a parameter study was performed, with 23 trajectories covering a large range of entropies and $Y_\mathrm{e}$. The resulting abundance uncertainties are given for each trajectory. The $\nu p$ process has been speculated to contribute to the light $p$ nuclides but it was not possible so far to reproduce the solar isotope ratios. It is found that it is possible to reproduce the solar $^{92}$Mo/$^{94}$Mo abundance ratio within nuclear uncertainties, even within a single trajectory. The solar values of the abundances in the Kr-Sr region relative to the Mo region, however, cannot be achieved within a single trajectory. They may still be obtained from a weighted superposition of different trajectories, though, depending on the actual conditions in the production site. For a stronger constraint of the required conditions, it would be necessary to reduce the uncertainties in the 3$\alpha$ and $^{56}$Ni(n,p)$^{56}$Co rates at temperatures $T>3$ GK.

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T. Rauscher, N. Nishimura, G. Cescutti, et. al.
Tue, 10 Sep 19
80/80

Comments: 6 pages, 1 figure, 2 tables; to appear in JPS Conference Proceedings (OMEG15, 2019); summarizes and expands on arXiv:1907.13129 with an additional discussion of isotopic ratios of p-nuclides

$\bf ^{12}{C} + {}^{16}{O}$ molecular resonances at deep sub-barrier energy [CL]

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http://arxiv.org/abs/1908.11638


The existence of $^{12}{\rm C} + {}^{16}{\rm O}$ molecular resonances at sub-barrier energy has been a significant problem in nuclear astrophysics because they strongly affect the $^{12}{\rm C} + {}^{16}{\rm O}$ fusion reaction rate in type Ia supernovae and heavy stars. However, experimental surveys have been limited to 4~MeV and cannot access the deep sub-barrier energy due to a very small fusion cross section. Here we predict a couple of resonances with $J^\pi=0^+$, $2^+$, and $4^+$ in the deep sub-barrier energy based on the antisymmetrized molecular dynamics calculation that reproduces the known resonances and low-lying spectrum of $^{28}{\rm Si}$.

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Y. Taniguchi and M. Kimura
Mon, 2 Sep 19
38/66

Comments: 10 pages, 4 figures

$\bf ^{12}{C} + {}^{16}{O}$ molecular resonances at deep sub-barrier energy [CL]

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http://arxiv.org/abs/1908.11638


The existence of $^{12}{\rm C} + {}^{16}{\rm O}$ molecular resonances at sub-barrier energy has been a significant problem in nuclear astrophysics because they strongly affect the $^{12}{\rm C} + {}^{16}{\rm O}$ fusion reaction rate in type Ia supernovae and heavy stars. However, experimental surveys have been limited to 4~MeV and cannot access the deep sub-barrier energy due to a very small fusion cross section. Here we predict a couple of resonances with $J^\pi=0^+$, $2^+$, and $4^+$ in the deep sub-barrier energy based on the antisymmetrized molecular dynamics calculation that reproduces the known resonances and low-lying spectrum of $^{28}{\rm Si}$.

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Y. Taniguchi and M. Kimura
Mon, 2 Sep 19
57/66

Comments: 10 pages, 4 figures

The beta-Oslo method: experimentally constrained ($n,γ$) reaction rates relevant to the $r$-process [CL]

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http://arxiv.org/abs/1908.09608


Unknown neutron-capture reaction rates remain a significant source of uncertainty in state-of-the-art $r$-process nucleosynthesis reaction network calculations. As the $r$-process involves highly neutron-rich nuclei for which direct ($n,\gamma$) cross-section measurements are virtually impossible, indirect methods are called for to constrain ($n,\gamma$) cross sections used as input for the $r$-process nuclear network. Here we discuss the newly developed beta-Oslo method, which is capable of providing experimental input for calculating ($n,\gamma$) rates of neutron-rich nuclei. The beta-Oslo method represents a first step towards constraining neutron-capture rates of importance to the $r$-process.

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A. Larsen, S. Liddick, A. Spyrou, et. al.
Tue, 27 Aug 19
69/85

Comments: 4 pages, 1 figure, conference proceedings Nuclei in the Cosmos XV 2018, Italy;

Comment on N. Rijal et al. "Measurement of d + 7Be Cross Sections for Big-Bang Nucleosynthesis" [CL]

Posted on by

http://arxiv.org/abs/1908.06451


Rijal, et al. in their recent publication [Phys. Rev. Lett {\bf 122}, 182701 (2019), arXiv:1808.07893], on “Measurement of d + $^7$Be Cross Sections for Big-Bang Nucleosynthesis (BBN)”, misrepresent their result, they misrepresent previous work of Parker (72) and of Caughlan and Fowler (88), and quite possibly, contradicts the very BBN theory that has been established over the last few decades. This comment is intended to correct these misrepresentations and critically review their claims on BBN.

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M. Gai
Tue, 20 Aug 19
62/86

Comments: N/A

Setting $\textit{ab initio}$ uncertainties on finite-temperature properties of neutron matter [CL]

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http://arxiv.org/abs/1908.04736


We present a comprehensive error band on neutron matter properties at finite temperature (finite-T) including uncertainties on the nuclear interaction, the many-body method convergence, and the thermodynamical consistency of the approach. This study provides $\textit{ab initio}$ predictions for finite-T neutron matter employing chiral interactions which are selected on the basis of their performance in both finite nuclei and infinite matter at zero temperature. Since proper theoretical uncertainties at finite-T are still generally lacking, the band provided here represents a significant step forward in setting first-principles constraints on thermal aspects of the nuclear matter equation of state.

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A. Carbone
Wed, 14 Aug 19
60/60

Comments: 6 pages, 4 figures

Constraints for stellar electron-capture rates on $^{86}$Kr via the $^{86}$Kr($t$,$^{3}$He$+γ$)$^{86}$Br reaction and the implications for core-collapse supernovae [CL]

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http://arxiv.org/abs/1908.03985


In the late stages of stellar core-collapse, prior to core bounce, electron captures on medium-heavy nuclei drive deleptonization and simulations require the use of accurate reaction rates. Nuclei with neutron number near $N=50$, just above atomic number $Z=28$, play an important role, but rates used in astrophysical simulations rely primarily on a relatively simple single-state approximation. In order to improve the accuracy of astrophysical simulations, experimental data are needed to test the electron-capture rates and to guide the development of better theoretical models. This work presents the results of the $^{86}$Kr($t$,$^{3}$He+$\gamma$) experiment at the NSCL, from which an upper limit for the Gamow-Teller strength up to an excitation energy in $^{86}$Br of 5 MeV is extracted. The derived upper limit for the electron-capture rate on $^{86}$Kr indicates that the rate estimated through the single-state approximation is too high and that rates based on Gamow-Teller strengths estimated in shell-model and QRPA calculations are more accurate. The QRPA calculations tested in this manner were used for estimating the electron capture rates for 78 isotopes near $N=50$ and above $Z=28$. The impact of using these new electron-capture rates in simulations of supernovae instead of the rates based on the single-state approximation is investigated, indicating a significant reduction in the deleptonization that affects multi-messenger signals, such as the emission of neutrinos and gravitational waves.

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R. Titus, E. Ney, R. Zegers, et. al.
Tue, 13 Aug 19
30/69

Comments: 15 pages, 10 figures

Uncertainties in $ν$p-process nucleosynthesis from Monte Carlo variation of reaction rates [SSA]

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http://arxiv.org/abs/1907.13129


It has been suggested that a $\nu$p process can occur when hot, dense, and proton-rich matter is expanding within a strong flux of anti-neutrinos. In such an environment, proton-rich nuclides can be produced in sequences of proton captures and (n,p) reactions, where the free neutrons are created in situ by $\overline{\nu}_\mathrm{e}+\mathrm{p} \rightarrow \mathrm{n}+\mathrm{e}^+$ reactions. The detailed hydrodynamic evolution determines where the nucleosynthesis path turns off from N = Z line and how far up the nuclear chart it runs. In this work, the uncertainties on the final isotopic abundances stemming from uncertainties in the nuclear reaction rates were investigated in a large-scale Monte Carlo approach, simultaneously varying ten thousand reactions. A large range of model conditions was investigated because a definitive astrophysical site for the $\nu$p process has not yet been identified. The present parameter study provides, for each model, identification of the key nuclear reactions dominating the uncertainty for a given nuclide abundance. As all rates appearing in the $\nu$p process involve unstable nuclei, and thus only theoretical rates are available, the final abundance uncertainties are larger than those for nucleosynthesis processes closer to stability. Nevertheless, most uncertainties remain below a factor of three in trajectories with robust nucleosynthesis. More extreme conditions allow production of heavier nuclides but show larger uncertainties because of the accumulation of the uncertainties in many rates and because the termination of nucleosynthesis is not at equilibrium conditions. It is also found that the solar ratio of the abundances of ${}^{92}$Mo and ${}^{94}$Mo could be reproduced within uncertainties.

