April 2021 (Page 2)

Iterative solutions for the gravitational lens equation in the strong deflection limit. (arXiv:2103.10649v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Takizawa_K/0/1/0/all/0/1">Keita Takizawa</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Asada_H/0/1/0/all/0/1">Hideki Asada</a> Two exact lens equations have been recently shown to be equivalent to each other, being consistent with the gravitational deflection angle of light from a source to an observer, both of which can be within a finite distance from a lens object [Phys. Rev. D 102, 064060 (2020)]. We examine methods for iterative solutions of the gravitational lens equations in the strong deflection limit. It has been so far unclear whether a convergent series expansion can be provided by the gravitational lens approach basedRead More →

The Atacama Cosmology Telescope: Summary of DR4 and DR5 Data Products and Data Access. (arXiv:2103.03154v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Mallaby_Kay_M/0/1/0/all/0/1">Maya Mallaby-Kay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Atkins_Z/0/1/0/all/0/1">Zachary Atkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiola_S/0/1/0/all/0/1">Simone Aiola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amodeo_S/0/1/0/all/0/1">Stefania Amodeo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austermann_J/0/1/0/all/0/1">Jason E. Austermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beall_J/0/1/0/all/0/1">James A. Beall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_D/0/1/0/all/0/1">Daniel T. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_J/0/1/0/all/0/1">J. Richard Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chesmore_G/0/1/0/all/0/1">Grace E. Chesmore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">Steve K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crowley_K/0/1/0/all/0/1">Kevin T. Crowley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Darwish_O/0/1/0/all/0/1">Omar Darwish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Denison_E/0/1/0/all/0/1">Edwawd V. Denison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark J. Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duff_S/0/1/0/all/0/1">Shannon M. Duff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_A/0/1/0/all/0/1">Adriaan J. Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">Jo Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fichman_K/0/1/0/all/0/1">Kyra Fichman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_P/0/1/0/all/0/1">Patricio A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golec_J/0/1/0/all/0/1">Joseph E. Golec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guan_Y/0/1/0/all/0/1">Yilun Guan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_D/0/1/0/all/0/1">Dongwon Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasselfield_M/0/1/0/all/0/1">Matthew Hasselfield</a>,Read More →

An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685. (arXiv:2103.01016v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bluhm_P/0/1/0/all/0/1">P. Bluhm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palle_E/0/1/0/all/0/1">E. Palle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molaverdikhani_K/0/1/0/all/0/1">K. Molaverdikhani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kemmer_J/0/1/0/all/0/1">J. Kemmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatzes_A/0/1/0/all/0/1">A. P. Hatzes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kossakowski_D/0/1/0/all/0/1">D. Kossakowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stock_S/0/1/0/all/0/1">S. Stock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lillo_Box_J/0/1/0/all/0/1">J. Lillo-Box</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bejar_V/0/1/0/all/0/1">V. J. S .Bejar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soto_M/0/1/0/all/0/1">M. G. Soto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amado_P/0/1/0/all/0/1">P. J. Amado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_P/0/1/0/all/0/1">P. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cadieux_C/0/1/0/all/0/1">C. Cadieux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cloutier_R/0/1/0/all/0/1">R. Cloutier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_K/0/1/0/all/0/1">K. A. Collins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_K/0/1/0/all/0/1">K. I. Collins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortes_Contreras_M/0/1/0/all/0/1">M. Cortes-Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doyon_R/0/1/0/all/0/1">R. Doyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dreizler_S/0/1/0/all/0/1">S. Dreizler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espinoza_N/0/1/0/all/0/1">N. Espinoza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukui_A/0/1/0/all/0/1">A. Fukui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Alvarez_E/0/1/0/all/0/1">E. Gonzalez-Alvarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Th. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horne_K/0/1/0/all/0/1">K. Horne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jeffers_S/0/1/0/all/0/1">S. V. Jeffers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">J. M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_E/0/1/0/all/0/1">E.Read More →

