RAS_WEB (Page 2,429)

Explosive nucleosynthesis of a metal-deficient star as the source of a distinct odd-even effect in the solar twin HIP 11915. (arXiv:2101.10182v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Galarza_J/0/1/0/all/0/1">Jhon Yana Galarza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melendez_J/0/1/0/all/0/1">Jorge Mel&#xe9;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karakas_A/0/1/0/all/0/1">Amanda I. Karakas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">Martin Asplund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Oliveira_D/0/1/0/all/0/1">Diego Lorenzo-Oliveira</a> The abundance patterns observed in the Sun and in metal-poor stars show a clear odd-even effect. An important question is whether the odd-even effect in solar-metallicity stars is similar to the Sun, or if there are variations that can tell us about different chemical enrichment histories. In this work, we report for the first time observational evidence of a differential odd-even effect in the solar twinRead More →

Scalar Multiplet Dark Matter in a Fast Expanding Universe: resurrection of the {it desert} region. (arXiv:2101.10175v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Barman_B/0/1/0/all/0/1">Basabendu Barman</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ghosh_P/0/1/0/all/0/1">Purusottam Ghosh</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Queiroz_F/0/1/0/all/0/1">Farinaldo S. Queiroz</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Saha_A/0/1/0/all/0/1">Abhijit Kumar Saha</a> We examine the impact of a faster expanding Universe on the phenomenology of scalar dark matter (DM) associated with $SU(2)_L$ multiplets. Earlier works with radiation dominated Universe have reported the presence of desert region for both inert $SU(2)_L$ doublet and triplet DM candidates where the DM is under abundant. We find that the existence of a faster expanding component before BBN can revive a major part of the desert parameter space consistent with relicRead More →

Comparison of classical and Bayesian imaging in radio interferometry. (arXiv:2008.11435v4 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Arras_P/0/1/0/all/0/1">Philipp Arras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bester_H/0/1/0/all/0/1">Hertzog L. Bester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perley_R/0/1/0/all/0/1">Richard A. Perley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leike_R/0/1/0/all/0/1">Reimar Leike</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smirnov_O/0/1/0/all/0/1">Oleg Smirnov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Westermann_R/0/1/0/all/0/1">R&#xfc;diger Westermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ensslin_T/0/1/0/all/0/1">Torsten A. En&#xdf;lin</a> CLEAN, the commonly employed imaging algorithm in radio interferometry, suffers from a number of shortcomings: in its basic version it does not have the concept of diffuse flux, and the common practice of convolving the CLEAN components with the CLEAN beam erases the potential for super-resolution; it does not output uncertainty information; it produces images with unphysical negative flux regions; and its results are highly dependent on the so-calledRead More →

Astrophysical hints for magnetic black holes. (arXiv:2009.03363v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Ghosh_D/0/1/0/all/0/1">Diptimoy Ghosh</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Thalapillil_A/0/1/0/all/0/1">Arun Thalapillil</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ullah_F/0/1/0/all/0/1">Farman Ullah</a> We discuss a cornucopia of potential astrophysical signatures and constraints on magnetically charged black holes of various masses. As recently highlighted, being potentially viable astrophysical candidates with immense electromagnetic fields, they may be ideal windows to fundamental physics, electroweak symmetry restoration and non-perturbative quantum field theoretic phenomena. We investigate various potential astrophysical pointers and bounds — including limits on charges, location of stable orbits and horizons in asymptotically flat and asymptotically de Sitter backgrounds, bounds from galactic magnetic fields and dark matter measurements, characteristic electromagnetic fluxes andRead More →

The Dark Matter Enigma. (arXiv:2101.10127v1 [physics.pop-ph]) <a href="http://arxiv.org/find/physics/1/au:+Luminet_J/0/1/0/all/0/1">Jean-Pierre Luminet</a> (Aix-Marseille Universit&#xe9;, CNRS, Laboratoire d&#x27;Astrophysique de Marseille, France) In this pedestrian approach I give my personal point of view on the various problems posed by dark matter in the universe. After a brief historical overview I discuss the various solutions stemming from high energy particle physics, and the current status of experimental research on candidate particles (WIMPS). In the absence of direct evidence, the theories can still be evaluated by comparing their implications for the formation of galaxies, clusters and superclusters of galaxies against astronomical observations. I conclude briefly with the attempts to circumvent the darkRead More →

