RAS_WEB (Page 4,431)

Predictions for the Abundance of High-redshift Galaxies in a Fuzzy Dark Matter Universe. (arXiv:1904.01604v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ni_Y/0/1/0/all/0/1">Yueying Ni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_M/0/1/0/all/0/1">Mei-Yu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feng_Y/0/1/0/all/0/1">Yu Feng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteo_T/0/1/0/all/0/1">Tiziana Di Matteo</a> During the last decades, rapid progress has been made in measurements of the rest-frame ultraviolet (UV) luminosity function (LF) for high-redshift galaxies ($z geq 6$). The faint-end of the galaxy LF at these redshifts provides powerful constraints on different dark matter models that suppress small-scale structure formation. In this work we perform full hydrodynamical cosmological simulations of galaxy formation using an alternative DM model composed of extremely light bosonic particles ($m sim 10^{-22}$ eV), also known asRead More →

Extremely metal-poor galaxies with HST/COS: laboratories for models of low-metallicity massive stars and high-redshift galaxies. (arXiv:1904.01615v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Senchyna_P/0/1/0/all/0/1">Peter Senchyna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stark_D/0/1/0/all/0/1">Daniel P. Stark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chevallard_J/0/1/0/all/0/1">Jacopo Chevallard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charlot_S/0/1/0/all/0/1">St&#xe9;phane Charlot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_T/0/1/0/all/0/1">Tucker Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_A/0/1/0/all/0/1">Alba Vidal Garc&#xed;a</a> Ultraviolet (UV) observations of local star-forming galaxies have begun to establish an empirical baseline for interpreting the rest-UV spectra of reionization-era galaxies. However, existing high-ionization emission line measurements at $z>6$ ($mathrm{W_{C IV, 0}} gtrsim 20$ {AA}) are uniformly stronger than observed locally ($mathrm{W_{C IV, 0}} lesssim 2$ {AA}), likely due to the relatively high metallicities ($Z/Z_odot > 0.1$) typically probed by UV surveys of nearby galaxies. We presentRead More →

Dark-ages Reionization and Galaxy Formation Simulation – XVII. Sizes, angular momenta and morphologies of high redshift galaxies. (arXiv:1904.01619v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_M/0/1/0/all/0/1">Madeline A. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mutch_S/0/1/0/all/0/1">Simon J. Mutch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qin_Y/0/1/0/all/0/1">Yuxiang Qin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poole_G/0/1/0/all/0/1">Gregory B. Poole</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyithe_J/0/1/0/all/0/1">J. Stuart B. Wyithe</a> We study the sizes, angular momenta and morphologies of high-redshift galaxies using an update of the Meraxes semi-analytic galaxy evolution model. Our model successfully reproduces a range of observations from redshifts $z=0$-$10$. We find that the effective radius of a galaxy disc scales with UV luminosity as $R_epropto L_{textrm{UV}}^{0.33}$ at $z=5$-$10$, and with stellar mass as $R_epropto M_ast^{0.24}$ at $z=5$ but with a slope that increasesRead More →

White dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 14. (arXiv:1904.01626v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kepler_S/0/1/0/all/0/1">S. O. Kepler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pelisoli_I/0/1/0/all/0/1">Ingrid Pelisoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koester_D/0/1/0/all/0/1">Detlev Koester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reindl_N/0/1/0/all/0/1">Nicole Reindl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geier_S/0/1/0/all/0/1">Stephan Geier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_A/0/1/0/all/0/1">Alejandra D. Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ourique_G/0/1/0/all/0/1">Gustavo Ourique</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliveira_C/0/1/0/all/0/1">Cristiane de Paula Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaral_L/0/1/0/all/0/1">Larissa A. Amaral</a> White dwarfs carry information on the structure and evolution of the Galaxy, especially through their luminosity function and initial-to-final mass relation. Very cool white dwarfs provide insight into the early ages of each population. Examining the spectra of all stars with $3sigma$ proper motion in the Sloan Digital Sky Survey Data Release 14, we report the classificationRead More →

