E
Edward F. Brown
Researcher at Michigan State University
Publications - 213
Citations - 17056
Edward F. Brown is an academic researcher from Michigan State University. The author has contributed to research in topics: Neutron star & X-ray binary. The author has an hindex of 61, co-authored 211 publications receiving 15421 citations. Previous affiliations of Edward F. Brown include University of Chicago & University of Cambridge.
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Journal ArticleDOI
Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars
Bill Paxton,Matteo Cantiello,Phil Arras,Lars Bildsten,Edward F. Brown,Aaron Dotter,Christopher R. Mankovich,Michael H. Montgomery,Dennis Stello,Francis Timmes,Richard H. D. Townsend +10 more
TL;DR: Modules for Experiments in Stellar Astrophysics (MESA) as discussed by the authors is an open source software package for modeling the evolution of stellar structures and composition. But it is not suitable for large-scale systems such as supernovae.
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Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
Bill Paxton,Matteo Cantiello,Phil Arras,Lars Bildsten,Edward F. Brown,Aaron Dotter,Christopher R. Mankovich,Michael H. Montgomery,Dennis Stello,Frank Timmes,Richard H. D. Townsend +10 more
TL;DR: The Modules for Experiments in Stellar Astrophysics (MESA) project as discussed by the authors provides a one-dimensional stellar evolution module, MESA Star, which can model the evolution of giant planets down to masses as low as one-tenth that of Jupiter.
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The equation of state from observed masses and radii of neutron stars
TL;DR: In this paper, an empirical dense matter equation of state (EOS) from a heterogeneous data set of six neutron stars was derived from a Markov chain Monte Carlo algorithm within a Bayesian framework to determine nuclear parameters such as the incompressibility and density dependence of the bulk symmetry energy.
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The Neutron Star Mass-Radius Relation and the Equation of State of Dense Matter
TL;DR: In this paper, it was shown that the radius of a 1.4 solar mass neutron star lies between 10.4 and 12.9 km, independent of assumptions about the composition of the core.
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Crustal Heating and Quiescent Emission from Transiently Accreting Neutron Stars
TL;DR: In this article, it was shown that the envelope relaxes to a thermal equilibrium set by the flux from the hot core, as if the neutron star were newly born, and the resulting luminosity is approximately 5×1032-5×1033 ergs s-1.