When tension is just a fluctuation: How noisy data affect model comparison. (arXiv:2102.09547v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Joachimi_B/0/1/0/all/0/1">B. Joachimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohlinger_F/0/1/0/all/0/1">F. K&#xf6;hlinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handley_W/0/1/0/all/0/1">W. Handley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemos_P/0/1/0/all/0/1">P. Lemos</a> Summary statistics of the likelihood, such as the Bayesian evidence, offer a principled way of comparing models and assessing tension between, or within, the results of physical experiments. Noisy realisations of the data induce scatter in these model comparison statistics. For a realistic case of cosmological inference from large-scale structure we show that the logarithm of the Bayes factor attains scatter of order unity, increasing significantly with stronger tension between the models under comparison. We develop an approximateRead More →

Probing core overshooting using subgiant asteroseismology: the case of KIC10273246. (arXiv:2101.11025v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Noll_A/0/1/0/all/0/1">A. Noll</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deheuvels_S/0/1/0/all/0/1">S. Deheuvels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballot_J/0/1/0/all/0/1">J. Ballot</a> The size of convective cores remains uncertain, despite its substantial influence on stellar evolution, and thus on stellar ages. The seismic modeling of young subgiants can be used to obtain indirect constraints on the core structure during main sequence, thanks to the high probing potential of mixed modes. We selected the young subgiant KIC10273246, observed by Kepler, based on its mixed-mode properties. We thoroughly modeled this star, with the aim of placing constraints on the size of its main sequence convective core. WeRead More →

Evryscope-South Survey of Upper- and Pre-main Sequence Solar Neighborhood Stars. (arXiv:2008.07570v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Galliher_N/0/1/0/all/0/1">Nathan W. Galliher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ratzloff_J/0/1/0/all/0/1">Jeffrey K. Ratzloff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corbett_H/0/1/0/all/0/1">Henry Corbett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Law_N/0/1/0/all/0/1">Nicholas M. Law</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_W/0/1/0/all/0/1">Ward S. Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glazier_A/0/1/0/all/0/1">Amy L. Glazier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soto_A/0/1/0/all/0/1">Alan Vasquez Soto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_R/0/1/0/all/0/1">Ramses Gonzalez</a> Using photometric data collected by Evryscope-South, we search for nearby young variable systems on the upper-main sequence (UMS) and pre-main sequence (PMS). The Evryscopes are all-sky high-cadence telescope arrays operating in the Northern and Southern hemispheres. We base our search on a Gaia-selected catalog of young neighborhood upper- and pre-main sequence stars which were chosen through both astrometric and photometric criteria. WeRead More →

Explaining the scatter in the galaxy mass-metallicity relation with gas flows. (arXiv:2101.11021v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Loon_M/0/1/0/all/0/1">Maria L. van Loon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mitchell_P/0/1/0/all/0/1">Peter D. Mitchell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaye_J/0/1/0/all/0/1">Joop Schaye</a> The physical origin of the scatter in the relation between galaxy stellar mass and the metallicity of the interstellar medium, i.e. the Mass-Metallicity Relation (MZR), reflects the relative importance of key processes in galaxy evolution. The eagle cosmological hydrodynamical simulation is used to investigate the correlations between the residuals of the MZR and the residuals of the relations between stellar mass and, respectively, specific inflow, outflow and star formation rate as well as the gas fraction for central galaxies.Read More →

Off-axis jet scenario for early afterglow emission of low-luminosity gamma-ray burst GRB 190829A. (arXiv:2101.10581v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sato_Y/0/1/0/all/0/1">Yuri Sato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Obayashi_K/0/1/0/all/0/1">Kaori Obayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamazaki_R/0/1/0/all/0/1">Ryo Yamazaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murase_K/0/1/0/all/0/1">Kohta Murase</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohira_Y/0/1/0/all/0/1">Yutaka Ohira</a> Recently, ground-based Imaging Atmospheric Cherenkov Telescopes have reported the detection of very-high-energy (VHE) gamma-rays from some gamma-ray bursts (GRBs). One of them, GRB~190829A, was triggered by the Swift satellite, and about 20000 s after the burst onset the VHE gamma-ray emission was detected by H.E.S.S. with ~ 5 sigma significance. This event had unusual features of having much smaller isotropic equivalent gamma-ray energy than typical long GRBs and achromatic peaks in X-ray and opticalRead More →