Stringent limits on the magnetic field strength in the disc of TW Hya: ALMA observations of CN polarisation. (arXiv:1904.01632v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vlemmings_W/0/1/0/all/0/1">W.H.T. Vlemmings</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lankhaar_B/0/1/0/all/0/1">B. Lankhaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cazzoletti_P/0/1/0/all/0/1">P. Cazzoletti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ceccobello_C/0/1/0/all/0/1">C. Ceccobello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DallOlio_D/0/1/0/all/0/1">D. Dall&#x27;Olio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dishoeck_E/0/1/0/all/0/1">E.F. van Dishoeck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Facchini_S/0/1/0/all/0/1">S. Facchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Humphreys_E/0/1/0/all/0/1">E.M.L. Humphreys</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Persson_M/0/1/0/all/0/1">M.V. Persson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testi_L/0/1/0/all/0/1">L. Testi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_J/0/1/0/all/0/1">J.P. Williams</a> Despite their importance in the star formation process, measurements of magnetic field strength in proto-planetary discs remain rare. While linear polarisation of dust and molecular lines can give insight into the magnetic field structure, only observations of the circular polarisation produced by Zeeman splitting provide a direct measurement of magnetic fieldRead More →

A Physical Basis for the H-band Blue-edge Velocity and Light-Curve Shape Correlation in Context of Type Ia Supernova Explosion Physics. (arXiv:1904.01633v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ashall_C/0/1/0/all/0/1">C. Ashall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoeflich_P/0/1/0/all/0/1">P. Hoeflich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsiao_E/0/1/0/all/0/1">E. Y. Hsiao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillips_M/0/1/0/all/0/1">M. M. Phillips</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stritzinger_M/0/1/0/all/0/1">M. Stritzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baron_E/0/1/0/all/0/1">E. Baron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_A/0/1/0/all/0/1">A. L. Piro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burns_C/0/1/0/all/0/1">C. Burns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_C/0/1/0/all/0/1">C. Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_S/0/1/0/all/0/1">S. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holmbo_S/0/1/0/all/0/1">S. Holmbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirshner_R/0/1/0/all/0/1">R. P. Kirshner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krisciunas_K/0/1/0/all/0/1">K. Krisciunas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marion_G/0/1/0/all/0/1">G. H. Marion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morrell_N/0/1/0/all/0/1">N. Morrell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sand_D/0/1/0/all/0/1">D. J. Sand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shahbandeh_M/0/1/0/all/0/1">M. Shahbandeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suntzeff_N/0/1/0/all/0/1">N. B. Suntzeff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taddia_F/0/1/0/all/0/1">F. Taddia</a> Our recent work demonstrates a correlation between the high-velocity blue edge, $v_{edge}$, of the iron-peak Fe/Co/NiRead More →

BICEP2 / Keck Array XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Dataset. (arXiv:1904.01640v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Array_K/0/1/0/all/0/1">Keck Array</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_BICEP2/0/1/0/all/0/1">BICEP2 Collaborations</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">P. A. R. Ade</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ahmed_Z/0/1/0/all/0/1">Z. Ahmed</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Aikin_R/0/1/0/all/0/1">R. W. Aikin</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Barkats_D/0/1/0/all/0/1">D. Barkats</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Benton_S/0/1/0/all/0/1">S. J. Benton</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Bischoff_C/0/1/0/all/0/1">C. A. Bischoff</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Bock_J/0/1/0/all/0/1">J. J. Bock</a> (3, 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Bowens_Rubin_R/0/1/0/all/0/1">R. Bowens-Rubin</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Brevik_J/0/1/0/all/0/1">J. A. Brevik</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Buder_I/0/1/0/all/0/1">I. Buder</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Bullock_E/0/1/0/all/0/1">E. Bullock</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Buza_V/0/1/0/all/0/1">V. Buza</a> (4, 9), <a href="http://arxiv.org/find/astro-ph/1/au:+Connors_J/0/1/0/all/0/1">J. Connors</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Cornelison_J/0/1/0/all/0/1">J. Cornelison</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Crill_B/0/1/0/all/0/1">B. P. Crill</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Crumrine_M/0/1/0/all/0/1">M. Crumrine</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Dierickx_M/0/1/0/all/0/1">M. Dierickx</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Duband_L/0/1/0/all/0/1">L. Duband</a> (11), <aRead More →

Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association. II. ISM kinematics and YSOs in the star cluster vdB 130 region. (arXiv:1904.01641v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sitnik_T/0/1/0/all/0/1">T.G. Sitnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egorov_O/0/1/0/all/0/1">O.V. Egorov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lozinskaya_T/0/1/0/all/0/1">T.A. Lozinskaya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moiseev_A/0/1/0/all/0/1">A.V. Moiseev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tatarnikov_A/0/1/0/all/0/1">A.M. Tatarnikov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vozyakova_O/0/1/0/all/0/1">O.V. Vozyakova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wiebe_D/0/1/0/all/0/1">D.S. Wiebe</a> We present an observational study of small-scale feedback processes operating in the star-forming region located in the wall of the expanding supershell around the Cyg OB1 association. The interstellar gas and dust content and pre-stellar populations in the vicinity of the open star cluster vdB 130 are analysed based on new optical and IR observations performed withRead More →

Prospects for Searching Thermal Effects, Non-Newtonian Gravity and Axion-Like Particles: Cannex Test of the Quantum Vacuum. (arXiv:1904.01642v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Klimchitskaya_G/0/1/0/all/0/1">Galina L. Klimchitskaya</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Mostepanenko_V/0/1/0/all/0/1">Vladimir M. Mostepanenko</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sedmik_R/0/1/0/all/0/1">Ren&#xe9; I. P. Sedmik</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Abele_H/0/1/0/all/0/1">Hartmut Abele</a> We consider the CANNEX (Casimir And Non-Newtonian force EXperiment) test of the quantum vacuum intended for measuring the gradient of the Casimir pressure between two flat parallel plates at large separations and constraining parameters of the chameleon model of dark energy in cosmology. A modification of the measurement scheme is proposed that allows simultaneous measurements of both the Casimir pressure and its gradient in one experiment. It is shown that withRead More →

Astro2020 Science White Paper: Physical Conditions in the Cold Gas of Local Galaxies. (arXiv:1904.01661v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Leroy_A/0/1/0/all/0/1">Adam K. Leroy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolatto_A/0/1/0/all/0/1">Alberto D. Bolatto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_T/0/1/0/all/0/1">Timothy A. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_A/0/1/0/all/0/1">Aaron S. Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harris_A/0/1/0/all/0/1">Andrew Harris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_P/0/1/0/all/0/1">Philip Hopkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">Annie Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Indebetouw_R/0/1/0/all/0/1">Remy Indebetouw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_K/0/1/0/all/0/1">Kelsey E. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kepley_A/0/1/0/all/0/1">Amanda A. Kepley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koda_J/0/1/0/all/0/1">Jin Koda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meier_D/0/1/0/all/0/1">David Meier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murphy_E/0/1/0/all/0/1">Eric Murphy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">Desika Narayanan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosolowsky_E/0/1/0/all/0/1">Erik Rosolowsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schinnerer_E/0/1/0/all/0/1">Eva Schinnerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_J/0/1/0/all/0/1">Jiayi Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_C/0/1/0/all/0/1">Christine Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wong_T/0/1/0/all/0/1">Tony Wong</a> We describe a next major frontier in observational studies of galaxy evolution and star formation: linking the physical conditions in the cold, star-forming interstellar medium to hostRead More →

Global Radiation Magneto-hydrodynamic Simulations of Sub-Eddington Accretion Disks around Supermassive Black Holes. (arXiv:1904.01674v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_Y/0/1/0/all/0/1">Yan-Fei Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blaes_O/0/1/0/all/0/1">Omer Blaes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">James Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_S/0/1/0/all/0/1">Shane W. Davis</a> We use global three dimensional radiation magneto-hydrodynamic simulations to study the properties of inner regions of accretion disks around a 5times 10^8 solar mass black hole with mass accretion rates reaching 7% and 20% of the Eddington value. This region of the disk is supported by magnetic pressure with surface density significantly smaller than the values predicted by the standard thin disk model but with a much larger disk scale height. The disks do not show any signRead More →

