RAS_WEB (Page 2,338)

Electroweak baryogenesis by primordial black holes in Brans-Dicke modified gravity. (arXiv:2006.13621v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Aliferis_G/0/1/0/all/0/1">Georgios Aliferis</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zarikas_V/0/1/0/all/0/1">Vasilios Zarikas</a> A successful baryogenesis mechanism is proposed in the cosmological framework of Brans-Dicke modified gravity. Primordial black holes with small mass are produced at the end of the Brans-Dicke field domination era. The Hawking radiation reheats a spherical region around every black hole to a high temperature and the electroweak symmetry is restored there. A domain wall is formed separating the region with the symmetric vacuum from the asymmetric region where electroweak baryogenesis takes place. First order phase transition is not needed. In Brans-Dicke cosmologies black holeRead More →

Diffusion of large-scale magnetic fields by reconnection in MHD turbulence. (arXiv:2005.07775v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_Lima_R/0/1/0/all/0/1">R. Santos-Lima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerrero_G/0/1/0/all/0/1">G. Guerrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pino_E/0/1/0/all/0/1">E. M. de Gouveia Dal Pino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazarian_A/0/1/0/all/0/1">A. Lazarian</a> The rate of magnetic field diffusion plays an essential role in several astrophysical plasma processes. It has been demonstrated that the omnipresent turbulence in astrophysical media induces fast magnetic reconnection, which consequently leads to large-scale magnetic flux diffusion at a rate independent of the plasma microphysics. This process is called “reconnection diffusion” (RD) and allows for the diffusion of fields which are dynamically important. The current theory describing RD is based on incompressible magnetohydrodynamic (MHD) turbulence.Read More →

Insights into searches for anisotropies in the nanohertz gravitational-wave background. (arXiv:2010.13958v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Ali_Haimoud_Y/0/1/0/all/0/1">Yacine Ali-Ha&#xef;moud</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Smith_T/0/1/0/all/0/1">Tristan L. Smith</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Mingarelli_C/0/1/0/all/0/1">Chiara M. F. Mingarelli</a> Within the next several years pulsar timing arrays (PTAs) are positioned to detect the stochastic gravitational-wave background (GWB) likely produced by the collection of inspiralling super-massive black holes binaries, and potentially constrain some exotic physics. So far most of the pulsar timing data analysis has focused on the monopole of the GWB, assuming it is perfectly isotropic. The natural next step is to search for anisotropies in the GWB. In this paper, we use the recently developed PTA Fisher matrixRead More →

Inflation in Motion: Unitarity Constraints in Effective Field Theories with Broken Lorentz Symmetry. (arXiv:2005.02366v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Grall_T/0/1/0/all/0/1">Tanguy Grall</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Melville_S/0/1/0/all/0/1">Scott Melville</a> During inflation, there is a preferred reference frame in which the expansion of the background spacetime is spatially isotropic. In contrast to Minkowski spacetime, observables can depend on the velocity of the system with respect to this cosmic rest frame. We derive new constraints from radiative stability and unitarity on effective field theories with such spontaneously broken Lorentz symmetry. In addition to a maximum energy scale, there is now also a critical velocity at which the theory breaks down. The theory therefore hasRead More →

Dynamical Modeling of Galaxies and Supermassive Black Holes: Axisymmetry in Triaxial Schwarzschild Orbit Superposition Models. (arXiv:2005.00542v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Quenneville_M/0/1/0/all/0/1">Matthew E. Quenneville</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liepold_C/0/1/0/all/0/1">Christopher M. Liepold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ma_C/0/1/0/all/0/1">Chung-Pei Ma</a> We present a detailed analysis of the behavior of the triaxial Schwarzschild orbit superposition method near the axisymmetric limit. Orbit superposition modeling is the primary method used to determine dynamical masses of supermassive black holes ($M_mathrm{BH}$) in nearby galaxies; however, prior studies have reported conflicting results when comparing the outcome from axisymmetric orbit codes with that from a triaxial orbit code in the axisymmetric limit. We show that in order to achieve (oblate) axisymmetry in aRead More →