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N. Nishimura, T. Rauscher, R. Hirschi, et. al.
Thu, 1 Aug 19
45/66

Comments: 19 pages, 12 figures, 8 tables, accepted for publication in MNRAS

Ruling out the supersoft high-density symmetry energy from the discovery of PSR J0740+6620 with mass $2.17^{+0.11}_{-0.10}M_\odot$ [CL]

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http://arxiv.org/abs/1907.12284


Using the very recently reported mass $2.17^{+0.11}{-0.10}M\odot$ of PSR J0740+6620 together with the data of finite nuclei and the constraints on the equation of state of symmetric nuclear matter at suprasaturation densities from flow data in heavy-ion collisions, we show that the symmetry energy $E_{\rm sym}(n)$ cannot be supersoft so that it becomes negative at suprasaturation densities in neutron stars (NSs) and thus may make the NS have a pure neutron matter core. This is in contrast to the fact that using mass $2.01 \pm 0.04 M_\odot$ of PSR J0348+0432 cannot rule out the supersoft high-density $E_{\rm sym}(n)$. Furthermore, we find the stiffer high-density $E_{\rm sym}(n)$ based on the existence of $2.17M_\odot$ NSs leads to a strong constraint of $\Lambda_{1.4} \ge 362^{+89}{-58}$ for the dimensionless tidal deformability of the canonical $1.4M\odot$ NS.

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Y. Zhou and L. Chen
Tue, 30 Jul 19
58/79

Comments: 6 pages, 2 figures, 1 table

Single-particle shell strengths near the doubly magic nucleus $^{56}$Ni and the $^{56}$Ni(p,$γ$)$^{57}$Cu reaction rate in explosive astrophysical burning [CL]

Posted on by

http://arxiv.org/abs/1907.11665


Angle-integrated cross-section measurements of the $^{56}$Ni(d,n) and (d,p) stripping reactions have been performed to determine the single-particle strengths of low-lying excited states in the mirror nuclei pair $^{57}$Cu-$^{57}$Ni situated adjacent to the doubly magic nucleus $^{56}$Ni. The reactions were studied in inverse kinematics utilizing a beam of radioactive $^{56}$Ni ions in conjunction with the GRETINA $\gamma$-array. Spectroscopic factors are compared with new shell-model calculations using a full $pf$ model space with the GPFX1A Hamiltonian for the isospin-conserving strong interaction plus Coulomb and charge-dependent Hamiltonians. These results were used to set new constraints on the $^{56}$Ni(p,$\gamma$)$^{57}$Cu reaction rate for explosive burning conditions in x-ray bursts, where $^{56}$Ni represents a key waiting point in the astrophysical rp-process.

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D. Kahl, P. Woods, T. Poxon-Pearson, et. al.
Mon, 29 Jul 19
33/52

Comments: Final version accepted and published. 5 pages, 2 figures

Bayesian Inference of High-density Nuclear Symmetry Energy from Radii of Canonical Neutron Stars [HEAP]

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http://arxiv.org/abs/1907.10741


The radius $R_{1.4}$ of canonical neutron stars (NSs) has been extracted consistently with about 6-13\% $1\sigma$ statistical and 10\% systematic errors in many recent studies of the tidal deformability of NSs involved in GW170817 and X-rays from quiescent low-mass X-ray binaries. Using representative $R_{1.4}$ data in the literature, we infer the high-density nuclear symmetry energy $E_{\rm{sym}}(\rho)$ and the associated nucleon specific energy $E_0(\rho)$ in symmetric nuclear matter (SNM) within a Bayesian statistical approach using an explicitly isospin-dependent parametric Equation of State (EOS). We find that: (1) The available astrophysical data can already improve significantly our knowledge about the $E_0(\rho)$ and $E_{\rm{sym}}(\rho)$ in the density range of $\rho_0-2.5\rho_0$ compared to what we currently know. In particular, the symmetry energy at twice the saturation density $\rho_0$ of nuclear matter is determined to be $E_{\mathrm{sym}}(2\rho_0)$ =39.2${-8.2}^{+12.1}$ MeV at 68\% confidence level approximately independent of the EOS parameterizations used. (2) A precise measurement of $R{1.4}$ alone with a 4\% 1$\sigma$ statistical error but no systematic error will not improve much the constraints on the EOS of dense neutron-rich nucleonic matter compared to those extracted already from using the available radius data. (3) The high-density behavior of $E_{\rm{sym}}(\rho)$ inferred depends strongly on how the high-density $E_0(\rho)$ is parameterized, and vice versa. (4) The value of the observed maximum NS mass and whether it is used as a sharp cut-off for the minimum maximum mass or through a Gaussian distribution in the Bayesian analyses affect significantly the lower boundaries of $E_0(\rho)$ and $E_{\rm{sym}}(\rho)$ only at densities higher than about $2.5\rho_0$.

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W. Xie and B. Li
Fri, 26 Jul 19
56/84

Comments: 24 pages

Impact of Uncertainties in Nuclear Reaction Cross Sections on p-Nucleosynthesis in Thermonuclear Supernovae [HEAP]

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http://arxiv.org/abs/1907.09178


The propagation of uncertainties in reaction cross sections and rates of neutron-, proton-, and alpha-induced reactions into the final isotopic abundances obtained in nucleosynthesis models is an important issue in studies of nucleosynthesis and Galactic Chemical Evolution. We developed a Monte Carlo method to allow large-scale postprocessing studies of the impact of nuclear uncertainties on nucleosynthesis. Temperature-dependent rate uncertainties combining realistic experimental and theoretical uncertainties are used. From detailed statistical analyses uncertainties in the final abundances are derived as probability density distributions. Furthermore, based on rate and abundance correlations an automated procedure identifies the most important reactions in complex flow patterns from superposition of many zones or tracers. The method so far was already applied to a number of nucleosynthesis processes. Here we focus on the production of p-nuclei in white dwarfs exploding as thermonuclear (type Ia) supernovae. We find generally small uncertainties in the final abundances despite of the dominance of theoretical nuclear uncertainties. A separate analysis of low- and high-density regions indicates that the total uncertainties are dominated by the high-density regions.

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T. Rauscher, N. Nishimura, G. Cescutti, et. al.
Tue, 23 Jul 19
8/72

Comments: 6 pages, 3 figures; invited talk at 13th Int. Conf. on Nucleus-Nucleus Collisions, Saitama, Japan, 2018. To be published in JPS Conf. Proceedinngs; summarizes results from arXiv:1807.11475

Resonance strengths in the 14N(p,gamma)15O astrophysical key reaction measured with activation [CL]

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http://arxiv.org/abs/1907.07446


The 14N(p,gamma)15O reaction plays a vital role in various astrophysical scenarios. Its reaction rate must be accurately known in the present era of high precision astrophysics. The cross section of the reaction is often measured relative to a low energy resonance, the strength of which must therefore be determined precisely. The activation method, based on the measurement of 15O decay, has not been used in modern measurements of the 14N(p,gamma)15O reaction. The aim of the present work is to provide strength data for two resonances in the 14N(p,gamma)15O reaction using the activation method. The obtained values are largely independent from previous data measured by in-beam gamma-spectroscopy and are free from some of their systematic uncertainties. Solid state TiN targets were irradiated with a proton beam provided by the Tandetron accelerator of Atomki using a cyclic activation. The decay of the produced 15O isotopes was measured by detecting the 511 keV positron annihilation gamma-rays. The strength of the Ep = 278 keV resonance was measured to be 13.4 +- 0.8 meV while for the Ep = 1058 keV resonance the strength is 442 +- 27 meV. The obtained Ep = 278 keV resonance strength is in fair agreement with the values recommended by two recent works. On the other hand, the Ep = 1058 keV resonance strength is about 20% higher than the previous value. The discrepancy may be caused in part by a previously neglected finite target thickness correction. As only the low energy resonance is used as a normalization point for cross section measurements, the calculated astrophysical reaction rate of the 14N(p,gamma)15O reaction and therefore the astrophysical consequences are not changed by the present results.

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G. Gyürky, Z. Halász, G. Kiss, et. al.
Thu, 18 Jul 19
57/64

Comments: Accepted for publication in Phys. Rev. C

Neutron rich matter in heaven and on Earth [CL]

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http://arxiv.org/abs/1907.02561


Despite a length-scale difference of 18 orders of magnitude, the internal structure of neutron stars and the spatial distribution of neutrons in atomic nuclei are profoundly connected.

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J. Piekarewicz and F. Fattoyev
Mon, 8 Jul 19
23/43

Comments: Manuscript published in final form in Physics Today, July 2019, page 30

Metastable Nuclear Isomers as Dark Matter Accelerators [CL]

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http://arxiv.org/abs/1907.00011


Inelastic dark matter and strongly interacting dark matter are poorly constrained by direct detection experiments since they both require the scattering event to deliver energy from the nucleus into the dark matter in order to have observable effects. We propose to test these scenarios by searching for the collisional de-excitation of meta-stable nuclear isomers by the dark matter particles. The longevity of these isomers is related to a strong suppression of $\gamma$- and $\beta$-transitions, typically inhibited by a large difference in the angular momentum for the nuclear transition. The collisional de-excitation by dark matter is possible since heavy dark matter particles can have a momentum exchange with the nucleus comparable to the inverse nuclear size, hence lifting tremendous angular momentum suppression of the nuclear transition. This de-excitation can be observed either by searching for the direct effects of the decaying isomer, or through the re-scattering or decay of excited dark matter states in a nearby conventional dark matter detector setup. Existing nuclear isomer sources such as naturally occurring $^{180m}$Ta, $^{137m}$Ba produced in decaying Cesium in nuclear waste, $^{177m}$Lu from medical waste, and $^{178m}$Hf from the Department of Energy storage can be combined with current dark matter detector technology to search for this class of dark matter.