Propagation of quantum gravity-modified gravitational waves on a classical FLRW spacetime. (arXiv:2012.09366v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Garcia_Chung_A/0/1/0/all/0/1">Angel Garcia-Chung</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Mertens_J/0/1/0/all/0/1">James B. Mertens</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Rastgoo_S/0/1/0/all/0/1">Saeed Rastgoo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Tavakoli_Y/0/1/0/all/0/1">Yaser Tavakoli</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moniz_P/0/1/0/all/0/1">Paulo Vargas Moniz</a> The linearized Einstein field equations provide a low-energy wave equation for the propagation of gravitational fields which may originate from a high energy source. Motivated by loop quantum gravity, we propose the polymer quantization scheme to derive the effective propagation of such waves on a classical Friedmann-Lemaitre-Robertson-Walker (FLRW) spacetime. To overcome the challenge of polymer quantizing a time-dependent Hamiltonian, we rewrite such a Hamiltonian in a time-independent manner in the extended phase space, polymerizeRead More →

Prospects for Measuring the Hubble Constant with Neutron-Star-Black-Hole Mergers. (arXiv:2012.06593v4 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Feeney_S/0/1/0/all/0/1">Stephen M. Feeney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peiris_H/0/1/0/all/0/1">Hiranya V. Peiris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nissanke_S/0/1/0/all/0/1">Samaya M. Nissanke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mortlock_D/0/1/0/all/0/1">Daniel J. Mortlock</a> Gravitational wave (GW) and electromagnetic (EM) observations of neutron-star-black-hole (NSBH) mergers can provide precise local measurements of the Hubble constant ($H_0$), ideal for resolving the current $H_0$ tension. We perform end-to-end analyses of realistic populations of simulated NSBHs, incorporating both GW and EM selection for the first time. We show that NSBHs could achieve unbiased 1.5-2.4% precision $H_0$ estimates by 2030. The achievable precision is strongly affected by the details of spin precession and tidal disruption, highlightingRead More →

Cooling of young neutron stars and dark gauge bosons. (arXiv:2012.05427v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Hong_D/0/1/0/all/0/1">Deog Ki Hong</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Shin_C/0/1/0/all/0/1">Chang Sub Shin</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yun_S/0/1/0/all/0/1">Seokhoon Yun</a> The standard cooling scenario in the presence of nucleon superfluidity fits rather well to the observation of the neutron stars. It implies that the stellar cooling arguments could place a stringent constraint on the properties of novel particles. We study in particular the cooling rate induced by dark gauge bosons for very young neutron stars: remnants of Cassiopeia A and SN1987A. The cooling is dominantly contributed either by the nucleon pair breaking and formation in the core or by the electron bremsstrahlungRead More →

Irreducible cosmic production of relic vortons. (arXiv:2010.04620v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Auclair_P/0/1/0/all/0/1">Pierre Auclair</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_P/0/1/0/all/0/1">Patrick Peter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ringeval_C/0/1/0/all/0/1">Christophe Ringeval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steer_D/0/1/0/all/0/1">Daniele Steer</a> The existence of a scaling network of current-carrying cosmic strings in our Universe is expected to continuously create loops endowed with a conserved current during the cosmological expansion. These loops radiate gravitational waves and may stabilise into centrifugally supported configurations. We show that this process generates an irreducible population of vortons which has not been considered so far. In particular, we expect vortons to be massively present today even if no loops are created at the time of string formation. We determine their cosmologicalRead More →

Purely kinetic k-essence description of $c_s^2(w)$ barotropic fluid models. (arXiv:2009.08680v4 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Perkovic_D/0/1/0/all/0/1">Dalibor Perkovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stefancic_H/0/1/0/all/0/1">Hrvoje Stefancic</a> Purely kinetic k-essence models have been shown in the literature to be a field theory equivalent of barotropic fluid models of dark energy or dark matter-dark energy unification. In the modeling framework where the speed of sound squared of a barotropic fluid is modeled as a function of its Equation of State parameter, a systematic procedure of obtaining the Lagrangian density of an equivalent purely kinetic k-essence model is presented. As this modeling approach starts from the speed of sound, purely kinetic k-essence models can be constructedRead More →