Limits on $w$CDM from the EFTofLSS with the PyBird code. (arXiv:2003.07956v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+DAmico_G/0/1/0/all/0/1">Guido D&#x27;Amico</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Senatore_L/0/1/0/all/0/1">Leonardo Senatore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_P/0/1/0/all/0/1">Pierre Zhang</a> We apply the Effective Field Theory of Large-Scale Structure to analyze the $w$CDM cosmological model. By using the full shape of the power spectrum and the BAO post-reconstruction measurements from BOSS, the Supernovae from Pantheon, and a prior from BBN, we set the competitive CMB-independent limit $w=-1.046_{-0.052}^{+0.055}$ at $68%$ C.L.. After adding the Planck CMB data, we find $w=-1.023_{-0.030}^{+0.033}$ at $68%$ C.L.. Our results are obtained using PyBird, a new, fast Python-based code which we make publicly available. We apply the Effective FieldRead More →

An Atmospheric Cerenkov Telescope Simulation System. (arXiv:2001.06978v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sinha_S/0/1/0/all/0/1">Srikanta Sinha</a> A detailed numerical procedure has been developed to simulate the mechanical configurations and optical properties of Imaging Atmospheric Cerenkov Telescope systems. To test these procedures a few existing ACT arrays are simulated. First results from these simulations are presented. A detailed numerical procedure has been developed to simulate the mechanical configurations and optical properties of Imaging Atmospheric Cerenkov Telescope systems. To test these procedures a few existing ACT arrays are simulated. First results from these simulations are presented. http://arxiv.org/icons/sfx.gifRead More →

Gravitational redshift/blueshift of light emitted by geodesic test particles, frame-dragging and pericentre-shift effects, in the Kerr-Newman-de Sitter and Kerr-Newman black hole geometries. (arXiv:1912.10320v5 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Kraniotis_G/0/1/0/all/0/1">G. V. Kraniotis</a> We investigate the redshift and blueshift of light emitted by timelike geodesic particles in orbits around a Kerr-Newman-(anti) de Sitter (KN(a)dS) black hole. Specifically we compute the redshift and blueshift of photons that are emitted by geodesic massive particles and travel along null geodesics towards a distant observer-located at a finite distance from the KN(a)dS black hole. For this purpose we use the Killing-vector formalism and the associated first integrals-constants of motion. We consider in detailRead More →

Radiation from Global Topological Strings using Adaptive Mesh Refinement: Methodology and Massless Modes. (arXiv:1910.01718v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Drew_A/0/1/0/all/0/1">Amelia Drew</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shellard_E/0/1/0/all/0/1">E.P.S. Shellard</a> We implement adaptive mesh refinement (AMR) simulations of global topological strings using the public numerical relativity code, GRChombo. We perform a quantitative investigation of the dynamics of single sinusoidally displaced string configurations, studying a wide range of string energy densities $mu propto ln{lambda}$, defined by the string width parameter $lambda$ over two orders of magnitude. We investigate the resulting massless (Goldstone boson or axion) radiation signals, using quantitative diagnostic tools to determine the eigenmode decomposition. Given analytic radiation predictions, we compare the oscillatingRead More →

