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How Salty is Enceladus’ Ocean Under the ice? An icy satellite of Saturn, Enceladus, has been a subject of increasing interest in recent years since Cassini captured jets of water and other material being ejected out of the south pole of the moon.  One particularly tantalizing hypothesis supported by the sample composition is that there might be life in the oceans under the ice shells of Enceladus. To evaluate Enceladus’ habitability and to figure out the best way to probe this icy moon, scientists need to better understand the chemical composition and dynamics of Enceladus’ ocean. Specifically, an appropriate salinity could be important for habitability.Read More →

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China Launches the Core Module of Its New Space Station Early on Thursday, a Long March 5B rocket – currently the most powerful of China’s space launch vehicles – blasted off from Wenchang, carrying the first major component of an ambitious new modular space station. The station module, dubbed Tianhe (Harmony of the Heavens), marks the next big step in China’s human spaceflight program in Low Earth Orbit (LEO). Barred from participating in the International Space Station (ISS) by US law, which forbids cooperation in space between the two countries, China has been developing its own LEO capabilities for over a decade now. It launchedRead More →

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Not just for finding planets: Exoplanet-hunter TESS telescope spots bright gamma-ray burst NASA has a long tradition of unexpected discoveries, and the space program’s TESS mission is no different. SMU astrophysicist and her team have discovered a particularly bright gamma-ray burst using a NASA telescope designed to find exoplanets—those occurring outside our solar system—particularly those that might be able to support life. phys.org Go to SourceRead More →

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11-Sigma Detection of Dark Energy Comes From Measuring Over a Million Extremely Distant Galaxies After galaxies began to form in the early universe, the universe continued to expand. The gravitational attraction between galaxies worked to pull galaxies together into superclusters, while dark energy and its resulting cosmic expansion worked to drive these clusters apart. As a result, the universe is filled with tight clusters of galaxies separated by vast voids of mostly empty space. The scale of these clusters and voids is based upon the rate at which the universe has expanded over time. The effect is similar to the way air molecules are clusteredRead More →

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The DALI experiment: Searching for the axion, a proposed component of dark matter The detection of the axion would mark a key episode in the history of science. This hypothetical particle could resolve two fundamental problems of Modern Physics at the same time: the problema of Charge and Parity in the strong interaction, and the mystery of dark matter. However, in spite of the high scientific interest in finding it, the search at high radio frequency—above 6 GHz—has been almost left aside for the lack of the high sensitivity technology which could be built at reasonable cost. Until now. phys.org Go to SourceRead More →

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ESA to build second deep space dish in Australia On 29 April, ESA and the Australian Space Agency announced the construction of a second 35-meter, deep space antenna at ESA’s New Norcia station, located 140 kilometers north of Perth in Western Australia. phys.org Go to SourceRead More →

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Latest observations by MUSER help clarify solar eruptions Prof. Yan Yihua and his research team from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC) recently released detailed results of observations by the new generation solar radio telescope—Mingantu Spectral Radio Heliograph (MUSER)—from 2014 to 2019. phys.org Go to SourceRead More →

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Constraints from LIGO O3 data on gravitational-wave emission due to r-modes in the glitching pulsar PSR J0537-6910. (arXiv:2104.14417v1 [astro-ph.HE]) The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_LIGO_Scientific/0/1/0/all/0/1">LIGO Scientific Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Virgo/0/1/0/all/0/1">Virgo Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_KAGRA/0/1/0/all/0/1">KAGRA Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_R/0/1/0/all/0/1">R. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. D. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_S/0/1/0/all/0/1">S. Abraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acernese_F/0/1/0/all/0/1">F. Acernese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackley_K/0/1/0/all/0/1">K. Ackley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_A/0/1/0/all/0/1">A. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_R/0/1/0/all/0/1">R. X. Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adya_V/0/1/0/all/0/1">V. B. Adya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Affeldt_C/0/1/0/all/0/1">C. Affeldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agarwal_D/0/1/0/all/0/1">D. Agarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agathos_M/0/1/0/all/0/1">M. Agathos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agatsuma_K/0/1/0/all/0/1">K. Agatsuma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aggarwal_N/0/1/0/all/0/1">N. Aggarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguiar_O/0/1/0/all/0/1">O. D. Aguiar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiello_L/0/1/0/all/0/1">L. Aiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ain_A/0/1/0/all/0/1">A. Ain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajith_P/0/1/0/all/0/1">P. Ajith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akutsu_T/0/1/0/all/0/1">T. Akutsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aleman_K/0/1/0/all/0/1">K. M. Aleman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_G/0/1/0/all/0/1">G. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allocca_A/0/1/0/all/0/1">A. Allocca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altin_P/0/1/0/all/0/1">P.Read More →

