Incompressible wind accretion [HEAP]

http://arxiv.org/abs/1705.07093


We present a simple, analytic model for the accretion flow of an incompressible wind onto a gravitating object. This solution corresponds to the Newtonian limit of a previously known relativistic model for a fluid obeying a stiff equation of state for which the sound speed is constant everywhere and equal to the speed of light. The new solution should be useful as a benchmark test for numerical hydrodynamics codes and, moreover, it can be used as an illustrative example in a gas dynamics course.

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E. Tejeda
Mon, 22 May 17
8/51

Comments: 7 pages, 3 figures. Submitted. Comments welcome

Stability of Einstein static universe in Eddington-inspire Born-Infeld theory [CL]

http://arxiv.org/abs/1705.06819


By considering the realization of emergent universe scenario in Eddington-inspire Born-Infeld (EiBI) theory, we study the stability of Einstein static universe filled with perfect fluid in EiBI theory against both the homogeneous and inhomogeneous scalar perturbations in this work. We find that in both the spatially flat and closed cases, the emergent universe scenario is no longer viable, since Einstein static universe cannot be stable against both the homogeneous and inhomogeneous scalar perturbations simultaneously. However, the emergent universe scenario survives in the spatially open case, while Einstein static universe can be stable under some conditions.

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S. Li and H. Wei
Mon, 22 May 17
15/51

Comments: 10 pages, revtex4

Oscillation modes of rapidly rotating neutron stars in scalar-tensor theories of gravity [CL]

http://arxiv.org/abs/1705.06984


We perform the first study of the oscillation frequencies of rapidly rotating neutron stars in alternative theories of gravity, focusing mainly on the fundamental $f$-modes. We concentrated on a particular class of alternative theories – the (massive) scalar-tensor theories. The generalization to rapid rotation is important because on one hand the rapid rotation can magnify the deviations from general relativity compared to the static case and on the other hand some of the most efficient emitters of gravitational radiation, such as the binary neutron star merger remnants, are supposed to be rotating close to their Kepler (mass-shedding) limits shortly after their formation. We have constructed several sequences of models starting from the nonrotating case and reaching up to the Kepler limit, with different values of the scalar-tensor theory coupling constant and the scalar field mass. The results show that the deviations from pure Einstein’s theory can be significant especially in the case of nonzero scalar field mass. An important property of the oscillation modes of rapidly rotating stars is that they can become secularly unstable due to the emission of gravitational radiation, that is so-called Chandrasekhar-Friedman-Schutz instability. Such unstable modes are efficient emitters of gravitational radiation. Our studies show that the inclusion of nonzero scalar field would decrease the threshold value of the normalized angular momentum where this instability stars to operate, but the growth time of the instability seems to be increased compared to pure general relativity.

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S. Yazadjiev, D. Doneva and K. Kokkotas
Mon, 22 May 17
26/51

Comments: 9 pages, 2 figures

The nonspinning binary black hole merger scenario revisited [CL]

http://arxiv.org/abs/1705.07034


We present the results of 14 simulations of nonspinning black hole binaries with mass ratios $q=m_1/m_2$ in the range $1/100\leq q\leq1$. For each of these simulations we perform three runs at increasing resolution to assess the finite difference errors and to extrapolate the results to infinite resolution. For $q\geq 1/6$, we follow the evolution of the binary typically for the last ten orbits prior to merger. By fitting the results of these simulations, we accurately model the peak luminosity, peak waveform frequency and amplitude, and the recoil of the remnant hole for unequal mass nonspinning binaries. We verify the accuracy of these new models and compare them to previously existing empirical formulas. These new fits provide a basis for a hierarchical approach to produce more accurate remnant formulas in the generic precessing case. They also provide input to gravitational waveform modeling.

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J. Healy, C. Lousto and Y. Zlochower
Mon, 22 May 17
34/51

Comments: 8 pages, 4 figures

On the Inflationary Perturbations of Massive Higher-Spin Fields [CL]

http://arxiv.org/abs/1705.05834


Cosmological perturbations of massive higher-spin fields are generated during inflation, but they decay on scales larger than the Hubble radius as a consequence of the Higuchi bound. By introducing suitable couplings to the inflaton field, we show that one can obtain statistical correlators of massive higher-spin fields which remain constant or decay very slowly outside the Hubble radius. This opens up the possibility of new observational signatures from inflation.

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A. Kehagias and A. Riotto
Fri, 19 May 17
15/62

Comments: 22 pages

Is Patience a Virtue? Cosmic Censorship of Infrared Effects in de Sitter [CL]

http://arxiv.org/abs/1705.06380


While the accumulation of long wavelength modes during inflation wreaks havoc on the large scale structure of spacetime, the question of even observability of their presence by any local observer has lead to considerable confusion. Though it is commonly agreed that infrared effects are not visible to a single sub-horizon observer at late times, we argue that the question is less trivial for a \emph{patient observer} who has lived long enough to have a record of the state before the soft mode was created. Though classically there is no obstruction to measuring this effect locally, we give several indications that quantum mechanical uncertainties censor the effect, rendering the observation of long modes ultimately forbidden.

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R. Ferreira, M. Sandora and M. Sloth
Fri, 19 May 17
20/62

Comments: 7 pages, awarded honorable mention in the 2017 Gravity Research Foundation Essays on Gravitation competition

A proof of the weak gravity conjecture [CL]

http://arxiv.org/abs/1705.06287


The weak gravity conjecture suggests that, in a self-consistent theory of quantum gravity, the strength of gravity is bounded from above by the strengths of the various gauge forces in the theory. In particular, this intriguing conjecture asserts that in a theory describing a U(1) gauge field coupled consistently to gravity, there must exist a particle whose proper mass is bounded (in Planck units) by its charge: $m/m_{\text{P}}<q$. This beautiful and remarkably compact conjecture has attracted the attention of physicists and mathematicians over the last decade. It should be emphasized, however, that despite the fact that there are numerous examples from field theory and string theory that support the conjecture, we still lack a general proof of its validity. In the present Letter we prove that the weak gravity conjecture (and, in particular, the mass-charge upper bound $m/m_{\text{P}}<q$) can be inferred directly from Bekenstein’s generalized second law of thermodynamics, a law which is widely believed to reflect a fundamental aspect of the elusive theory of quantum gravity.

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S. Hod
Fri, 19 May 17
22/62

Comments: 7 pages. This essay is awarded 4th Prize in the 2017 Essay Competition of the Gravity Research Foundation