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M. Pospelov, S. Rajendran and H. Ramani
Tue, 2 Jul 19
20/79

Comments: 13 pages, 6 figures

Experimental Constraint on Stellar Electron-Capture Rates from the ${}^{88}\text{Sr}(t,{}^{3}\text{He}+γ){}^{88}\text{Rb}$ reaction at 115 MeV/u [CL]

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http://arxiv.org/abs/1906.05934


The Gamow-Teller strength distribution from ${}^{88}$Sr was extracted from a $(t,{}^{3}\text{He}+\gamma)$ experiment at 115 MeV/$u$ to constrain estimates for the electron-capture rates on nuclei around $N=50$, between and including $^{78}$Ni and $^{88}$Sr, which are important for the late evolution of core-collapse supernovae. The observed strength below an excitation energy of 8 MeV was consistent with zero and below 10 MeV amounted to $0.1\pm0.05$. Except for a very-weak transition that could come from the 2.231-MeV $1^{+}$ state, no $\gamma$ lines that could be associated with the decay of known $1^{+}$ states were identified. The derived electron-capture rate from the measured strength distribution is more than an order of magnitude smaller than rates based on the single-state approximation presently used in astrophysical simulations for most nuclei near $N=50$. Rates based on shell-model and quasiparticle random-phase approximation calculations that account for Pauli blocking and core-polarization effects provide better estimates than the single-state approximation, although a relatively strong transition to the first $1^{+}$ state in $^{88}$Rb is not observed in the data. Pauli unblocking effects due to high stellar temperatures could partially counter the low electron-capture rates. The new data serves as a zero-temperature benchmark for constraining models used to estimate such effects.

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J. Zamora, R. Zegers, S. Austin, et. al.
Mon, 17 Jun 19
15/53

Comments: N/A

Calculation of resonance energies from Q-values [CL]

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http://arxiv.org/abs/1906.06282


Resonance energies are frequently derived from precisely measured excitation energies and reaction Q-values. The latter quantities are usually calculated from atomic instead of nuclear mass differences. This procedure disregards the energy shift caused by the difference in the total electron binding energies before and after the interaction. Assuming that the interacting nuclei in a stellar plasma are fully ionized, this energy shift can have a significant effect, considering that the resonance energy enters exponentially into the expression for the narrow-resonance thermonuclear reaction rates. As an example, the rate of the $^{36}$Ar(p,$\gamma$)$^{37}$K reaction is discussed, which, at temperatures below 1 GK, depends only on the contributions of a single resonance and direct capture. In this case, disregarding the energy shift caused by the total electron binding energy difference erroneously enhances the rate by $\approx$40\% near temperatures of 70 MK.

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C. Iliadis
Mon, 17 Jun 19
21/53

Comments: 3 pages, 2 figures

Constraining the Neutron Star Compactness: Extraction of the $^{23}$Al($p,γ$) Reaction Rate for the $rp$-Process [CL]

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http://arxiv.org/abs/1906.06091


The $^{23}$Al($p,\gamma$)$^{24}$Si reaction is among the most important reactions driving the energy generation in Type-I X-ray bursts. However, the present reaction-rate uncertainty limits constraints on neutron star properties that can be achieved with burst model-observation comparisons. Here, we present a novel technique for constraining this important reaction by combining the GRETINA array with the neutron detector LENDA coupled to the S800 spectrograph at the National Superconducting Cyclotron Laboratory. The $^{23}$Al($d,n$) reaction was used to populate the astrophysically important states in $^{24}$Si. This enables a measurement in complete kinematics for extracting all relevant inputs necessary to calculate the reaction rate. For the first time, a predicted close-lying doublet of a 2$_2^+$ and (4$_1^+$,0$_2^+$) state in $^{24}$Si was disentangled, finally resolving conflicting results from two previous measurements. Moreover, it was possible to extract spectroscopic factors using GRETINA and LENDA simultaneously. This new technique may be used to constrain other important reaction rates for various astrophysical scenarios.

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C. Wolf, C. Langer, F. Montes, et. al.
Mon, 17 Jun 19
48/53

Comments: N/A

Probing high-energy interactions of atmospheric and astrophysical neutrinos [HEAP]

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http://arxiv.org/abs/1906.02221


Astrophysical and atmospheric neutrinos are important probes of the powerful accelerators that produce cosmic-rays with EeV energies. Understanding these accelerators is a key goal of neutrino observatories, along with searches for neutrinos from supernovae, from dark matter annihilation, and other astrophysics topics. Here, we discuss how neutrino observatories like IceCube and future facilities like KM3NeT and IceCube-Gen2 can study the properties of high-energy (above 1 TeV) neutrino interactions. This is far higher than is accessible at man-made accelerators, where the highest energy neutrino beam reached only 500 GeV. In contrast, neutrino observatories have observed events with energies above 5 PeV – 10,000 times higher in energy – and future large observatories may probe neutrinos with energies up to $10^{20}$ eV. These data have implications for both Standard Model measurements, such as of low Bjorken$-x$ parton distributions and gluon shadowing, and also for searches for beyond Standard Model physics. This chapter will review the existing techniques and results, and discuss future prospects.

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S. Klein
Fri, 7 Jun 19
5/49

Comments: Prepared for the forthcoming book “Particle Physics with Neutrino Telescopes”, C. P\’erez de los Heros, editor, (World Scientific)

The early life of millisecond magnetars [HEAP]

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http://arxiv.org/abs/1906.02610


Some neutron stars may be born spinning fast and with strong magnetic fields—the so-called \emph{millisecond magnetars}. It is important to understand how a star’s magnetic axis moves with respect to the spin axis in the star’s early life, as this effects both electromagnetic and gravitational wave emission. Previous studies have highlighted the importance of viscous dissipation within the star in this process. We advance this program by additionally considering the effect of the electromagnetic torque. We find an interesting interplay between the viscous dissipation, which makes the magnetic axis orthogonalise with respect to the spin, verses magnetic torques that tend to make the magnetic axis align with the spin axis. We present some results, and highlight areas where our model needs to be made more realistic.

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D. Jones
Fri, 7 Jun 19
29/49

Comments: To appear in the AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7 2019, Xiamen, China

Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy [CL]

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http://arxiv.org/abs/1905.13175


Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry \esym is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.

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B. Li, P. Krastev, D. Wen, et. al.
Fri, 31 May 19
31/58

Comments: 77 pages. Invited Review Article, EPJA (2019) in press

C$ν$B detection through angular correlations in inverse $β$-decay [CL]

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http://arxiv.org/abs/1905.10207


Neutrino capture on beta-decaying nuclei is currently the only known potentially viable method of detection of cosmic background neutrinos. It is based on the idea of separation of the spectra of electrons or positrons produced in captures of relic neutrinos on unstable nuclei from those from the usual $\beta$-decay and requires very high energy resolution of the detector, comparable to the neutrino mass. In this paper we suggest an alternative method of discrimination between neutrino capture and $\beta$-decay, based on periodic variations of angular correlations in inverse beta decay transitions induced by relic neutrino capture. The time variations are expected to arise due to the peculiar motion of the Sun with respect to the C$\nu$B rest frame and the rotation of the Earth about its axis and can be observed in experiments with both polarized and unpolarized nuclear targets. The main advantage of the suggested method is that it does not depend crucially on the energy resolution of detection of the produced $\beta$-particles and can be operative even if this resolution exceeds the largest neutrino mass.

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E. Akhmedov
Mon, 27 May 19
32/51

Comments: 27 pages, 1 figure

Discovery of exceptionally strong nuclear transition sheds new light on the fate of intermediate-mass stars [SSA]

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http://arxiv.org/abs/1905.09407


A significant fraction of stars between 7-11 solar masses are thought to become supernovae, but the explosion mechanism is unclear. The answer depends critically on the rate of electron capture on $^{20}$Ne in the degenerate oxygen-neon stellar core. However, due to the unknown strength of the transition between the ground states of $^{20}$Ne and $^{20}$F, it has not previously been possible to fully constrain the rate. By measuring the transition, we have established that its strength is exceptionally large and enhances the capture rate by several orders of magnitude. This has a decisive impact on the evolution of the core, increasing the likelihood that the star is (partially) disrupted by a thermonuclear explosion rather than collapsing to form a neutron star. Importantly, our measurement resolves the last remaining nuclear physics uncertainty in the final evolution of degenerate oxygen-neon stellar cores, allowing future studies to address the critical role of convection, which at present is poorly understood.

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O. Kirsebom, S. Jones, D. Strömberg, et. al.
Fri, 24 May 19
55/60

Comments: 6 pages, 5 figures, supplemental material

A study of $^{35}$Cl excited states via $^{32}$S($α, p$) [CL]

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http://arxiv.org/abs/1905.08774


Presolar grains originating in oxygen-neon novae may be identified by their sulfur isotopic ratios compared with theoretical estimates. These ratios depend on reliable $^{33}$S($p, \gamma$)$^{34}$Cl and $^{34}$S($p, \gamma$)$^{35}$Cl reaction rates. The latter rate has recently been computed based on experimental input, and many new excited states in $^{35}$Cl were discovered above the proton threshold. The experimental $^{34}$S($p, \gamma$)$^{35}$Cl rate was found to be 2 – 5 times smaller than the theoretical one, and the simulated $^{34}$S/$^{32}$S isotopic ratio for nova presolar grains was thus predicted to be smaller than that of type II supernova grains by up to a factor of 3.7. The present study was performed to confirm the existence of these new resonances, and to improve the remaining uncertainties in the $^{34}$S($p, \gamma$)$^{35}$Cl reaction rate. Energies and spin-parities of the $^{35}$Cl excited levels were investigated with an Enge split-pole spectrograph using the $^{32}$S($\alpha, p$)$^{35}$Cl reaction. Differential cross sections of the outgoing protons were measured at $E_{\alpha}$ = 21 MeV. The existence of the newly discovered states are largely confirmed, although a few states were not observed in this study. The spins and parities of several $^{35}$Cl states were assigned tentatively for the first time. The present $^{34}$S($p, \gamma$)$^{35}$Cl experimental thermonuclear reaction rate is consistent within 1$\sigma$ with the previous evaluation. However, our rate uncertainty is larger due to a more realistic treatment of the experimental uncertainties. The uncertainty in the present rate is up to a factor of 3.5 at nova temperatures. We recommend future work to focus on the unknown properties of four excited states of $^{35}$Cl at 6643 keV, 6761 keV, 6780 keV, and 6800 keV.

