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Chandrasekhar limit
Sign in to savemaximum mass of a stable white dwarf star, approximately 1.4 solar masses
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Vinony's link graph records 184 inbound references to Chandrasekhar limit, and connects out to supernova, degenerate matter and mass density.
It sits within the topics Astrophysics, Neutron stars and Stellar dynamics.
Vinony links it to 50 Wikipedia language editions.
Wikidata facts
- Instance of
- physical constant
- Part of
- stellar physics
- Named after
- Subrahmanyan Chandrasekhar
Show 3 more facts
- facet of
- type Ia supernova
- numeric value
- 1.4
- maintained by WikiProject
- WikiProject Mathematics
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Encyclopedic overview
The Chandrasekhar limit (/ˌtʃəndrəˈʃeɪkər/) is the maximum mass of a stable white dwarf star. These stars resist gravitational collapse primarily through electron degeneracy pressure, compared to main sequence stars, which resist collapse through thermal pressure. 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. The value of the Chandrasekhar limit depends upon the ratio of the number of electrons to nucleons (neutrons plus protons) in the star. For small stars this ratio is around 1/2 and the limit is about 1.44 M☉. The limit was named after Subrahmanyan Chandrasekhar who won the 1983 Nobel prize together with William Alfred Fowler for work on stellar models.
Physics
Excerpted from Wikipedia’s “Chandrasekhar limit” article, available under the CC BY-SA 4.0 licence.