229:, the star leaves the main sequence with a core mass already greater than the Schönberg–Chandrasekhar limit so its core is never isothermal before helium fusion. In the remaining case, where the mass is between 1.5 and 6 solar masses, the core will grow until the limit is reached, at which point it will contract rapidly until helium starts to fuse in the core.
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at the center of the star. The star then contracts until hydrogen fuses in a shell surrounding a helium-rich core, both of which are surrounded by an envelope consisting primarily of hydrogen. The core increases in mass as the shell burns its way outwards through the star. If the star's mass is
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core that can support an enclosing envelope. It is expressed as the ratio of the core mass to the total mass of the core and envelope. Estimates of the limit depend on the models used and the assumed chemical compositions of the core and envelope; typical values given are from 0.10 to 0.15 (10% to
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15% of the total stellar mass). This is the maximum to which a helium-filled core can grow, and if this limit is exceeded, as can only happen in massive stars, the core collapses, releasing energy that causes the outer layers of the star to expand to become a red giant. It is named after the
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150:{\displaystyle \operatorname {\left({\frac {\operatorname {M} _{c}}{M}}\right)} _{SC}=0.37\left({\frac {\operatorname {\mu } _{e}}{\operatorname {\mu } _{c}}}\right)^{2}}
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The
Schoenberg–Chandrasekhar limit: A polytropic approximation, Martin Beech,
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The Schönberg–Chandrasekhar limit comes into play when fusion in a
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The
Encyclopedia of Astrobiology, Astronomy, and Spaceflight
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285:On the Evolution of the Main-Sequence Stars
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269:Schönberg–Chandrasekhar limit
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