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K. Setoodehnia, J. Kelley, C. Marshall, et. al.
Wed, 22 May 19
47/59

Comments: 17 pages, 9 figures, accepted to Phys. Rev. C

Investigation of neutron-induced reaction at the Goethe University Frankfurt [CL]

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http://arxiv.org/abs/1905.05584


We present first results and plans for future neutron activation measurements at the Goethe University Frankfurt. The measurements were performed at the Van-de-Graaff accelerator employing the 7Li(p,n) reaction.

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R. Reifarth, L. Bott, B. Brückner, et. al.
Wed, 15 May 19
55/57

Comments: 5 pages, 5 figures, accepted as proceeding of the Nuclei in the Cosmos XV conference 2018

An efficient method for mapping the 12C+12C molecular resonances at low energies [CL]

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http://arxiv.org/abs/1905.02054


The 12C+12C fusion reaction is famous for its complication of molecular resonances, and plays an important role in both nuclear structure and astrophysics. It is extremely difficult to measure the cross sections of 12C+12C fusions at energies of astrophysical relevance due to very low reaction yields. To measure the complicated resonant structure existing in this important reaction, an efficient thick target method has been developed and applied for the first time at energies Ec.m.<5.3 MeV. A scan of the cross sections over a relatively wide range of energies can be carried out using only a single beam energy. The result of measurement at Ec.m.= 4.1 MeV is compared with other results from previous work. This method would be useful for searching potentially existing resonances of 12C+12C in the energy range 1 MeV<Ec.m.<3 MeV.

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X. Tang, S. Ma, X. Fang, et. al.
Tue, 7 May 19
26/76

Comments: unpublished, submitted to Nuclear Science and Techniques

Implications of the mass $M=2.17^{+0.11}_{-0.10}$M$_\odot$ of PSR~J0740+6620 on the Equation of State of Super-Dense Neutron-Rich Nuclear Matter [CL]

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http://arxiv.org/abs/1904.10998


We study implications of the very recently reported mass $M=2.17^{+0.11}{-0.10}$M$\odot$ of PSR~J0740+6620 on the Equation of State (EOS) of super-dense neutron-rich nuclear matter with respect to existing constraints on the EOS based on the mass $M=2.01\pm 0.04$M$\odot$ of PSR~J0348+0432, the maximum tidal deformability of GW170817 and earlier results of various terrestrial nuclear laboratory experiments. The lower limit of the skewness $J_0$ measuring the stiffness of super-dense isospin-symmetric nuclear matter is raised raised from about -220 MeV to -150 MeV, reducing significantly its current uncertainty range. The lower bound of the high-density symmetry energy also increases appreciably leading to a rise of the minimum proton fraction in neutron stars at $\beta$-equilibrium from about 0 to 5\% around three times the saturation density of nuclear matter. The difficulties for some of the most widely used and previously well tested model EOSs to predict simultaneously both a maximum mass higher than 2.17 M$\odot$ and a pressure consistent with that extracted from GW170817 present some interesting new challenges for nuclear theories.

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N. Zhang and B. Li
Fri, 26 Apr 19
36/69

Comments: 7 pages including 4 figures

Novel Techniques for Constraining Neutron-Capture Rates Relevant for r-Process Heavy-Element Nucleosynthesis [CL]

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http://arxiv.org/abs/1904.09962


The rapid-neutron capture process ($r$ process) is identified as the producer of about 50\% of elements heavier than iron. This process requires an astrophysical environment with an extremely high neutron flux over a short amount of time ($\sim$ seconds), creating very neutron-rich nuclei that are subsequently transformed to stable nuclei via $\beta^-$ decay. One key ingredient to large-scale $r$-process reaction networks is radiative neutron-capture ($n,\gamma$) rates, for which there exist virtually no data for extremely neutron-rich nuclei involved in the $r$ process. Due to the current status of nuclear-reaction theory and our poor understanding of basic nuclear properties such as level densities and average $\gamma$-decay strengths, theoretically estimated ($n,\gamma$) rates may vary by orders of magnitude and represent a major source of uncertainty in any nuclear-reaction network calculation of $r$-process abundances. In this review, we discuss new approaches to provide information on neutron-capture cross sections and reaction rates relevant to the $r$ process. In particular, we focus on indirect, experimental techniques to measure radiative neutron-capture rates. While direct measurements are not available at present, but could possibly be realized in the future, the indirect approaches present a first step towards constraining neutron-capture rates of importance to the $r$ process.

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A. Larsen, A. Spyrou, S. Liddick, et. al.
Tue, 23 Apr 19
6/58

Comments: 62 pages, 24 figures, accepted for publication in Progress in Particle and Nuclear Physics

Interface effects of strange quark matter [CL]

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http://arxiv.org/abs/1904.08347


The interface effects play important roles for the properties of strange quark matter (SQM) and the related physical processes. We show several examples on the implications of interface effects for both stable and unstable SQM. Based on an equivparticle model and adopting mean-field approximation (MFA), the surface tension and curvature term of SQM can be obtained, which are increasing monotonically with the density of SQM at zero external pressure. For a parameter set constrained according to the 2$M_\odot$ strange star, we find the surface tension is $\sim$2.4 MeV/fm${}^2$, while it is larger for other cases.

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C. Xia
Thu, 18 Apr 19
52/75

Comments: To appear in the AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China

A search for solar axion induced signals with COSINE-100 [CL]

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http://arxiv.org/abs/1904.06860


We present results from a search for solar axions with the COSINE-100 detector. We find no evidence of solar axion events from a data set of 6,303.9 kg$\cdot$days exposure and set a 90\,\% confidence level upper limit on the axion-electron coupling, $g_{ae}$, at 1.70~$\times$~$10^{-11}$ for an axion mass less than 1\,keV/c$^2$. This limit excludes QCD axions heavier than 0.59\,eV/c$^2$ in the DFSZ model and 168.1\,eV/c$^2$ in the KSVZ model.

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P. Adhikari, G. Adhikari, E. Souza, et. al.
Tue, 16 Apr 19
36/88

Comments: 6 pages, 5 figures

Beta-delayed-neutron studies of $^{135,136}$Sb and $^{140}$I performed with trapped ions [CL]

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http://arxiv.org/abs/1904.06623


Beta-delayed-neutron ($\beta$n) spectroscopy was performed using the Beta-decay Paul Trap and an array of radiation detectors. The $\beta$n branching ratios and energy spectra for $^{135,136}$Sb and $^{140}$I were obtained by measuring the time of flight of recoil ions emerging from the trapped ion cloud. These nuclei are located at the edge of an isotopic region identified as having $\beta$n branching ratios that impact the r-process abundance pattern around the A~130 peak. For $^{135,136}$Sb and $^{140}$I, $\beta$n branching ratios of 14.6(11)%, 17.6(28)%, and 7.6(28)% were determined, respectively. The $\beta$n energy spectra obtained for $^{135}$Sb and $^{140}$I are compared with results from direct neutron measurements, and the $\beta$n energy spectrum for $^{136}$Sb has been measured for the first time.

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B. Alan, S. Caldwell, N. Scielzo, et. al.
Tue, 16 Apr 19
41/88

Comments: N/A

A New Approach to Determine Radiative Capture Reaction Rates at Astrophysical Energies [CL]

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http://arxiv.org/abs/1904.05819


Radiative capture reactions play a crucial role in stellar nucleosynthesis but have proved challenging to determine experimentally. In particular, the large uncertainty ($\sim$100%) in the measured rate of the $^{12}$C$(\alpha,\gamma)^{16}$O reaction is the largest source of uncertainty in any stellar evolution model. With development of new high current energy-recovery linear accelerators (ERLs) and high density gas targets, measurement of the $^{16}$O$(e,e^\prime \alpha)^{12}$C reaction close to threshold using detailed balance opens up a new approach to determine the $^{12}$C$(\alpha,\gamma)^{16}$O reaction rate with significantly increased precision ($<$20%). We present the formalism to relate photo- and electro-disintegration reactions and consider the design of an optimal experiment to deliver increased precision. Once the new ERLs come online, an experiment to validate the new approach we propose should be carried out. This new approach has broad applicability to radiative capture reactions in astrophysics.

