RAS_WEB (Page 2,255)

Velocity-dependent J-factors for annihilation radiation from cosmological simulations. (arXiv:2101.06284v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Board_E/0/1/0/all/0/1">Erin Board</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozorgnia_N/0/1/0/all/0/1">Nassim Bozorgnia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strigari_L/0/1/0/all/0/1">Louis E. Strigari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grand_R/0/1/0/all/0/1">Robert J. J. Grand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fattahi_A/0/1/0/all/0/1">Azadeh Fattahi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frenk_C/0/1/0/all/0/1">Carlos S. Frenk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marinacci_F/0/1/0/all/0/1">Federico Marinacci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Navarro_J/0/1/0/all/0/1">Julio F. Navarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oman_K/0/1/0/all/0/1">Kyle A. Oman</a> We determine the dark matter pair-wise relative velocity distribution in a set of Milky Way-like halos in the Auriga and APOSTLE simulations. Focusing on the smooth halo component, the relative velocity distribution is well-described by a Maxwell-Boltzmann distribution over nearly all radii in the halo. We explore the implications for velocity-dependent dark matter annihilation, focusing on four models which scale asRead More →

The Tully-Fisher relation in dense groups at $z sim 0.7$ in the MAGIC survey. (arXiv:2101.08069v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Abril_Melgarejo_V/0/1/0/all/0/1">Valentina Abril-Melgarejo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Epinat_B/0/1/0/all/0/1">Beno&#xee;t Epinat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mercier_W/0/1/0/all/0/1">Wilfried Mercier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contini_T/0/1/0/all/0/1">Thierry Contini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boogaard_L/0/1/0/all/0/1">Leindert A. Boogaard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brinchmann_J/0/1/0/all/0/1">Jarle Brinchmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finley_H/0/1/0/all/0/1">Hayley Finley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michel_Dansac_L/0/1/0/all/0/1">L&#xe9;o Michel-Dansac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ventou_E/0/1/0/all/0/1">Emmy Ventou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amram_P/0/1/0/all/0/1">Philipe Amram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krajnovic_D/0/1/0/all/0/1">Davor Krajnovi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahler_G/0/1/0/all/0/1">Guillaume Mahler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">Juan C. B. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richard_J/0/1/0/all/0/1">Johan Richard</a> Galaxies in dense environments are subject to interactions and mechanisms which directly affect their evolution by lowering their gas fractions and reducing their star-forming capacity earlier than their isolated counterparts. The aim of our project is to get new insights about the roleRead More →

The Role of Strong Gravity and the Nuclear Equation of State on Neutron-Star Common-Envelope Accretion. (arXiv:2101.08267v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Holgado_A/0/1/0/all/0/1">A. Miguel Holgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silva_H/0/1/0/all/0/1">Hector O. Silva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_P/0/1/0/all/0/1">Paul M. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yunes_N/0/1/0/all/0/1">Nicolas Yunes</a> Common-envelope evolution is important in the formation of neutron star binaries within the isolated binary formation channel. As a neutron star inspirals within the envelope of a primary massive star, it accretes and spins up. Because neutron stars are in the strong-gravity regime, they have a substantial relativistic mass deficit, i.e., their gravitational mass is less than their baryonic mass. This effect causes some fraction of the accreted baryonic mass to convertRead More →

Processing of Global Solar Irradiance and Ground-Based Infrared Sky Images for Very Short-Term Solar Forecasting. (arXiv:2101.08694v3 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Terren_Serrano_G/0/1/0/all/0/1">Guillermo Terr&#xe9;n-Serrano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Ramon_M/0/1/0/all/0/1">Manel Mart&#xed;nez-Ram&#xf3;n</a> The projection of shadows from moving clouds in the troposphere impacts energy generation in power grids using Photovoltaic (PV) systems. This investigation proposes an efficient method of data processing for the statistical quantification of cloud features using long-wave Infrared (IR) images and Global Solar Irradiance (GSI) measurements. The infrared images are obtained using a Data Acquisition System (DAQ) mounted on a solar tracker. We explain how to remove cyclostationary biases in global solar irradiance measurements. Seasonal trends are removed from theRead More →

Dynamics of Laterally Propagating Flames in X-ray Bursts. II. Realistic Burning & Rotation. (arXiv:2102.00051v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Harpole_A/0/1/0/all/0/1">A. Harpole</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ford_N/0/1/0/all/0/1">N. M. Ford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eiden_K/0/1/0/all/0/1">K. Eiden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zingale_M/0/1/0/all/0/1">M. Zingale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Willcox_D/0/1/0/all/0/1">D. E. Willcox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cavecchi_Y/0/1/0/all/0/1">Y. Cavecchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_M/0/1/0/all/0/1">M. P. Katz</a> We continue to investigate two-dimensional laterally propagating flames in type I X-ray bursts using fully compressible hydrodynamics simulations. In the current study we relax previous approximations where we artificially boosted the flames. We now use more physically realistic reaction rates, thermal conductivities, and rotation rates, exploring the effects of neutron star rotation rate and thermal structure on the flame. We find that at lower rotationRead More →