Entering into the Wide Field Adaptive Optics Era on Maunakea. (arXiv:1907.08169v3 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sivo_G/0/1/0/all/0/1">Gaetano Sivo</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Blakeslee_J/0/1/0/all/0/1">John Blakeslee</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Lotz_J/0/1/0/all/0/1">Jennifer Lotz</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Roe_H/0/1/0/all/0/1">Henry Roe</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Andersen_M/0/1/0/all/0/1">Morten Andersen</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Scharwachter_J/0/1/0/all/0/1">Julia Scharwachter</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Palmer_D/0/1/0/all/0/1">David Palmer</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Kleinman_S/0/1/0/all/0/1">Scot Kleinman</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Adamson_A/0/1/0/all/0/1">Andy Adamson</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Hirst_P/0/1/0/all/0/1">Paul Hirst</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Marin_E/0/1/0/all/0/1">Eduardo Marin</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Catala_L/0/1/0/all/0/1">Laure Catala</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Dam_M/0/1/0/all/0/1">Marcos van Dam</a> (Flat Wavefronts), <a href="http://arxiv.org/find/astro-ph/1/au:+Goodsell_S/0/1/0/all/0/1">Stephen Goodsell</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Provost_N/0/1/0/all/0/1">Natalie Provost</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_R/0/1/0/all/0/1">Ruben Diaz</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_I/0/1/0/all/0/1">Inger Jorgensen</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_H/0/1/0/all/0/1">Hwihyun Kim</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Lemoine_Busserole_M/0/1/0/all/0/1">Marie Lemoine-Busserole</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Blain_C/0/1/0/all/0/1">Celia Blain</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Chun_M/0/1/0/all/0/1">Mark Chun</a> (IfA – U. Hawaii), <a href="http://arxiv.org/find/astro-ph/1/au:+Ammons_M/0/1/0/all/0/1">Mark Ammons</a>Read More →

Finding Strong Gravitational Lenses in the DESI DECam Legacy Survey. (arXiv:1906.00970v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_X/0/1/0/all/0/1">X. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Domingo_M/0/1/0/all/0/1">M. Domingo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pilon_A/0/1/0/all/0/1">A. Pilon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ravi_V/0/1/0/all/0/1">V. Ravi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Storfer_C/0/1/0/all/0/1">C. Storfer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlegel_D/0/1/0/all/0/1">D.J. Schlegel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailey_S/0/1/0/all/0/1">S. Bailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dey_A/0/1/0/all/0/1">A. Dey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herrera_D/0/1/0/all/0/1">D. Herrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juneau_S/0/1/0/all/0/1">S. Juneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landriau_M/0/1/0/all/0/1">M. Landriau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lang_D/0/1/0/all/0/1">D. Lang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meisner_A/0/1/0/all/0/1">A. Meisner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moustakas_J/0/1/0/all/0/1">J. Moustakas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Myers_A/0/1/0/all/0/1">A.D. Myers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlafly_E/0/1/0/all/0/1">E.F. Schlafly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valdes_F/0/1/0/all/0/1">F. Valdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_B/0/1/0/all/0/1">B.A. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_J/0/1/0/all/0/1">J. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yeche_C/0/1/0/all/0/1">C. Yeche</a> We perform a semi-automated search for strong gravitational lensing systems in the 9,000 deg$^2$ Dark Energy Camera Legacy Survey (DECaLS), part of the DESI Legacy Imaging Surveys (Dey et al.). The combinationRead More →

Primary beam effects of radio astronomy antennas — II. Modelling the MeerKAT L-band beam. (arXiv:1904.07155v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Asad_K/0/1/0/all/0/1">K. M. B. Asad</a> (1, 2, 3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Girard_J/0/1/0/all/0/1">J. N. Girard</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Villers_M/0/1/0/all/0/1">M. de Villers</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Ansah_Narh_T/0/1/0/all/0/1">T. Ansah-Narh</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Iheanetu_K/0/1/0/all/0/1">K. Iheanetu</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Smirnov_O/0/1/0/all/0/1">O. Smirnov</a> (2, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_M/0/1/0/all/0/1">M. G. Santos</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Lehmensiek_R/0/1/0/all/0/1">R. Lehmensiek</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Jonas_J/0/1/0/all/0/1">J. Jonas</a> (2, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Villiers_D/0/1/0/all/0/1">D. I. L. de Villiers</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Thorat_K/0/1/0/all/0/1">K. Thorat</a> (2, 4, 8), <a href="http://arxiv.org/find/astro-ph/1/au:+Hugo_B/0/1/0/all/0/1">B. Hugo</a> (2, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Makhathini_S/0/1/0/all/0/1">S. Makhathini</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Jozsa_G/0/1/0/all/0/1">G. I. G. Jozsa</a> (2, 4, 9), <a href="http://arxiv.org/find/astro-ph/1/au:+Sirothia_S/0/1/0/all/0/1">S. K. Sirothia</a> (2, 4) ((2) Department of Physics andRead More →

