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White Dwarfs and Neutron Stars
2004This chapter on the physics of compact objects begins with a section on white dwarfs. It will be shown that the famous Chandrasekhar equation is just the relativistic Thomas–Fermi equation. For white dwarfs the Thomas–Fermi approximation is ideally justified. For neutron stars the general relativistic stellar structure equations are needed.
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New white dwarf stars in the Sloan Digital Sky Survey Data Release 10
Monthly Notices of the Royal Astronomical Society, 2015Alejandra Romero +2 more
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Evolutionary and pulsational properties of white dwarf stars
Astronomy and Astrophysics Review, 2010A Corsico +2 more
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Non-validity of I–Love–Q Relations for Hot White Dwarf Stars
Monthly Notices of the Royal Astronomical Society, 2018Kuantay Boshkayev, Quevedo H
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White dwarf–red giant mergers, early-type R stars, J stars and lithium
Monthly Notices of the Royal Astronomical Society, 2013Xianfei Zhang +2 more
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The structure of white dwarf stars
2012A FORTRAN code to compute the structure of white dwarf Stars has been written. It is assumed that a good model for the matter in white dwarf stars is the free Fermi gas of electrons at zero temperature, treated with relativistic kinematics. The code written essentially solves numerically the two coupled first-order differential equations that ...
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