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The aox–HeII EW Connection in Radio-Loud Quasars. (arXiv:2104.14407v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Timlin_J/0/1/0/all/0/1">John D. Timlin III</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_S/0/1/0/all/0/1">Shifu Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_W/0/1/0/all/0/1">W. Niel Brandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laor_A/0/1/0/all/0/1">Ari Laor</a> Radio-loud quasars (RLQs) are known to produce excess X-ray emission, compared to radio-quiet quasars (RQQs) of the same luminosity, commonly attributed to jet-related emission. Recently, we found that the HeII EW and $alpha_{rm{ox}}$ in RQQs are strongly correlated, which suggests that their extreme-ultraviolet (EUV) and X-ray emission mechanisms are tightly related. Using 48 RLQs, we show that steep-spectrum radio quasars (SSRQs) and low radio-luminosity ($L_{rm R}$) flat-spectrum radio quasars (FSRQs) follow the $alpha_{rm ox}$–HeII EW relation of RQQs. This suggests thatRead More →

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Pseudo-2D Modelling of Heat Redistribution Through H$_2$ Thermal Dissociation/Recombination: Consequences for Ultra-Hot Jupiters. (arXiv:2104.14376v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Roth_A/0/1/0/all/0/1">Alexander Roth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drummond_B/0/1/0/all/0/1">Benjamin Drummond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebrard_E/0/1/0/all/0/1">Eric H&#xe9;brard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblin_P/0/1/0/all/0/1">Pascal Tremblin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goyal_J/0/1/0/all/0/1">Jayesh Goyal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayne_N/0/1/0/all/0/1">Nathan Mayne</a> Thermal dissociation and recombination of molecular hydrogen, H_2, in the atmospheres of ultra-hot Jupiters (UHJs) has been shown to play an important role in global heat redistribution. This, in turn, significantly impacts their planetary emission, yet only limited investigations on the atmospheric effects have so far been conducted. Here we investigate the heat redistribution caused by this dissociation/recombination reaction, alongside feedback mechanisms between the atmospheric chemistry and radiative transfer, for a planetaryRead More →

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Improved Treatment of Dark Matter Capture in White Dwarfs. (arXiv:2104.14367v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Bell_N/0/1/0/all/0/1">Nicole F. Bell</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Busoni_G/0/1/0/all/0/1">Giorgio Busoni</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ramirez_Quezada_M/0/1/0/all/0/1">Maura E. Ramirez-Quezada</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Robles_S/0/1/0/all/0/1">Sandra Robles</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Virgato_M/0/1/0/all/0/1">Michael Virgato</a> White dwarfs, the most abundant stellar remnants, provide a promising means of probing dark matter interactions, complimentary to terrestrial searches. The scattering of dark matter from stellar constituents leads to gravitational capture, with important observational consequences. In particular, white dwarf heating occurs due to the energy transfer in the dark matter capture and thermalisation processes, and the subsequent annihilation of captured dark matter. We consider the capture of dark matter by scattering on either the ion orRead More →

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Millimeter-wave spectroscopy of the $^{13}$CH$_3$OD isotopic species of methyl alcohol. (arXiv:2104.14340v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_L/0/1/0/all/0/1">Li-Hong Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lees_R/0/1/0/all/0/1">R. M. Lees</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zakharenko_O/0/1/0/all/0/1">O. Zakharenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_H/0/1/0/all/0/1">H. S. P. M&#xfc;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewen_F/0/1/0/all/0/1">F. Lewen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlemmer_S/0/1/0/all/0/1">S. Schlemmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">K. M. Menten</a> The dramatic increase in sensitivity, spectral coverage and resolution of radio astronomical facilities in recent years has opened new possibilities for observation of chemical differentiation and isotopic fractionation in protostellar sources to shed light on their spatial and temporal evolution. In warm interstellar environments, methanol is an abundant species, hence spectral data for its isotopic forms are of special interest. In the present work, the millimeter-wave spectrum ofRead More →

