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definition | This represents the maximum fraction of a star's mass that can be contained within an isothermal core while still supporting the rest of the star in hydrostatic equilibrium. Once the mass of an isothermal helium core exceeds this limit, the corse collapses and the star evolve rapidly. The limit varies depending on the star. | ||||||
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scope note | Not to be confused with the Chandrasekhar limit. | ||||||
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contributor | AAS_Frey.Katie original | ||||||
creator | AAS_Frey.Katie original |