Non-linear damping of standing kink waves computed with Elsasser variables. (arXiv:2104.14331v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Doorsselaere_T/0/1/0/all/0/1">Tom Van Doorsselaere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goossens_M/0/1/0/all/0/1">Marcel Goossens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magyar_N/0/1/0/all/0/1">Norbert Magyar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruderman_M/0/1/0/all/0/1">Michael S. Ruderman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ismayilli_R/0/1/0/all/0/1">Rajab Ismayilli</a> In a previous paper, we computed the energy density and the non-linear energy cascade rate for transverse kink waves using Elsasser variables. In this paper, we focus on the standing kink waves, which are impulsively excited in coronal loops by external perturbations. We present an analytical calculation to compute the damping time due to the non-linear development of the Kelvin-Helmholtz instability. The main result is that the damping time is inversely proportional to the oscillation amplitude.Read More →

The Sharpest Ultraviolet view of the star formation in an extreme environment of the nearest Jellyfish Galaxy IC 3418. (arXiv:2104.14325v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hota_A/0/1/0/all/0/1">Ananda Hota</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Devaraj_A/0/1/0/all/0/1">Ashish Devaraj</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Pradhan_A/0/1/0/all/0/1">Ananta C. Pradhan</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Stalin_C/0/1/0/all/0/1">C S Stalin</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+George_K/0/1/0/all/0/1">Koshy George</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Mohapatra_A/0/1/0/all/0/1">Abhisek Mohapatra</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Rey_S/0/1/0/all/0/1">Soo-Chang Rey</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Ohyama_Y/0/1/0/all/0/1">Youichi Ohyama</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Vaddi_S/0/1/0/all/0/1">Sravani Vaddi</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Pechetti_R/0/1/0/all/0/1">Renuka Pechetti</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Sethuram_R/0/1/0/all/0/1">Ramya Sethuram</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Jose_J/0/1/0/all/0/1">Jessy Jose</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_J/0/1/0/all/0/1">Jayashree Roy</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Konar_C/0/1/0/all/0/1">Chiranjib Konar</a> (11) ((1) UM-DAE Centre for Excellence in Basic Sciences, University of Mumbai, India (2) Indian Institute of Astrophysics, India (3) National Institute of Technology, Rourkela, India (4)Read More →

Searching For Gravitational Waves From Cosmological Phase Transitions With The NANOGrav 12.5-year dataset. (arXiv:2104.13930v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Arzoumanian_Z/0/1/0/all/0/1">Zaven Arzoumanian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baker_P/0/1/0/all/0/1">Paul T. Baker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blumer_H/0/1/0/all/0/1">Harsha Blumer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becsy_B/0/1/0/all/0/1">Bence B&#xe9;csy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brazier_A/0/1/0/all/0/1">Adam Brazier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brook_P/0/1/0/all/0/1">Paul R. Brook</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_Spolaor_S/0/1/0/all/0/1">Sarah Burke-Spolaor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charisi_M/0/1/0/all/0/1">Maria Charisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Shami Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">Siyuan Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cordes_J/0/1/0/all/0/1">James M. Cordes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cornish_N/0/1/0/all/0/1">Neil J. Cornish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crawford_F/0/1/0/all/0/1">Fronefield Crawford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cromartie_H/0/1/0/all/0/1">H. Thankful Cromartie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeCesar_M/0/1/0/all/0/1">Megan E. DeCesar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demorest_P/0/1/0/all/0/1">Paul B. Demorest</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolch_T/0/1/0/all/0/1">Timothy Dolch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ellis_J/0/1/0/all/0/1">Justin A. Ellis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrara_E/0/1/0/all/0/1">Elizabeth C. Ferrara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fiore_W/0/1/0/all/0/1">William Fiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fonseca_E/0/1/0/all/0/1">Emmanuel Fonseca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garver_Daniels_N/0/1/0/all/0/1">Nathan Garver-Daniels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gentile_P/0/1/0/all/0/1">Peter A. Gentile</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Good_D/0/1/0/all/0/1">Deborah C. Good</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hazboun_J/0/1/0/all/0/1">Jeffrey S. Hazboun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holgado_A/0/1/0/all/0/1">A. MiguelRead More →