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I. Friščić, T. Donnelly and R. Milner
Fri, 12 Apr 19
48/62

Comments: 37 pages, 27 figures

Delineating the properties of matter in cold, dense QCD [HEAP]

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http://arxiv.org/abs/1904.05080


The properties of dense QCD matter are delineated through the construction of equations of state which should be consistent with QCD calculations in the low and high density limits, nuclear laboratory experiments, and the neutron star observations. These constraints, together with the causality condition of the sound velocity, are used to develop the picture of hadron-quark continuity in which hadronic matter continuously transforms into quark matter (modulo small 1st order phase transitions). For hadronic matter (at baryon density nB > ~2n0 with n0 ~ 0.16 fm^(-3) being the nuclear saturation density) we use equations of state by Togashi et al. based on microscopic variational many-body calculations, and for quark matter (nB > ~5n0) we construct equations of state using a schematic quark model (with strangeness) whose interactions are motivated by the hadron phenomenology. The region between hadronic and quark matters (~2n0 < nB < ~5n0), which is most difficult to calculate, is treated by highly constrained interpolation between nuclear and quark matter equations of state. The resultant unified equation of state at zero temperature and beta-equilibrium, which we call Quark-Hadron-Crossover (QHC18 and QHC19), is consistent with the measured properties of neutron stars and in addition gives us microscopic insights into the properties of dense QCD matter. In particular to ~10n0 the gluons can remain as non-perturbative as in vacuum and the strangeness can be as abundant as up- and down-quarks at the core of two-solar mass neutron stars. Within our modeling the maximum mass is found less than ~2.35 times solar mass and the baryon density at the core ranges in ~5-8n0.

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T. Kojo
Thu, 11 Apr 19
1/54

Comments: 18 pages 11 figures, AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China

Studying newborn neutron stars by the transient emission after stellar collapses and compact binary mergers [HEAP]

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http://arxiv.org/abs/1904.04440


The formation of neutron stars (NSs), both from collapses of massive stars and mergers of compact objects, can be usually indicated by bright transients emitted from explosively-ejected material. In particular, if the newborn NSs can rotate at a millisecond period and have a sufficiently high magnetic field, then the spin-down of the NSs would provide a remarkable amount of energy to the emitting material. As a result, super-luminous supernovae could be produced in the massive stellar collapse cases, while some unusual fast evolving and luminous optical transients could arise from the cases of NS mergers and accretion-induced collapses of white dwarfs. In all cases, if the dipolar magnetic fields of the newborn NSs can be amplified to be as high as $10^{15}$ G, a relativistic jet could be launched and then a gamma-ray burst can be produced as the jet successfully breaks out from the surrounding nearly-isotropic ejected material.

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Y. Yu, A. Chen, Z. Dai, et. al.
Wed, 10 Apr 19
37/54

Comments: 10 pages, 9 pictures, to appear in the AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China

Equation-of-state Constraints and the QCD Phase Transition in the Era of Gravitational-Wave Astronomy [HEAP]

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http://arxiv.org/abs/1904.01306


We describe a multi-messenger interpretation of GW170817, which yields a robust lower limit on NS radii. This excludes NSs with radii smaller than about 10.7 km and thus rules out very soft nuclear matter. We stress the potential of this type of constraints when future detections become available. A very similar argumentation may yield an upper bound on the maximum mass of nonrotating NSs. We also discuss simulations of NS mergers, which undergo a first-order phase transition to quark matter. We point out a different dynamical behavior. Considering the gravitational-wave signal, we identify an unambiguous signature of the QCD phase transition in NS mergers. The occurrence of quark matter through a strong first-order phase transition during merging leads to a characteristic shift of the dominant postmerger frequency. The frequency shift is indicative for a phase transition if it is compared to the postmerger frequency which is expected for purely hadronic EoS models. A very strong deviation of several 100 Hz is observed for hybrid EoSs in an otherwise tight relation between the tidal deformability and the postmerger frequency. We address the potential impact of a first-order phase transition on the electromagnetic counterpart of NS mergers. Our simulations suggest that there would be no significant qualitative differences between a system undergoing a phase transition to quark matter and purely hadronic mergers. The quantitative differences are within the spread which is found between different hadronic EoS models. This implies on the one hand that GW170817 is compatible with a possible transition to quark matter. On the other hand these considerations show that it may not be easy to identify quantitative differences between purely hadronic mergers and events in which quark matter occurs considering solely their electromagnetic counterpart or their nucleosynthesis products. (abridged)

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A. Bauswein, N. Bastian, D. Blaschke, et. al.
Wed, 3 Apr 19
43/68

Comments: 15 pages, 11 figures, submitted to the AIP Conference Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy (January 3 – 7, 2019, Xiamen, China)

High Density with Elliptic Flows [CL]

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http://arxiv.org/abs/1903.12543


The elliptic flow of emitted particles and fragments observed in heavy-ion reactions at high energy has become an important observable reflecting the pressure generated in the dense collision zone. More recently, the strength of the nuclear symmetry energy has been investigated by measuring the ratios or differences of the elliptic flows exhibited by neutrons and charged particles in 197Au+197Au collisions at 400 MeV/nucleon incident energy at the GSI laboratory. A moderately soft to linear dependence on density was deduced for a range of densities shown to reach beyond twice the saturation value in these experiments. The known sources of uncertainties and possible model dependencies were thoroughly studied with transport models of the UrQMD and Tuebingen QMD type. A new source of information on the nuclear equation of state at high density has opened up with the observation of the first LIGO and Virgo GW170817 gravitational wave signal from a neutron star merger. The quantitative comparison of terrestrial and celestial results on the basis of measured or inferred neutron star radii or core pressures, including those obtained from X-ray observations, reveals a rather satisfactory agreement. Depending on the precision that can be achieved with future measurements and observations, it will thus become possible to assess the validity of the applied models and methods. The perspectives for improved experiments at FAIR using the NeuLAND and KRAB detection systems are outlined.

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W. Trautmann
Mon, 1 Apr 19
20/56

Comments: 15 pages, 10 figures, to appear in the AIP Conference Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy (January 3 – 7, 2019, Xiamen, China)

Near-Earth Supernova Explosions: Evidence, Implications, and Opportunities [SSA]

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http://arxiv.org/abs/1903.04589


There is now solid experimental evidence of at least one supernova explosion within 100 pc of Earth within the last few million years, from measurements of the short-lived isotope 60Fe in widespread deep-ocean samples, as well as in the lunar regolith and cosmic rays. This is the first established example of a specific dated astrophysical event outside the Solar System having a measurable impact on the Earth, offering new probes of stellar evolution, nuclear astrophysics, the astrophysics of the solar neighborhood, cosmic-ray sources and acceleration, multi-messenger astronomy, and astrobiology. Interdisciplinary connections reach broadly to include heliophysics, geology, and evolutionary biology. Objectives for the future include pinning down the nature and location of the established near-Earth supernova explosions, seeking evidence for others, and searching for other short-lived isotopes such as 26Al and 244Pu. The unique information provided by geological and lunar detections of radioactive 60Fe to assess nearby supernova explosions make now a compelling time for the astronomy community to advocate for supporting multi-disciplinary, cross-cutting research programs.

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B. Fields, J. Ellis, W. Binns, et. al.
Wed, 13 Mar 19
93/125

Comments: 11 pages, 2 figures. Astro2020 Science White Paper submitted to the 2020 Decadal Survey on Astronomy and Astrophysics

The activation method for cross section measurements in nuclear astrophysics [CL]

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http://arxiv.org/abs/1903.03339


The primary aim of experimental nuclear astrophysics is to determine the rates of nuclear reactions taking place in stars in various astrophysical conditions. These reaction rates are important ingredient for understanding the elemental abundance distribution in our solar system and the galaxy. The reaction rates are determined from the cross sections which need to be measured at energies as close to the astrophysically relevant ones as possible. In many cases the final nucleus of an astrophysically important reaction is radioactive which allows the cross section to be determined based on the off-line measurement of the number of produced isotopes. In general, this technique is referred to as the activation method, which often has substantial advantages over in-beam particle- or gamma-detection measurements. In this paper the activation method is reviewed from the viewpoint of nuclear astrophysics. Important aspects of the activation method are given through several reaction studies for charged particle, neutron and gamma-induced reactions. Various techniques for the measurement of the produced activity are detailed. As a special case of activation, the technique of Accelerator Mass Spectrometry in cross section measurements is also reviewed.

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G. Gyürky, Z. Fülöp, F. Käppeler, et. al.
Mon, 11 Mar 19
72/78

Comments: Review paper accepted for publication in European Physical Journal A

Note on neutron star equation of state in the light of GW170817 [CL]

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http://arxiv.org/abs/1903.01280


From the very first multimessenger event of GW170817, clean robust constraints can be obtained for the tidal deformabilities of the two stars involved in the merger, which provides us unique opportunity to study the equation of states (EOSs) of dense stellar matter. In this contribution, we employ a model from the quark level, describing consistently a nucleon and many-body nucleonic system from a quark potential. We check that our sets of EOSs are consistent with available experimental and observational constraints at both sub-nuclear saturation densities and higher densities. The agreements with ab-initio calculations are also good. Especially, we tune the density dependence of the symmetry energy (characterized by its slope at nuclear saturation $L$) and study its influence on the tidal deformability. The so-called $QMF18$ EOS is named after the case of $L=40~\rm MeV$, and it gives $M_{\rm TOV} =2.08~M_\odot$ and $R= 11.77~\rm km$, $\Lambda=331$ for a $1.4\,M_\odot$ star. The tidal signals are demonstrated to be insensitive to the uncertain crust-core matching, despite the good correlation between the symmetry energy slope and the radius of the star.

