Astrophysics (index)about

gravitational collapse

(shrinking of an object from gravitational force)

Gravitational collapse is the shrinking of an object due to the force of gravity not being fully counteracted. An object in hydrostatic equilibrium is balancing the force of gravity with internal pressure. An object undoubtedly attained hydrostatic equilibrium through previous gravitational collapse, and if the internal pressure for some reason is reduced (slowly through cooling, or more quickly, as through the exhaustion of fuel for the fusion that maintains the internal temperature within stars), gravitational collapse will resume.

Gravitational collapse releases energy (gravitational collapse energy, via the Kelvin-Helmholtz mechanism), which, at one time, was thought to be the source of the Sun's energy and is still considered a significant energy source during some phases of a star's lifetime, such as pre-main-sequence stars that have yet to trigger fusion. The energy that could be released if a body (star, cloud, etc.) collapses can be determined through the virial theorem which states the balance between thermal/kinetic energy versus potential energy in a system in hydrostatic equilibrium.

Gravitational collapse energy can be extreme, i.e., in strong-field gravity. It is considered the energy source of active galactic nuclei/quasars, and is sizable in the formation of compact objects. It is often a natural candidate for the explanation of observed phenomena that imply huge amounts of energy expenditure.


Referenced by:
black hole (BH)
direct collapse black hole (DCBH)
free-fall time
HII region (HII)
homologous collapse
main sequence star (V)
neutron star