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Chandrasekhar limit
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<p> The Chandrasekhar limit is the maximum mass of a <a href="/facts/Hydrostatic_equilibrium/e75gVkh2">stable</a> <a href="/facts/White_dwarf/gIYlTtrC">white dwarf</a> <a href="/facts/Star/PFbd6ICx">star</a>. The currently accepted value of the Chandrasekhar limit is about 1.4 <a href="/facts/Solar_mass/j6Auhku8">M☉</a> (2.765×1030 kg). The limit was named after <a href="/facts/Subrahmanyan_Chandrasekhar/LQID778M">Subrahmanyan Chandrasekhar</a>. </p><p>White dwarfs resist <a href="/facts/Gravitational_collapse/7f4zQs8Y">gravitational collapse</a> primarily through <a href="/facts/Electron_degeneracy_pressure/fupuyb5c">electron degeneracy pressure</a>, compared to <a href="/facts/Main_sequence/DJ3Wq8kd">main sequence</a> stars, which resist collapse through <a href="/facts/Pressure/eyc37GRG">thermal pressure</a>. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction. </p>