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A. Li and Z. Zhu
Tue, 5 Mar 19
3/73

Comments: 8 pages, 6 figures, Submitted to the AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China

Neutron Skin in CsI and Low-Energy Effective Weak Mixing Angle from COHERENT Data [CL]

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http://arxiv.org/abs/1902.07625


Both the neutron skin thickness $\Delta R_{np}$ of atomic nuclei and the low-energy neutrino-nucleon ($\nu N$) interactions are of fundamental importance in nuclear and particle physics, astrophysics as well as new physics beyond the standard model (SM) but largely uncertain currently, and the coherent elastic neutrino-nucleus scattering (CE$\nu$NS) provides a clean way to extract their information. The new physics beyond the SM may cause effectively a shift of the SM weak mixing angle $\theta_W$ in low-energy $\nu N$ interactions, leading to an effective weak mixing angle $\theta^W$. By analyzing the CE$\nu$NS data of the COHERENT experiment, we find that while a one-parameter fit to the COHERENT data produces an unrealistically large central value of $\Delta R^{\rm{CsI}}{np} \simeq 0.7$ fm for CsI when the low-energy $\sin^2 \theta^W$ is fixed at the low-energy SM value of $\sin^2\theta_W^{\rm{SM}} = 0.23857(5)$, a two-dimensional fit gives significantly smaller central values of $\Delta R^{\rm{CsI}}{np} \simeq 0.25$ fm and $\sin^2 \theta^_W \simeq 0.21$, although their uncertainties are large. The implication of the substantial deviation of the low-energy effective $\sin^2 \theta^_W$ from $\sin^2\theta_W^{\rm{SM}}$ on the new physics scenarios in neutrino physics is discussed.

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X. Huang and L. Chen
Thu, 21 Feb 19
9/54

Comments: 5 pages, 2 figures

States of the $^{12}$C Nucleus in the Toroidal Configuration [CL]

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http://arxiv.org/abs/1902.06595


The $^{12}$C nucleus with $N$=6 and $Z$=6 is a doubly-magic closed-shell nucleus in a toroidal potential and Wheeler’s triangular resonating group model of $^{12}$C as three clusters of alpha particles will naturally generate a toroidal density if the nucleons interchanging between the clusters are allowed to circulate continuously from one cluster to another. Experimentally, many excited states of $^{12}$C decay predominantly into three alpha particles, and the triangular clusters of three alpha particles have a high degree of overlap with a torus. We explore a toroidal description for some excited states of $^{12}$C and search for the signature that will reveal a possible toroidal configuration of the nucleus. We find that the $^{12}$C nucleus in a toroidal configuration distinguishes itself by toroidal multiplets of particle-hole excitations between one toroidal shell to another. Subject to further confirmation, the Hoyle state and many of its higher excited states may be tentatively attributed to those of a $^{12}$C nucleus in a toroidal configuration.

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C. Wong and A. Staszczak
Thu, 21 Feb 19
13/54

Comments: 20 pages, 6 figures

Experimental nuclear astrophysics in Italy [CL]

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http://arxiv.org/abs/1902.05262


Nuclear astrophysics, the union of nuclear physics and astronomy, went through an impressive expansion during the last twenty years. This could be achieved thanks to milestone improvements in astronomical observations, cross section measurements, powerful computer simulations and much refined stellar models. Italian groups are giving quite important contributions to every domain of nuclear astrophysics, sometimes being the leaders of worldwide unique experiments. In this paper we will discuss the astrophysical scenarios where nuclear astrophysics plays a key role and we will provide detailed descriptions of the present and future of the experiments on nuclear astrophysics which belong to the scientific programme of INFN (the National Institute for Nuclear Physics in Italy).

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C. Broggini, O. Straniero, M. Taiuti, et. al.
Fri, 15 Feb 19
8/48

Comments: To be published in La Rivista del Nuovo Cimento. arXiv admin note: text overlap with arXiv:1502.01559 by other authors

Transparent tiles of silica aerogels for high-energy physics [CL]

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http://arxiv.org/abs/1902.05374


Silica aerogels are important to be used as photon radiators in Cherenkov counters for high-energy-physics experiments because of their optical transparency and intermediate refractive indices between those of gases and liquids or solids. Cherenkov counters that employ silica aerogels as radiators and photodetectors are often used to identify subatomic charged particles (e.g., electrons, protons, and pions) with momenta on the order of sub-GeV/$c$ to GeV/$c$; they are also used to measure particle velocities in accelerator-based particle- and nuclear-physics experiments and in space- and balloon-borne experiments in the field of cosmic-ray physics. Recent studies have demonstrated that it is important for the design of Cherenkov counters that the transparent silica-aerogel tiles comprise solid material with recently improved transparency and a refractive index that can be controlled between 1.003 and 1.26 by varying the bulk density in the range of 0.01$-$1.0 g/cm$^3$. Additionally, a technique for fabricating large-area silica-aerogel tiles without cracking has been developed. In this chapter, we describe advances in the technologies for producing silica aerogels with high optical performances to be used in scientific instruments. We further discuss the principles underlying the operation of detectors based on the Cherenkov effect. We also review applications of silica aerogels in specific high-energy-physics experiments.

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M. Tabata
Fri, 15 Feb 19
11/48

Comments: Contributed chapter submitted to Springer Handbook of Aerogels (2nd ed.)

Neutron-mirror neutron oscillations in stars [SSA]

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http://arxiv.org/abs/1902.03685


Based on a newly proposed model of neutron-mirror neutron ($n-n’$) oscillations, evolution and nucleosynthesis in single stars under a new theory is presented. The new theory with the new $n-n’$ model can demonstrate the evolution in a much more convincing way than the conventional belief. In particular, many observations in stars show strong support for the new theory and the new $n-n’$ model. For example, progenitor mass limits and structures for white dwarfs and neutron stars, two different types of core collapse supernovae (Type II-P and Type II-L), pulsating phenomena in stars, etc, can all be easily and naturally explained under the new theory.

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W. Tan
Tue, 12 Feb 19
10/83

Comments: N/A

Degeneracy in Studying the Supranuclear Equation of State and Modified Gravity with Neutron Stars [CL]

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http://arxiv.org/abs/1901.07546


It is generally acknowledged that an extrapolation in physics from a well-known scale to an unknown scale is perilous. This prevents us from using laboratory experience to gain precise information for the supranuclear matter inside neutron stars (NSs). With operating and upcoming astronomical facilities, NSs’ equation of state (EOS) is expected to be determined at a new level in the near future, under the assumption that general relativity (GR) is the correct theory for gravitation. While GR is a reasonable working assumption yet still an extrapolation, there could be a large uncertainty due to the not-so-well-tested strong gravitational field inside NSs. Here we review some recent theoretical efforts towards a better understanding of the degeneracy between the supranuclear EOS and alternative gravity theories.

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L. Shao
Tue, 5 Feb 19
26/86

Comments: 11 pages, 6 figures

Nuclear collective dynamics in lattice Hamiltonian Vlasov method [CL]

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http://arxiv.org/abs/1902.01256


The lattice Hamiltonian method is developed for solving the Vlasov equation with nuclear mean-field that is based on the Skyrme pseudopotential up to next-to-next-to-next-to leading order. The ground states of nuclei are obtained through varying the total energy with respect to the density distribution of nucleons. Owing to the self-consistent treatment of initial nuclear ground state and the exact energy conservation in the lattice Hamiltonian method, the present framework of solving the Vlasov equation exhibits very stable nuclear ground state evolution. As a first application of the new lattice Hamiltonian Vlasov method, we explore the iso-scalar giant monopole and iso-vector giant dipole modes of finite nuclei. The obtained results are shown to be comparable to that from random-phase approximation and consistent with the experimental data, indicating the capability of the present method in dealing with the long-time near-equilibrium nuclear dynamics.

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R. Wang, L. Chen and Z. Zhang
Tue, 5 Feb 19
37/86

Comments: 15 pages, 7 figures

$s$-wave scattering lengths for the $^7$Be+$p$ system from an $\textit{R}$-matrix analysis [CL]

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http://arxiv.org/abs/1902.00417


The astrophysical $S$-factor for the radiative proton capture reaction on $^7$Be ($S_{17}$) at low energies is affected by the $s$-wave scattering lengths. We report the measurement of elastic and inelastic scattering cross sections for the $^7$Be+$p$ system in the center of mass energy range of 0.474 – 2.740 MeV and center of mass angular range of 70$^\circ$- 150$^\circ$. A radioactive $^7$Be beam produced at Oak Ridge National Laboratory’s (ORNL) Holifield Radioactive Ion Beam Facility (HRIBF) was accelerated and bombarded a thin polypropylene (CH${2}$)$\text n$ target. Scattered ions were detected in the segmented Silicon Detector Array (SIDAR). Using an $\textit{R}$-matrix analysis of ORNL and Louvain-la-Neuve cross section data, the $s$-wave scattering lengths for channel spin 1 and 2 were determined to be 17.34$^{+1.11}{-1.33}$ fm and -3.18$^{+0.55}{-0.50}$ fm, respectively. The uncertainty in the $s$-wave scattering lengths reported in this work is smaller by a factor of 5-8 compared to the previous measurement, which may reduce the overall uncertainty in $S_{17}$ at zero energy. The level structure of $^8$B is discussed based upon the results from this work. Evidence for the existence of 0$^+$ and 2$^+$ levels in $^8$B at 1.9 and 2.21 MeV, respectively, is observed.