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In: arXiv

Coagulation of inertial particles in supersonic turbulence. (arXiv:2002.12172v2 [physics.flu-dyn] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Li_X/0/1/0/all/0/1">Xiang-Yu Li</a>, <a href="http://arxiv.org/find/physics/1/au:+Mattsson_L/0/1/0/all/0/1">Lars Mattsson</a> Coagulation driven by supersonic turbulence is primarily an astrophysical problem because coagulation processes on Earth are normally associated with incompressible fluid flows at low Mach numbers, while dust aggregation in the interstellar medium (ISM) for instance is an example of the opposite regime. We study coagulation of inertial particles in compressible turbulence using high-resolution direct and shock-capturing numerical simulations with a wide range of Mach numbers from nearly incompressible to moderately supersonic. The particle dynamics is simulated by representative particles and the effects on the size distribution and coagulationRead More →

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On moving shadows and pressure bumps in HD 169142. (arXiv:2007.11565v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bertrang_G/0/1/0/all/0/1">Gesa H.-M. Bertrang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flock_M/0/1/0/all/0/1">Mario Flock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keppler_M/0/1/0/all/0/1">Miriam Keppler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trifonov_T/0/1/0/all/0/1">Trifon Trifonov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penzlin_A/0/1/0/all/0/1">Anna B. T. Penzlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avenhaus_H/0/1/0/all/0/1">Henning Avenhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Thomas Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montesinos_M/0/1/0/all/0/1">Matias Montesinos</a> The search for young planets had its first breakthrough with the detection of the accreting planet PDS70b. In this study, we aim to broaden our understanding towards the formation of multi-planet systems such as HR8799 or the Solar System. Our previous study on HD169142, one of the closest Herbig stars, points towards a shadow-casting protoplanetary candidate. Here, we present follow-up observations to test our previously proposedRead More →

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Age and helium content of the open cluster NGC 6791 from multiple eclipsing binary members. III. Constraints from a subgiant. (arXiv:2104.14330v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Brogaard_K/0/1/0/all/0/1">K. Brogaard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grundahl_F/0/1/0/all/0/1">F. Grundahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sandquist_E/0/1/0/all/0/1">E. L. Sandquist</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slumstrup_D/0/1/0/all/0/1">D. Slumstrup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_M/0/1/0/all/0/1">M. L. Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomsen_J/0/1/0/all/0/1">J. B. Thomsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_J/0/1/0/all/0/1">J. H. J&#xf8;rgensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larsen_J/0/1/0/all/0/1">J. R. Larsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bjorn_S/0/1/0/all/0/1">S. T. Bj&#xf8;rn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sorensen_C/0/1/0/all/0/1">C. T. G. S&#xf8;rensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruntt_H/0/1/0/all/0/1">H. Bruntt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arentoft_T/0/1/0/all/0/1">T. Arentoft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frandsen_S/0/1/0/all/0/1">S. Frandsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jessen_Hansen_J/0/1/0/all/0/1">J. Jessen-Hansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orosz_J/0/1/0/all/0/1">J. A. Orosz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathieu_R/0/1/0/all/0/1">R. Mathieu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geller_A/0/1/0/all/0/1">A. Geller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryde_N/0/1/0/all/0/1">N. Ryde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stello_D/0/1/0/all/0/1">D. Stello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meibom_S/0/1/0/all/0/1">S. Meibom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Platais_I/0/1/0/all/0/1">I. Platais</a> Models of stellar structure and evolution can be constrained using accurateRead More →