Prospects for Measuring the Hubble Constant with Neutron-Star-Black-Hole Mergers. (arXiv:2012.06593v2 [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 →

The VMC survey — XLI. Stellar proper motions within the Small Magellanic Cloud. (arXiv:2101.09099v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Niederhofer_F/0/1/0/all/0/1">F. Niederhofer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cioni_M/0/1/0/all/0/1">M.-R. L. Cioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubele_S/0/1/0/all/0/1">S. Rubele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmidt_T/0/1/0/all/0/1">T. Schmidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_J/0/1/0/all/0/1">J. D. Diaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matijevic_G/0/1/0/all/0/1">G. Matijevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bekki_K/0/1/0/all/0/1">K. Bekki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bell_C/0/1/0/all/0/1">C. P. M. Bell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grijs_R/0/1/0/all/0/1">R. de Grijs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Youssoufi_D/0/1/0/all/0/1">D. El Youssoufi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivanov_V/0/1/0/all/0/1">V. D. Ivanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliveira_J/0/1/0/all/0/1">J. M. Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ripepi_V/0/1/0/all/0/1">V. Ripepi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subramanian_S/0/1/0/all/0/1">S. Subramanian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_N/0/1/0/all/0/1">N.-C. Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loon_J/0/1/0/all/0/1">J. Th. van Loon</a> We used data from the near-infrared VISTA survey of the Magellanic Cloud system (VMC) to measure proper motions (PMs) of stars within the Small Magellanic Cloud (SMC). The data analysed inRead More →

Blind Map Level Systematics Cleaning: A Quadratic Estimator Approach. (arXiv:2101.09097v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_J/0/1/0/all/0/1">Joel Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCallum_N/0/1/0/all/0/1">Nialh McCallum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rotti_A/0/1/0/all/0/1">Aditya Rotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_D/0/1/0/all/0/1">Daniel Thomas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battye_R/0/1/0/all/0/1">Richard Battye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_M/0/1/0/all/0/1">Michael L. Brown</a> We present the first detailed case study using quadratic estimators (QE) to diagnose and remove systematics present in observed Cosmic Microwave Background (CMB) maps. In this work we focus on the temperature to polarization leakage. We use an iterative QE analysis to remove systematics, in analogy to de-lensing, recovering the primordial B-mode signal and the systematic maps. We introduce a new Gaussian filtering scheme crucial to stable convergence of the iterative cleaning procedure andRead More →

