Linked from

The 13 pages that link to Chandrasekhar limit, each with the reason it gives.

• White dwarfRelated: Above this limit, electron pressure cannot support the star against collapse.

• SupernovaRelated: Approaching this limit can lead to runaway thermonuclear burning.

• Core-collapse supernovaRelated: The growing core approaches this limit as electron pressure becomes inadequate.

• Planetary nebulaRelated: The remnant's mass helps distinguish this pathway from stellar deaths that produce neutron stars.

• Electron degeneracy pressureRelated: Relativistic weakening of the pressure prevents electron support above this mass scale.

• Fermi gasRelated: It shows where Fermi pressure can no longer balance stellar gravity.

• Helium flashRelated: It frames the pressure physics of degenerate matter, though flash cores remain below this limit.

• Solar massRelated: Its value shows how the unit marks a decisive limit in stellar evolution.

• Degenerate matterRelated: Above this limit, electron pressure cannot support a white dwarf against gravity.

• Black dwarfRelated: The limit separates white-dwarf remnants from cores that collapse instead.