Template Bank for Compact Binary Coalescence Searches in Gravitational Wave Data: A General Geometric Placement Algorithm. (arXiv:1904.01683v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Roulet_J/0/1/0/all/0/1">Javier Roulet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_L/0/1/0/all/0/1">Liang Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venumadhav_T/0/1/0/all/0/1">Tejaswi Venumadhav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zackay_B/0/1/0/all/0/1">Barak Zackay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zaldarriaga_M/0/1/0/all/0/1">Matias Zaldarriaga</a> We introduce an algorithm for placing template waveforms for the search of compact binary mergers in gravitational wave interferometer data. We exploit the smooth dependence of the amplitude and unwrapped phase of the frequency-domain waveform on the parameters of the binary. We group waveforms with similar amplitude profiles and perform a singular value decomposition of the phase profiles to obtain an orthonormal basis for the phase functions. The leading basis functions spanRead More →

Gaia-assisted selection of a quasar reddened by dust in an extremely-strong Damped Lyman-{alpha} Absorber at z=2.226. (arXiv:1904.01686v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Geier_S/0/1/0/all/0/1">Stefan Geier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heintz_K/0/1/0/all/0/1">Kasper Elm Heintz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fynbo_J/0/1/0/all/0/1">Johan Fynbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ledoux_C/0/1/0/all/0/1">C&#xe9;dric Ledoux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_L/0/1/0/all/0/1">Lise Christensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jakobsson_P/0/1/0/all/0/1">Pall Jakobsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krogager_J/0/1/0/all/0/1">Jens-Kristian Krogager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milvang_Jensen_B/0/1/0/all/0/1">Bo Milvang-Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moller_P/0/1/0/all/0/1">Palle M&#xf8;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noterdaeme_P/0/1/0/all/0/1">Pasquier Noterdaeme</a> Damped Lyman-{alpha} Absorbers (DLAs) as a class of QSO absorption-line systems are currently our most important source of detailed information on the cosmic chemical evolution of galaxies. However, the degree to which this information is biased by dust remains to be understood. One strategy is to specifically search for QSOs reddened by metal-rich and dusty foregroundRead More →

Resolution Study for Three-dimensional Supernova Simulations with the Prometheus-Vertex Code. (arXiv:1904.01699v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Melson_T/0/1/0/all/0/1">Tobias Melson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janka_H/0/1/0/all/0/1">H.-Thomas Janka</a> (MPI Astrophysics, Garching) We present a carefully designed, systematic study of the angular resolution dependence of simulations with the Prometheus-Vertex neutrino-hydrodynamics code. Employing a simplified neutrino heating-cooling scheme in the Prometheus hydrodynamics module allows us to sample the angular resolution between 4 degrees and 0.5 degrees. With a newly-implemented static mesh refinement (SMR) technique on the Yin-Yang grid, the angular coordinates can be refined in concentric shells, compensating for the diverging structure of the spherical grid. In contrast to previous studies with Prometheus and other codes, weRead More →

The Wolf-Rayet Stellar Response To The Iron Opacity Bump: Envelope Inflation, Winds, and Microturbulence. (arXiv:1904.01703v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ro_S/0/1/0/all/0/1">Stephen Ro</a> Early-type Wolf-Rayet(WR) stellar models harbor a super-Eddington layer in their outer envelopes due to a prominent iron opacity bump. In the past few decades, one-dimensional hydrostatic and time-steady hydrodynamic models have suggested a variety of WR responses to a super-Eddington force including envelope inflation and optically thick winds. In this paper, I study these responses using semianalytical estimates and WR models from both MESA and Ro & Matzner; four conclusions are present. First, early-type WR stars do not harbor inflated envelopes because they have either strongRead More →

Weak Shock Propagation with Accretion. III. A Numerical Study On Shock Propagation & Stability. (arXiv:1904.01706v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ro_S/0/1/0/all/0/1">Stephen Ro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_E/0/1/0/all/0/1">Eric R. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quataert_E/0/1/0/all/0/1">Eliot Quataert</a> Core-collapse supernovae span a wide range of energies, from much less than to much greater than the binding energy of the progenitor star. As a result, the shock wave generated from a supernova explosion can have a wide range of Mach numbers. In this paper, we investigate the propagation of shocks with arbitrary initial strengths in polytropic stellar envelopes using a suite of spherically symmetric hydrodynamic simulations. We interpret these results using the three known self-similar solutions for thisRead More →