Approach to scaling in axion string networks. (arXiv:2102.07723v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hindmarsh_M/0/1/0/all/0/1">Mark Hindmarsh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lizarraga_J/0/1/0/all/0/1">Joanes Lizarraga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Eiguren_A/0/1/0/all/0/1">Asier Lopez-Eiguren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urrestilla_J/0/1/0/all/0/1">Jon Urrestilla</a> We study the approach to scaling in axion string networks in the radiation era, through measuring the root-mean-square velocity $v$ as well as the scaled mean string separation $x$. We find good evidence for a fixed point in the phase-space analysis in the variables $(x,v)$, providing a strong indication that standard scaling is taking place. We show that the approach to scaling can be well described by a two parameter velocity-one-scale (VOS) model, and show that the values of the parameters are insensitive toRead More →

Fully general-relativistic simulations of isolated and binary strange quark stars. (arXiv:2102.07721v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Z/0/1/0/all/0/1">Zhenyu Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rezzolla_L/0/1/0/all/0/1">Luciano Rezzolla</a> The hypothesis that strange quark matter is the true ground state of matter has been investigated for almost four decades, but only a few works have explored the dynamics of binary systems of quark stars. This is partly due to the numerical challenges that need to be faced when modelling the large discontinuities at the surface of these stars. We here present a novel technique in which the EOS of a quark star is suitably rescaled to produce a smooth change of the specific enthalpy across aRead More →

Probing Galaxy Bias and Intergalactic Gas Pressure with KiDS Galaxies-tSZ-CMB Lensing Cross-correlations. (arXiv:2102.07701v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_Z/0/1/0/all/0/1">Ziang Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Waerbeke_L/0/1/0/all/0/1">Ludovic van Waerbeke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Troster_T/0/1/0/all/0/1">Tilman Tr&#xf6;ster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_A/0/1/0/all/0/1">Angus H. Wright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_D/0/1/0/all/0/1">David Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asgari_M/0/1/0/all/0/1">Marika Asgari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilicki_M/0/1/0/all/0/1">Maciej Bilicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erben_T/0/1/0/all/0/1">Thomas Erben</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu_S/0/1/0/all/0/1">Shiming Gu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heymans_C/0/1/0/all/0/1">Catherine Heymans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hildebrandt_H/0/1/0/all/0/1">Hendrik Hildebrandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinshaw_G/0/1/0/all/0/1">Gary Hinshaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koukoufilippas_N/0/1/0/all/0/1">Nick Koukoufilippas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kannawadi_A/0/1/0/all/0/1">Arun Kannawadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuijken_K/0/1/0/all/0/1">Konrad Kuijken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mead_A/0/1/0/all/0/1">Alexander Mead</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shan_H/0/1/0/all/0/1">HuanYuan Shan</a> We constrain the redshift dependence of gas pressure bias $leftlangle b_{y} P_{mathrm{e}}rightrangle$ (bias-weighted average electron pressure), which characterises the thermodynamics of intergalactic gas, through a combination of cross-correlations between galaxy positions and the thermal Sunyaev-Zeldovich (tSZ) effect, asRead More →

On the Core-Halo Mass Relation in Scalar Field Dark Matter Models and its Consequences for the Formation of Supermassive Black Holes. (arXiv:2010.12716v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_L/0/1/0/all/0/1">Luis E. Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rindler_Daller_T/0/1/0/all/0/1">Tanja Rindler-Daller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shapiro_P/0/1/0/all/0/1">Paul R. Shapiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matos_T/0/1/0/all/0/1">Tonatiuh Matos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazquez_J/0/1/0/all/0/1">J. Alberto V&#xe1;zquez</a> Scalar-field dark matter (SFDM) halos exhibit a core-envelope structure with soliton-like cores and CDM-like envelopes. Simulations without self-interaction (free-field case) report a core-halo mass relation $M_cpropto M_{h}^{beta}$, with either $beta=1/3$ or $beta=5/9$, which can be understood if core and halo obey certain energy or velocity scalings. We extend the core-halo mass relations to include SFDM with self-interaction (SI), either repulsive or attractive, andRead More →