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S. Paneru, C. Brune, R. Giri, et. al.
Mon, 4 Feb 19
26/60

Comments: N/A

The Equation of State of Dense Matter in the Multimessenger Era [CL]

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http://arxiv.org/abs/1901.11364


While the equation of state (EOS) of symmetric nuclear matter (SNM) at suprasaturation densities has been relatively well constrained from heavy-ion collisions, the EOS of high-density neutron-rich matter is still largely uncertain due to the poorly known high-density behavior of the symmetry energy. Using the constraints on the EOS of SNM at suprasaturation densities from heavy-ion collisions together with the data of finite nuclei and the existence of $2M_\odot$ neutron stars from electromagnetic (EM) observations, we show that the high-density symmetry energy cannot be too soft, which leads to lower bounds on dimensionless tidal deformability of $\Lambda_{1.4} \ge 193$ and radius of $R_{1.4} \ge 11.1$ km for $1.4M_\odot$ neutron star. Furthermore, we find that the recent constraint of $\Lambda_{1.4} \le 580$ from the gravitational wave signal GW170817 detected from the binary neutron star merger by the LIGO and Virgo Collaborations rules out too stiff high-density symmetry energy, leading to an upper limit of $R_{1.4} \le 13.3$ km. All these terrestrial nuclear experiments and astrophysical observations based on strong, EM and gravitational measurements together put stringent constraints on the high-density symmetry energy and the EOS of SNM, pure neutron matter and neutron star matter.

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Y. Zhou, L. Chen and Z. Zhang
Fri, 1 Feb 19
18/61

Comments: 6 pages, 4 figures

Developing a silica aerogel radiator for the HELIX ring-imaging Cherenkov system [CL]

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http://arxiv.org/abs/1901.06663


This paper reports the successful fabrication of silica aerogel Cherenkov radiators produced in the first batches from a 96-tile mass production performed using pin-drying technique in our laboratory. The aerogels are to be used in a ring-imaging Cherenkov detector in the spectrometer of a planned balloon-borne cosmic-ray observation program, HELIX (High Energy Light Isotope eXperiment). A total of 36 transparent, hydrophobic aerogel tiles with a high refractive index of 1.16 and dimensions of 10 cm $\times $ 10 cm $\times $ 1 cm will be chosen as the flight radiators. Thus far, 40 out of the 48 tiles fabricated were confirmed as having no tile cracking. In the first screening, 8 out of the first 16 tiles were accepted as flight-qualified candidates, based on basic optical measurement results. To fit the aerogel tiles into a radiator support structure, the trimming of previously manufactured prototype tiles using a water-jet cutting device was successful.

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M. Tabata, P. Allison, J. Beatty, et. al.
Wed, 23 Jan 19
87/111

Comments: Submitted to Nucl. Instrum. Methods Phys. Res. A (NIMA Proc. Special Issue: RICH 2018), 5 pages, 6 figures

GW170817 implications on the frequency and damping time of f-mode oscillations of neutron stars [CL]

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http://arxiv.org/abs/1901.03779


Within a minimum model for neutron stars consisting of nucleons, electrons and muons at $\beta$-equilibrium using about a dozen Equation of States (EOSs) from microscopic nuclear many-body theories and 40,000 EOSs randomly generated using an explicitly isospin-dependent parametric EOS model for high-density neutron-rich nucleonic matter within its currently known uncertainty range, we study correlations among the f-mode frequency, its damping time and the tidal deformability as well as the compactness of neutron stars. Except for quark stars, both the f-mode frequency and damping time of canonical neutron stars are found to scale with the tidal deformability independent of the EOSs used. Applying the constraint on the tidal deformability of canonical neutron stars $\Lambda_{1.4}=190^{+390}_{-120}$ extracted by the LIGO+VIRGO Collaborations from their improved analyses of the GW170817 event, the f-mode frequency and its damping time of canonical neutron stars are limited to 1.67 kHz – 2.18 kHz and 0.155 s – 0.255 s, respectively, providing a useful guidance for the ongoing search for gravitational waves from the f-mode oscillations of isolated neutron stars. Moreover, assuming either or both the f-mode frequency and its damping time will be measured precisely in future observations with advanced gravitational wave detectors, we discuss how information about the mass and/or radius as well as the still rather elusive nuclear symmetry energies at supra-saturation densities may be extracted.

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D. Wen, B. Li, H. Chen, et. al.
Wed, 16 Jan 19
55/76

Comments: 10 pages including 8 figures

Thermonuclear fusion rates for tritium + deuterium using Bayesian methods [CL]

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http://arxiv.org/abs/1901.04857


The $^3$H(d,n)$^4$He reaction has a large low-energy cross section and will likely be utilized in future commercial fusion reactors. This reaction also takes place during big bang nucleosynthesis. Studies of both scenarios require accurate and precise fusion rates. To this end, we implement a one-level, two-channel R-matrix approximation into a Bayesian model. Our main goals are to predict reliable astrophysical S-factors and to estimate R-matrix parameters using the Bayesian approach. All relevant parameters are sampled in our study, including the channel radii, boundary condition parameters, and data set normalization factors. In addition, we take uncertainties in both measured bombarding energies and S-factors rigorously into account. Thermonuclear rates and reactivities of the $^3$H(d,n)$^4$He reaction are derived by numerically integrating the Bayesian S-factor samples. The present reaction rate uncertainties at temperatures between $1.0$ MK and $1.0$ GK are in the range of 0.2% to 0.6%. Our reaction rates differ from previous results by 2.9% near 1.0 GK. Our reactivities are smaller than previous results, with a maximum deviation of 2.9% near a thermal energy of $4$ keV. The present rate or reactivity uncertainties are more reliable compared to previous studies that did not include the channel radii, boundary condition parameters, and data set normalization factors in the fitting. Finally, we investigate previous claims of electron screening effects in the published $^3$H(d,n)$^4$He data. No such effects are evident and only an upper limit for the electron screening potential can be obtained.

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R. Souza, S. Boston, A. Coc, et. al.
Wed, 16 Jan 19
65/76

Comments: Phys. Rev. C, 2019, in press

GW170817 implications on the frequency and damping time of f-mode oscillations of neutron stars [CL]

Posted on by

http://arxiv.org/abs/1901.03779


Within a minimum model for neutron stars consisting of nucleons, electrons and muons at $\beta$-equilibrium using about a dozen Equation of States (EOSs) from microscopic nuclear many-body theories and 40,000 EOSs randomly generated using an explicitly isospin-dependent parametric EOS model for high-density neutron-rich nucleonic matter within its currently known uncertainty range, we study correlations among the f-mode frequency, its damping time and the tidal deformability as well as the compactness of neutron stars. Except for quark stars, both the f-mode frequency and damping time of canonical neutron stars are found to scale with the tidal deformability independent of the EOSs used. Applying the constraint on the tidal deformability of canonical neutron stars $\Lambda_{1.4}=190^{+390}_{-120}$ extracted by the LIGO+VIRGO Collaborations from their improved analyses of the GW170817 event, the f-mode frequency and its damping time of canonical neutron stars are limited to 1.67 kHz – 2.18 kHz and 0.155 s – 0.255 s, respectively, providing a useful guidance for the ongoing search for gravitational waves from the f-mode oscillations of isolated neutron stars. Moreover, assuming either or both the f-mode frequency and its damping time will be measured precisely in future observations with advanced gravitational wave detectors, we discuss how information about the mass and/or radius as well as the still rather elusive nuclear symmetry energies at supra-saturation densities may be extracted.

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D. Wen, B. Li, H. Chen, et. al.
Tue, 15 Jan 19
57/83

Comments: 10 pages including 8 figures

What laboratory experiments can teach us about cosmology: A chameleon example [CEA]

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http://arxiv.org/abs/1901.01784


Laboratory experiments can shed light on theories of new physics introduced in order to explain cosmological mysteries, including the nature of dark energy and dark matter. In this article I will focus on one particular example of this, the chameleon model. The chameleon is an example of a theory which could modify gravity on cosmological distance scales, but its non-linear behavior means that it can also be tested with suitably designed laboratory experiments. The aim of this overview is to present recent theoretical developments to the experimental community.