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What Makes Quadruply Lensed Quasars Quadruple?. (arXiv:2102.08470v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Luhtaru_R/0/1/0/all/0/1">Richard Luhtaru</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Schechter_P/0/1/0/all/0/1">Paul L. Schechter</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Soto_K/0/1/0/all/0/1">Kaylee M. de Soto</a> (1) ((1) MIT Department of Physics, (2) MIT Kavli Institute for Astrophysics and Space Research) Among known strongly lensed quasar systems, ~25% have gravitational potentials sufficiently flat (and sources sufficiently well aligned) to produce four images rather than two. The projected flattening of the lensing galaxy and tides from neighboring galaxies both contribute to the potential’s quadrupole. Witt’s hyperbola and Wynne’s ellipse permit determination of the overall quadrupole from the positions of the quasar images. The position of the lensingRead More →

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Hyperbolic compactification of M-theory and de Sitter quantum gravity. (arXiv:2104.13380v1 [hep-th] CROSS LISTED) <a href="http://arxiv.org/find/hep-th/1/au:+Luca_G/0/1/0/all/0/1">G. Bruno De Luca</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Silverstein_E/0/1/0/all/0/1">Eva Silverstein</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Torroba_G/0/1/0/all/0/1">Gonzalo Torroba</a> We present a mechanism for accelerated expansion of the universe in the generic case of negative-curvature compactifications of M-theory, with minimal ingredients. M-theory on a hyperbolic manifold with small closed geodesics supporting Casimir energy — along with a single classical source (7-form flux) — contains an immediate 3-term structure for volume stabilization at positive potential energy. Hyperbolic manifolds are well-studied mathematically, with an important rigidity property at fixed volume. They and their Dehn fillings to more general Einstein spaces exhibit explicitRead More →

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PHANGS-ALMA: Arcsecond CO(2-1) Imaging of Nearby Star-Forming Galaxies. (arXiv:2104.07739v2 [astro-ph.GA] UPDATED) <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:+Schinnerer_E/0/1/0/all/0/1">Eva Schinnerer</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:+Rosolowsky_E/0/1/0/all/0/1">Erik Rosolowsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pety_J/0/1/0/all/0/1">J&#xe9;r&#xf4;me Pety</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schruba_A/0/1/0/all/0/1">Andreas Schruba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Usero_A/0/1/0/all/0/1">Antonio Usero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanc_G/0/1/0/all/0/1">Guillermo A. Blanc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chevance_M/0/1/0/all/0/1">M&#xe9;lanie Chevance</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Emsellem_E/0/1/0/all/0/1">Eric Emsellem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faesi_C/0/1/0/all/0/1">Christopher M. Faesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herrera_C/0/1/0/all/0/1">Cinthya N. Herrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">Daizhong Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meidt_S/0/1/0/all/0/1">Sharon E. Meidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Querejeta_M/0/1/0/all/0/1">Miguel Querejeta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saito_T/0/1/0/all/0/1">Toshiki Saito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sandstrom_K/0/1/0/all/0/1">Karin M. Sandstrom</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:+Williams_T/0/1/0/all/0/1">Thomas G. Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anand_G/0/1/0/all/0/1">Gagandeep S. Anand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barnes_A/0/1/0/all/0/1">Ashley T. Barnes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Behrens_E/0/1/0/all/0/1">Erica A. Behrens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belfiore_F/0/1/0/all/0/1">Francesco Belfiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benincasa_S/0/1/0/all/0/1">Samantha M. Benincasa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beslic_I/0/1/0/all/0/1">Ivana Be&#x161;li&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bigiel_F/0/1/0/all/0/1">Frank Bigiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolatto_A/0/1/0/all/0/1">Alberto D. Bolatto</a>, <aRead More →

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In: arXiv

How likely are Snowball episodes near the inner edge of the habitable zone?. (arXiv:2104.06216v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wordsworth_R/0/1/0/all/0/1">R. Wordsworth</a> Understanding when global glaciations occur on Earth-like planets is a major challenge in climate evolution research. Most models of how greenhouse gases like CO2 evolve with time on terrestrial planets are deterministic, but the complex, nonlinear nature of Earth’s climate history motivates study of non-deterministic climate models. Here a maximally simple stochastic model of CO2 evolution and climate on an Earth-like planet with an imperfect CO2 thermostat is investigated. It is shown that as stellar luminosity is increased in this model, the decrease in the averageRead More →