A super-Earth on a close-in orbit around the M1V star GJ 740. A HADES and CARMENES collaboration. (arXiv:2102.09441v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Toledo_Padron_B/0/1/0/all/0/1">B. Toledo-Padr&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mascareno_A/0/1/0/all/0/1">A. Su&#xe1;rez Mascare&#xf1;o</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_J/0/1/0/all/0/1">J. I. Gonz&#xe1;lez Hern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rebolo_R/0/1/0/all/0/1">R. Rebolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinamonti_M/0/1/0/all/0/1">M. Pinamonti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perger_M/0/1/0/all/0/1">M. Perger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scandariato_G/0/1/0/all/0/1">G. Scandariato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Damasso_M/0/1/0/all/0/1">M. Damasso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sozzetti_A/0/1/0/all/0/1">A. Sozzetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maldonado_J/0/1/0/all/0/1">J. Maldonado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desidera_S/0/1/0/all/0/1">S. Desidera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ribas_I/0/1/0/all/0/1">I. Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Micela_G/0/1/0/all/0/1">G. Micela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Affer_L/0/1/0/all/0/1">L. Affer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Alvarez_E/0/1/0/all/0/1">E. Gonz&#xe1;lez-Alvarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leto_G/0/1/0/all/0/1">G. Leto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pagano_I/0/1/0/all/0/1">I. Pagano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_R/0/1/0/all/0/1">R. Zanmar S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giacobbe_P/0/1/0/all/0/1">P. Giacobbe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herrero_E/0/1/0/all/0/1">E. Herrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_J/0/1/0/all/0/1">J. C. Morales</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:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quirrenbach_A/0/1/0/all/0/1">A. Quirrenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiners_A/0/1/0/all/0/1">A. Reiners</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zechmeister_M/0/1/0/all/0/1">M. Zechmeister</a>Read More →

Inflation and Scale-invariant $R^2$-Gravity. (arXiv:2102.11719v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Bruck_C/0/1/0/all/0/1">Carsten van de Bruck</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Daniel_R/0/1/0/all/0/1">Richard Daniel</a> In scale-invariant models of fundamental physics, mass scales are generated by spontaneous symmetry breaking. In this work, we study inflation in scale-invariant $R^2$ gravity, in which the Planck mass is generated by a scalar field, which is responsible for spontaneous breaking of scale–symmetry. If the self-interactions of the scalar field are non-zero, a cosmological constant is generated, which can be potentially quite large. To avoid fine-tuning at late times, we introduce another scalar field which drives the classical cosmological constant to zero during inflation. Working in the Einstein-frame, we findRead More →

In the Realm of the Hubble tension $-$ a Review of Solutions. (arXiv:2103.01183v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_E/0/1/0/all/0/1">Eleonora Di Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mena_O/0/1/0/all/0/1">Olga Mena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_S/0/1/0/all/0/1">Supriya Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Visinelli_L/0/1/0/all/0/1">Luca Visinelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_W/0/1/0/all/0/1">Weiqiang Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melchiorri_A/0/1/0/all/0/1">Alessandro Melchiorri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mota_D/0/1/0/all/0/1">David F. Mota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riess_A/0/1/0/all/0/1">Adam G. Riess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silk_J/0/1/0/all/0/1">Joseph Silk</a> The $Lambda$CDM model provides a good fit to a large span of cosmological data but harbors areas of phenomenology. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the $4-6sigma$ disagreement between predictions of the Hubble constant $H_0$ by early time probesRead More →

Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-Cool Dwarfs. (arXiv:2103.01990v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tannock_M/0/1/0/all/0/1">Megan E. Tannock</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Metchev_S/0/1/0/all/0/1">Stanimir Metchev</a> (2 and 3), <a href="http://arxiv.org/find/astro-ph/1/au:+Heinze_A/0/1/0/all/0/1">Aren Heinze</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Miles_Paez_P/0/1/0/all/0/1">Paulo A. Miles-P&#xe1;ez</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Gagne_J/0/1/0/all/0/1">Jonathan Gagn&#xe9;</a> (6 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Burgasser_A/0/1/0/all/0/1">Adam Burgasser</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Marley_M/0/1/0/all/0/1">Mark S. Marley</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Apai_D/0/1/0/all/0/1">D&#xe1;niel Apai</a> (10 and 11), <a href="http://arxiv.org/find/astro-ph/1/au:+Suarez_G/0/1/0/all/0/1">Genaro Su&#xe1;rez</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Plavchan_P/0/1/0/all/0/1">Peter Plavchan</a> (12) ((1) University of Western Ontario, (2) Institute for Earth and Space Exploration, The University of Western Ontario, (3) American Museum of Natural History, (4) Institute for Astronomy, University of Hawaii, (5) European Southern Observatory, (6) Plan&#xe9;tarium Rio Tinto Alcan, Espace pourRead More →