Separating $^{39}$Ar from $^{40}$Ar by cryogenic distillation with Aria for dark matter searches. (arXiv:2101.08686v2 [physics.ins-det] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Collaboration_DarkSide/0/1/0/all/0/1">DarkSide Collaboration</a>: <a href="http://arxiv.org/find/physics/1/au:+Agnes_P/0/1/0/all/0/1">P. Agnes</a>, <a href="http://arxiv.org/find/physics/1/au:+Albergo_S/0/1/0/all/0/1">S. Albergo</a>, <a href="http://arxiv.org/find/physics/1/au:+Albuquerque_I/0/1/0/all/0/1">I. F. M. Albuquerque</a>, <a href="http://arxiv.org/find/physics/1/au:+Alexander_T/0/1/0/all/0/1">T. Alexander</a>, <a href="http://arxiv.org/find/physics/1/au:+Alici_A/0/1/0/all/0/1">A. Alici</a>, <a href="http://arxiv.org/find/physics/1/au:+Alton_A/0/1/0/all/0/1">A. K. Alton</a>, <a href="http://arxiv.org/find/physics/1/au:+Amaudruz_P/0/1/0/all/0/1">P. Amaudruz</a>, <a href="http://arxiv.org/find/physics/1/au:+Arba_M/0/1/0/all/0/1">M. Arba</a>, <a href="http://arxiv.org/find/physics/1/au:+Arpaia_P/0/1/0/all/0/1">P. Arpaia</a>, <a href="http://arxiv.org/find/physics/1/au:+Arcelli_S/0/1/0/all/0/1">S. Arcelli</a>, <a href="http://arxiv.org/find/physics/1/au:+Ave_M/0/1/0/all/0/1">M. Ave</a>, <a href="http://arxiv.org/find/physics/1/au:+Avetissov_I/0/1/0/all/0/1">I. Ch. Avetissov</a>, <a href="http://arxiv.org/find/physics/1/au:+Avetisov_R/0/1/0/all/0/1">R. I. Avetisov</a>, <a href="http://arxiv.org/find/physics/1/au:+Azzolini_O/0/1/0/all/0/1">O. Azzolini</a>, <a href="http://arxiv.org/find/physics/1/au:+Back_H/0/1/0/all/0/1">H. O. Back</a>, <a href="http://arxiv.org/find/physics/1/au:+Balmforth_Z/0/1/0/all/0/1">Z. Balmforth</a>, <a href="http://arxiv.org/find/physics/1/au:+Barbarian_V/0/1/0/all/0/1">V. Barbarian</a>, <a href="http://arxiv.org/find/physics/1/au:+Olmedo_A/0/1/0/all/0/1">A. Barrado Olmedo</a>, <a href="http://arxiv.org/find/physics/1/au:+Barrillon_P/0/1/0/all/0/1">P. Barrillon</a>, <a href="http://arxiv.org/find/physics/1/au:+Basco_A/0/1/0/all/0/1">A. Basco</a>, <a href="http://arxiv.org/find/physics/1/au:+Batignani_G/0/1/0/all/0/1">G. Batignani</a>, <a href="http://arxiv.org/find/physics/1/au:+Bondar_A/0/1/0/all/0/1">A. Bondar</a>, <a href="http://arxiv.org/find/physics/1/au:+Bonivento_W/0/1/0/all/0/1">W. M. Bonivento</a>, <a href="http://arxiv.org/find/physics/1/au:+Borisova_E/0/1/0/all/0/1">E. Borisova</a>, <a href="http://arxiv.org/find/physics/1/au:+Bottino_B/0/1/0/all/0/1">B. Bottino</a>, <a href="http://arxiv.org/find/physics/1/au:+Boulay_M/0/1/0/all/0/1">M. G.Read More →

The Cosmological Constant as a Zero Action Boundary. (arXiv:2101.07368v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Gaztanaga_E/0/1/0/all/0/1">Enrique Gaztanaga</a> The cosmological constant $Lambda$ is usually interpreted as Dark Energy (DE) or modified gravity (MG). Here we propose instead that $Lambda$ corresponds to a boundary term in the action of classical General Relativity. The action is zero for a perfect fluid solution and this fixes $Lambda$ to the average density $rho$ and pressure $p$ inside a primordial causal boundary: $Lambda = 4pi G <rho+3p>$. This explains both why the observed value of $Lambda$ is related to the matter density today and also why other contributions to $Lambda$, such as DE orRead More →

Flux variability from ejectas in structured relativistic jets with large-scale magnetic fields. (arXiv:2101.06962v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Clairfontaine_G/0/1/0/all/0/1">Ga&#xeb;tan Fichet de Clairfontaine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meliani_Z/0/1/0/all/0/1">Zakaria Meliani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zech_A/0/1/0/all/0/1">Andreas Zech</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hervet_O/0/1/0/all/0/1">Olivier Hervet</a> Using the relativistic MHD code MPI-AMRVAC and a radiative transfer code in post-processing, we explore the influence of the magnetic-field configuration and transverse stratification of an over-pressured jet on its morphology, on the moving shock dynamics, and on the emitted radio light curve. First, we investigate different large-scale magnetic fields with their effects on the standing shocks and on the stratified jet morphology. Secondly, we study the interaction of a moving shock wave with the standingRead More →