The impact of mass-transfer physics on the observable properties of field binary black hole populations. (arXiv:2010.16333v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bavera_S/0/1/0/all/0/1">Simone S. Bavera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fragos_T/0/1/0/all/0/1">Tassos Fragos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zevin_M/0/1/0/all/0/1">Michael Zevin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berry_C/0/1/0/all/0/1">Christopher P. L. Berry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchant_P/0/1/0/all/0/1">Pablo Marchant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_J/0/1/0/all/0/1">Jeff J. Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_S/0/1/0/all/0/1">Scott Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dotter_A/0/1/0/all/0/1">Aaron Dotter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovlakas_K/0/1/0/all/0/1">Konstantinos Kovlakas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Misra_D/0/1/0/all/0/1">Devina Misra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serra_Perez_J/0/1/0/all/0/1">Juan G. Serra-Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qin_Y/0/1/0/all/0/1">Ying Qin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rocha_K/0/1/0/all/0/1">Kyle A. Rocha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roman_Garza_J/0/1/0/all/0/1">Jaime Rom&#xe1;n-Garza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tran_N/0/1/0/all/0/1">Nam H. Tran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zapartas_E/0/1/0/all/0/1">Emmanouil Zapartas</a> We study the impact of mass-transfer physics on the observable properties of binary black hole populations formed through isolated binary evolution. We investigate the impact of mass-accretion efficiency onto compact objects andRead More →

A backward-spinning star with two coplanar planets. (arXiv:2102.07677v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hjorth_M/0/1/0/all/0/1">Maria Hjorth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albrecht_S/0/1/0/all/0/1">Simon Albrecht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirano_T/0/1/0/all/0/1">Teruyuki Hirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_R/0/1/0/all/0/1">Rebekah I. Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zanazzi_J/0/1/0/all/0/1">J. J. Zanazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knudstrup_E/0/1/0/all/0/1">Emil Knudstrup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sato_B/0/1/0/all/0/1">Bun&#x27;ei Sato</a> It is widely assumed that a star and its protoplanetary disk are initially aligned, with the stellar equator parallel to the disk plane. When observations reveal a misalignment between stellar rotation and the orbital motion of a planet, the usual interpretation is that the initial alignment was upset by gravitational perturbations that took place after planet formation. Most of the previously known misalignments involve isolated hot Jupiters, for whichRead More →

Closer look at white hole remnants. (arXiv:2101.01949v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Barrau_A/0/1/0/all/0/1">Aur&#xe9;lien Barrau</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ferdinand_L/0/1/0/all/0/1">L&#xe9;onard Ferdinand</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Martineau_K/0/1/0/all/0/1">Killian Martineau</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Renevey_C/0/1/0/all/0/1">Cyril Renevey</a> The idea that, after their evaporation, Planck-mass black holes might tunnel into metastable white holes has recently been intensively studied. Those relics have been considered as a dark matter candidate. We show that the model is severely constrained and underline some possible detection paths. We also investigate, in a more general setting, the way the initial black hole mass spectrum would be distorted by both the bouncing effect and the Hawking evaporation. The idea that, after their evaporation, Planck-mass black holes might tunnel intoRead More →

One-electron ion in a quantizing magnetic field. (arXiv:2102.06488v2 [physics.atom-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Demidov_I/0/1/0/all/0/1">I. V. Demidov</a>, <a href="http://arxiv.org/find/physics/1/au:+Potekhin_A/0/1/0/all/0/1">A. Y. Potekhin</a> A charged particle in a magnetic field possesses discrete energy levels associated with particle rotation around the field lines. A bound complex of particles with a nonzero net charge possesses an analogous levels associated with its center-of-mass motion and, in addition, the levels associated with internal degrees of freedom, that is with relative motions of its constituent particles. The center-of-mass and internal motions are mutually dependent, which complicates theoretical studies of the binding energies, radiative transitions and other properties of the complex ions moving in quantizing magneticRead More →