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C. Burrage
Tue, 8 Jan 19
21/99

Comments: 5 pages, 2 figures. To appear in the Proceedings of the International Workshop on Particle Physics at Neutron Sources PPNS 2018, Grenoble, France, May 24-26, 2018

Making the Heaviest Elements in the Universe: A Review of the Rapid Neutron Capture Process [HEAP]

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http://arxiv.org/abs/1901.01410


The production of about half the heavy elements beyond Fe and Ni is assigned the rapid neutron capture process (r process). The full understanding faces two open questions. (a) The nucleosynthesis path runs close to the neutron-drip line, where presently only limited experimental information is available, and one has to rely on theoretical predictions. (b) While for many years the occurrence of the r process has been associated with supernovae recent studies have cast substantial doubts on this environment. Possibly only a weak r process, not producing the third r-process peak, can be accounted for, while much more neutron-rich conditions are likely responsible for the majority of the heavy r-process elements. Possible scenarios are the mergers of neutron stars (recently observed, GW170817) but include also rare classes of supernovae/hypernovae with polar jet ejecta (and possibly also accretion disk outflows in case of black hole formation) related to the collapse of fast rotating massive stars with high magnetic fields. The composition of the ejecta from each event determines the temporal evolution of the r-process abundances during the “chemical” evolution of the Galaxy. Stellar r-process abundance observations, have provided insights into, and constraints on the frequency of and conditions in the responsible stellar production sites. These observations, increasingly more precise due to improved experimental atomic data and high resolution observations, have been particularly important in defining the heavy element abundance patterns of the old halo stars, and the nature of the earliest nucleosynthesis in our Galaxy. Combining new results and important breakthroughs in the related nuclear, atomic and astronomical fields of science, this review attempts to provide an answer to the question “How Were the Elements from Iron to Uranium Made?” (Abridged)

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J. Cowan, C. Sneden, J. Lawler, et. al.
Tue, 8 Jan 19
99/99

Comments: 85 pages, 45 figures, 2 tables, submitted to Reviews of Modern Physics

Simulations of radiation damage in spacecraft camera for ESA JUICE mission [CL]

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http://arxiv.org/abs/1901.00205


The JUpiter ICy moons Explorer (JUICE) is an ESA interplanetary spacecraft being developed to perform detailed investigations of the Jupiter system and three of its icy moons: Europa, Callisto and Ganymede. The emphasis will be given on Ganymede as a small planetary body to be studied as a potential habitat. The spacecraft is set for launch in 2022 and would reach Jupiter in 2030. Two identical optical cameras are proposed for the mission to monitor the spacecraft and its surroundings. The sensors of the cameras need to be protected from hazardous radiation levels caused by extremely high fluxes of very energetic electrons. A precise model of the camera was developed to be used for intense Monte Carlo simulations performed to optimize the shielding and to determine the radiation damage during the mission. Simulations included determination of the total ionizing and non-ionizing doses in the sensors and crucial electronic components. This paper presents both simulation methods and results.

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H. Xiao, W. Hajdas, S. Beauvivre, et. al.
Thu, 3 Jan 19
41/48

Comments: RADECS Workshop 2018 Proceedings

Median statistics estimate of the neutron lifetime [CL]

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http://arxiv.org/abs/1812.09671


We construct the error distributions for the neutron lifetime using a subset of measurements compiled in the 2018 edition of Particle Data Group (PDG), as well as a few recent measurements, which are not yet included in PDG. We then checked the Gaussianity of the error distribution (using the techniques pioneered by Ratra and collaborators). We find that the error distributions using the weighted mean as well as median estimate are not consistent with a Gaussian distribution. We find that the Student’s $t$ and Cauchy distribution provide a better fit to the residuals. We then argue that median statistics based estimate should be used for the central estimate of the neutron lifetime. This median statistic estimate of the neutron lifetime from these measurements is given by $881.5 \pm 0.47$ seconds. We also note that the discrepancy between beam and bottle-based measurements using median statistics based estimates of the neutron lifetime persists to between 4-8$\sigma$, depending on which combination of measurements are used.

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A. Rajan and S. Desai
Thu, 27 Dec 18
9/80

Comments: 5 pages

Impact of the neutron star crust on the tidal polarizability [CL]

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http://arxiv.org/abs/1812.09974


The first detection of a binary neutron star merger has opened the brand new era of multimessenger astronomy. This historic detection has been instrumental in providing constraints on the tidal polarizability of neutron stars. In turn, the tidal polarizability has been used to impose limits on stellar radii and ultimately on the equation of state (EOS). The tidal polarizability is also sensitive to the second tidal Love number k2. It is the main purpose of this work to perform a detailed study of k2 which, for a given compactness parameter, encodes the entire sensitivity of the tidal polarizability to the EOS. In particular, we examine the role that the crustal component of the EOS plays in the determination of k2. A set of realistic models of the equation of state that yield an accurate description of the properties of finite nuclei and support neutron stars of two solar masses is used. Given that the tidal polarizability scales as the fifth power of the compactness parameter, a universal relation exists among the tidal polarizability and the compactness parameter that is highly insensitive to the underlying EOS. Thus, besides an extraction of the tidal polarizabilities, a measurement of the individual stellar masses is also required to impact the mass-radius relation. However, we observe a strong sensitivity of k2 to the EOS, particularly to the contribution from the inner crust. Although by itself the tidal polarizability can not contribute to the determination of the mass-radius relation, future detections of binary neutron star mergers are poised to provide significant constraints on both the tidal polarizabilities and masses of the individual stars, and thus ultimately on the mass-radius relation. Yet, subleading corrections to the tidal polarizability are encoded in the second Love number k2 which displays a large sensitivity to the entire (crust-plus-core) EOS.

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J. Piekarewicz and F. Fattoyev
Thu, 27 Dec 18
57/80

Comments: 15 pages and 5 figures; submitted to Physical Review C

Impact of the neutron star crust on the tidal polarizability [CL]

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http://arxiv.org/abs/1812.09974


The first detection of a binary neutron star merger has opened the brand new era of multimessenger astronomy. This historic detection has been instrumental in providing constraints on the tidal polarizability of neutron stars. In turn, the tidal polarizability has been used to impose limits on stellar radii and ultimately on the equation of state (EOS). The tidal polarizability is also sensitive to the second tidal Love number k2. It is the main purpose of this work to perform a detailed study of k2 which, for a given compactness parameter, encodes the entire sensitivity of the tidal polarizability to the EOS. In particular, we examine the role that the crustal component of the EOS plays in the determination of k2. A set of realistic models of the equation of state that yield an accurate description of the properties of finite nuclei and support neutron stars of two solar masses is used. Given that the tidal polarizability scales as the fifth power of the compactness parameter, a universal relation exists among the tidal polarizability and the compactness parameter that is highly insensitive to the underlying EOS. Thus, besides an extraction of the tidal polarizabilities, a measurement of the individual stellar masses is also required to impact the mass-radius relation. However, we observe a strong sensitivity of k2 to the EOS, particularly to the contribution from the inner crust. Although by itself the tidal polarizability can not contribute to the determination of the mass-radius relation, future detections of binary neutron star mergers are poised to provide significant constraints on both the tidal polarizabilities and masses of the individual stars, and thus ultimately on the mass-radius relation. Yet, subleading corrections to the tidal polarizability are encoded in the second Love number k2 which displays a large sensitivity to the entire (crust-plus-core) EOS.

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J. Piekarewicz and F. Fattoyev
Thu, 27 Dec 18
23/80

Comments: 15 pages and 5 figures; submitted to Physical Review C

Median statistics estimate of the neutron lifetime [CL]

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http://arxiv.org/abs/1812.09671


We construct the error distributions for the neutron lifetime using a subset of measurements compiled in the 2018 edition of Particle Data Group (PDG), as well as a few recent measurements, which are not yet included in PDG. We then checked the Gaussianity of the error distribution (using the techniques pioneered by Ratra and collaborators). We find that the error distributions using the weighted mean as well as median estimate are not consistent with a Gaussian distribution. We find that the Student’s $t$ and Cauchy distribution provide a better fit to the residuals. We then argue that median statistics based estimate should be used for the central estimate of the neutron lifetime. This median statistic estimate of the neutron lifetime from these measurements is given by $881.5 \pm 0.47$ seconds. We also note that the discrepancy between beam and bottle-based measurements using median statistics based estimates of the neutron lifetime persists to between 4-8$\sigma$, depending on which combination of measurements are used.

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A. Rajan and S. Desai
Thu, 27 Dec 18
63/80

Comments: 5 pages

Nuclear Astrophysics in the Multimessenger Era: A Partnership Made in Heaven [CL]

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http://arxiv.org/abs/1812.04438


On August 17, 2017 the LIGO-Virgo collaboration detected for the first time gravitational waves from the binary merger of two neutron stars (GW170817). Unlike the merger of two black holes, the associated electromagnetic radiation was also detected by a host of telescopes operating over a wide range of frequencies—opening a brand new era of multimessenger astronomy. This historical detection is providing fundamental new insights into the astrophysical site for the r-process and on the nature of dense matter. In this contribution we examine the impact of GW170817 on the equation of state of neutron rich matter, particularly on the density dependence of the symmetry energy. Limits on the tidal polarizability extracted from GW170817 seem to suggest that the symmetry energy is soft, thereby excluding models that predict overly large stellar radii.

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J. Piekarewicz
Wed, 12 Dec 18
42/92

Comments: 16 pages, 4 figures, Invited Lecture presented at the Zakopane Conference on Nuclear Physics “Extremes of the Nuclear Landscape”, Zakopane, Poland, August 26-September 2, 2018. To be published in ACTA PHYSICA POLONICA B Volume 50

Solar Neutrino Measurements [CL]

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http://arxiv.org/abs/1812.02326


We present the most recent results from the two currently running solar neutrino experiments, Borexino at the Gran Sasso laboratory in Italy and SuperK at Kamioka mine in Japan. SuperK has released the most precise yet measurement of the 8B solar neutrino interaction rate, with a precision better than 2\%, consistent with a constant solar neutrino emission over more than a decade. Borexino has released refined measurements of all neutrinos produced in the pp fusion chain. For the first time, one single detector has measured the entire range of solar neutrinos at once. These new data weakly favor a high-metallicity Sun. Prospects for measuring CNO solar neutrinos with Borexino are discussed, and a brief outlook on the field provided.

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A. Pocar
Fri, 7 Dec 18
64/66

Comments: 10 pages, 9 figures, “XXXVIII International Symposium on Physics in Collision, Bogot\’a, Colombia, 11-15 september 2018”. arXiv admin note: substantial text overlap with arXiv:1810.12967