Low thermal conductivity of the superfast rotator (499998) 2011 PT. (arXiv:2101.04399v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fenucci_M/0/1/0/all/0/1">Marco Fenucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novakovic_B/0/1/0/all/0/1">Bojan Novakovi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vokrouhlicky_D/0/1/0/all/0/1">David Vokrouhlick&#xfd;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weryk_R/0/1/0/all/0/1">Robert J. Weryk</a> Context: Asteroids with a diameter of up to a few dozen meters may spin very fast and complete an entire rotation within a few minutes. These small and fast-rotating bodies are thought to be monolithic objects because the gravitational force due to their small size is not strong enough to counteract the strong centripetal force caused by the fast rotation. Additionally, it is not clear whether the fast spin prevents dust and small particles (regolith) from being kept onRead More →

A population of heavily reddened, optically missed novae from Palomar Gattini-IR: Constraints on the Galactic nova rate. (arXiv:2101.04045v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+De_K/0/1/0/all/0/1">Kishalay De</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasliwal_M/0/1/0/all/0/1">Mansi M. Kasliwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hankins_M/0/1/0/all/0/1">Matthew J. Hankins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokoloski_J/0/1/0/all/0/1">Jennifer L. Sokoloski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_S/0/1/0/all/0/1">Scott M. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashley_M/0/1/0/all/0/1">Michael C. B. Ashley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babul_A/0/1/0/all/0/1">Aliya-Nur Babul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bagdasaryan_A/0/1/0/all/0/1">Ashot Bagdasaryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delacroix_A/0/1/0/all/0/1">Alexandre Delacroix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dekany_R/0/1/0/all/0/1">Richard Dekany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greffe_T/0/1/0/all/0/1">Timothee Greffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hale_D/0/1/0/all/0/1">David Hale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jencson_J/0/1/0/all/0/1">Jacob E. Jencson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karambelkar_V/0/1/0/all/0/1">Viraj R. Karambelkar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lau_R/0/1/0/all/0/1">Ryan M. Lau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahabal_A/0/1/0/all/0/1">Ashish Mahabal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKenna_D/0/1/0/all/0/1">Daniel McKenna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moore_A/0/1/0/all/0/1">Anna M. Moore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ofek_E/0/1/0/all/0/1">Eran O. Ofek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_M/0/1/0/all/0/1">Manasi Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Roger M. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soon_J/0/1/0/all/0/1">Jamie Soon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soria_R/0/1/0/all/0/1">Roberto Soria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srinivasaragavan_G/0/1/0/all/0/1">Gokul Srinivasaragavan</a>, <aRead More →

High Spatial and Spectral Resolution Observations of the Forbidden 1.707 micron Rovibronic SO Emissions on Io: Evidence for Widespread Stealth Volcanism. (arXiv:2101.01789v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pater_I/0/1/0/all/0/1">Imke de Pater</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleer_K/0/1/0/all/0/1">Katherine de Kleer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adamkovics_M/0/1/0/all/0/1">Mate Adamkovics</a> We present observations obtained with the 10-m Keck telescopes of the forbidden SO rovibronic transition at 1.707 micron on Io while in eclipse. We show its spatial distribution at a resolution of ~0.12″ and a spectral resolution of R ~2500, as well as disk-integrated spectra at a high spectral resolution (R~15,000). Both the spatial distribution and the spectral shape of the SO emission band vary considerably across Io and overRead More →

Polytropic spheres modelling dark matter halos of dwarf galaxies. (arXiv:2101.00891v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Novotny_J/0/1/0/all/0/1">Jan Novotn&#xfd;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stuchlik_Z/0/1/0/all/0/1">Zden&#x11b;k Stuchl&#xed;k</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hladik_J/0/1/0/all/0/1">Jan Hlad&#xed;k</a> Dwarf galaxies and their dark matter (DM) halos have the velocity curves of a different character than those in large galaxies. They are modelled by a simple pseudo iso-thermal model containing only two parameters that do not allow to obtain insight into physics of the DM halo. We would like to obtain some insight into the physical conditions in DM halos of dwarf galaxies by using a simple physically based model of DM halos. In order to treat a diversity of the dwarf galaxyRead More →

