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Chandrasekhar limit
In Binary Pulse Theory: Chandrasekhar Mass Limit
BPT explains itIn standard physics
About 1.4 solar masses, the most a white dwarf can hold before collapsing.
In Binary Pulse Theory
Derived from the Planck mass, so it follows the level: M⊘ = 3.098 · m_P³ / (μₑ · m_H)².
The BPT terms behind it
Chandrasekhar Mass LimitM⊘
The Chandrasekhar Mass Limit is the critical mass, M⊘ ≈ 1.43 solar masses for a carbon–oxygen white dwarf, above which a dead stellar core collapses; the book derives it as M⊘ = 3.098 · m_P³ / (μₑ · m_H)², the heaviest a white dwarf can be.
Also known as
white dwarf · white dwarf mass limit
Related
The standard physics term is here to help you find your way in; the book itself writes in BPT's own terms. Read them in the lexicon, or start the book at Binary Pulse Theory.