The Challenge to MOND from ultra faint dwarf galaxies. (arXiv:2104.13961v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Safarzadeh_M/0/1/0/all/0/1">Mohammadtaher Safarzadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> Modified Newtonian Dynamics (MOND) at low acceleration has been astonishingly powerful at explaining the flat rotation curve of galaxies and the relation between the baryonic content of the galaxies and their observed circular velocity, known as the Baryonic Tully-Fisher Relationship (BTFR). It is known that MOND fails at explaining the observed velocity dispersion of the ultra-faint dwarf galaxies (UFDs) with the justification that UFDs are more prone to tidal disruption in MOND compared to cold dark matter model. We show that: (i) the ratio of tidal to internalRead More →

Testing $f(Q, T)$ gravity models that reduce to $Lambda CDM$. (arXiv:2104.14065v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Najera_A/0/1/0/all/0/1">Antonio N&#xe1;jera</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Fajardo_A/0/1/0/all/0/1">Amanda Fajardo</a> We tested four $f(Q,T)$ models in an extension of symmetric teleparallel gravity whose Friedmann equations reduce to $Lambda CDM$ for certain parameters. Using low-redshift data we found that all our models were 2$sigma$ consistent with $Lambda CDM$ and the Hubble constant value were $sigma$ consistent with the one of the SH0ES collaboration and at $12sigma$ tension with the one of the Planck Collaboration. To see whether one of our models can challenge $Lambda CDM$ at a background perspective, we computed the Bayesian evidence for our four modelsRead More →

Collision Probabilities in the Edgeworth-Kuiper belt. (arXiv:2104.14039v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Abedin_A/0/1/0/all/0/1">Abedin Y. Abedin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kavelaars_J/0/1/0/all/0/1">JJ Kavelaars</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greenstreet_S/0/1/0/all/0/1">Sarah Greenstreet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petit_J/0/1/0/all/0/1">Jean-Marc Petit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladman_B/0/1/0/all/0/1">Brett Gladman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lawler_S/0/1/0/all/0/1">Samantha Lawler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bannister_M/0/1/0/all/0/1">Michele Bannister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alexandersen_M/0/1/0/all/0/1">Mike Alexandersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Ying-Tung Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gwyn_S/0/1/0/all/0/1">Stephen Gwyn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Volk_K/0/1/0/all/0/1">Kathryn Volk</a> Here, we present results on the intrinsic collision probabilities, $ P_I$, and range of collision speeds, $V_I$, as a function of the heliocentric distance, $r$, in the trans-Neptunian region. The collision speed is one of the parameters, that serves as a proxy to a collisional outcome e.g., complete disruption and scattering of fragments, or formation of crater, where both processes are directly relatedRead More →

How Sublimation Delays the Onset of Dusty Debris Disk Formation Around White Dwarf Stars. (arXiv:2104.14035v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Steckloff_J/0/1/0/all/0/1">Jordan K. Steckloff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debes_J/0/1/0/all/0/1">John Debes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steele_A/0/1/0/all/0/1">Amy Steele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_B/0/1/0/all/0/1">Brandon Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_E/0/1/0/all/0/1">Elisabeth R. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jacobson_S/0/1/0/all/0/1">Seth A. Jacobson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Springmann_A/0/1/0/all/0/1">Alessondra Springmann</a> Although numerous white dwarf stars host dusty debris disks, the temperature distribution of these stars differs significantly from the white dwarf population as a whole. Dusty debris disks exist exclusively around white dwarfs cooler than 27,000 K. This is all the more enigmatic given that the formation processes of dusty debris disks should favor younger, hotter white dwarfs, which likely host more dynamically unstable planetaryRead More →