Properties of Compact Faint Radio Sources as a Function of Angular Size from Stacking. (arXiv:2101.00680v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_R/0/1/0/all/0/1">Ryan S. Johnston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stil_J/0/1/0/all/0/1">Jeroen M. Stil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keller_B/0/1/0/all/0/1">Ben W. Keller</a> The polarization properties of radio sources powered by an Active Galactic Nucleus (AGN) have attracted considerable attention because of the significance of magnetic fields in the physics of these sources, their use as probes of plasma along the line of sight, and as a possible contaminant of polarization measurements of the cosmic microwave background. For each of these applications, a better understanding of the statistics of polarization in relation to source characteristics is crucial. In thisRead More →

Three-dimensional Hydrodynamics Simulations of Precollapse Shell Burning in the Si- and O-rich Layers. (arXiv:2012.13261v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_T/0/1/0/all/0/1">Takashi Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takiwaki_T/0/1/0/all/0/1">Tomoya Takiwaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kotake_K/0/1/0/all/0/1">Kei Kotake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_K/0/1/0/all/0/1">Koh Takahashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamura_K/0/1/0/all/0/1">Ko Nakamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umeda_H/0/1/0/all/0/1">Hideyuki Umeda</a> We present 3D hydrodynamics simulations of shell burning in two progenitors with zero-age main-sequence masses of 22 and 27 $M_{odot}$ for $sim$65 and 200 s up to the onset of gravitational collapse, respectively. The 22 and 27 $M_{odot}$ stars are selected from a suite of 1D progenitors. The former and the latter have an extended Si- and O-rich layer with a width of $sim$10$^9$ cm and $sim$5$times 10^9$ cm, respectively. OurRead More →

Review on Dark Matter Tools. (arXiv:2012.09462v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Arina_C/0/1/0/all/0/1">Chiara Arina</a> Whilst the need for dark matter was established almost a century ago, only its gravitational interaction has been confirmed so far, allowing for plethora of models for dark matter. The Weakly Interacting Massive Particles (WIMPs) category has received by far the biggest attention, however despite the enormous experimental efforts, these particles remain elusive. The attention of the community has hence moved on to investigate the dark matter landscape over a much larger number of models with varying degrees of resemblances and differences in their predictions. This calls for the need to organise the variousRead More →

Energetic Proton Propagation and Acceleration Simulated for the Bastille Day Event of July 14, 2000. (arXiv:2012.09078v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Young_M/0/1/0/all/0/1">Matthew A. Young</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwadron_N/0/1/0/all/0/1">Nathan A. Schwadron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gorby_M/0/1/0/all/0/1">Matthew Gorby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Linker_J/0/1/0/all/0/1">Jon Linker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caplan_R/0/1/0/all/0/1">Ronald M. Caplan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Downs_C/0/1/0/all/0/1">Cooper Downs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torok_T/0/1/0/all/0/1">Tibor T&#xf6;r&#xf6;k</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riley_P/0/1/0/all/0/1">Pete Riley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lionello_R/0/1/0/all/0/1">Roberto Lionello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Titov_V/0/1/0/all/0/1">Viacheslav Titov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mewaldt_R/0/1/0/all/0/1">Richard A. Mewaldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cohen_C/0/1/0/all/0/1">Christina M. S. Cohen</a> This work presents results from simulations of the 14 July 2000 (“Bastille Day”) solar proton event. We used the Energetic Particle Radiation Environment Model (EPREM) and the CORona-HELiosphere (CORHEL) software suite within the SPE Threat Assessment Tool (STAT) framework to model proton acceleration to GeVRead More →

A giant central red disk galaxy at redshift $z=0.76$: challenge to theories of galaxy formation. (arXiv:2012.08798v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_K/0/1/0/all/0/1">Kun Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">Chengze Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jing_Y/0/1/0/all/0/1">Yipeng Jing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sawicki_M/0/1/0/all/0/1">Marcin Sawicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gwyn_S/0/1/0/all/0/1">Stephen Gwyn</a> We report a giant red central disk galaxy in the XMM-LSS north region. The region is covered with a rich variety of multiband photometric and spectroscopic observations. Using the photometric data of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) and spectroscopic observation of the Baryon Oscillation Spectroscopic Survey (BOSS), we find that the galaxy has a stellar mass of $sim 10^{11.6}$ times of the solar mass $M_odot$. The galaxy has a red colorRead More →