Editing Gravitational collapse (section)

{{short description|Contraction of an astronomical object due to the influence of its gravity}}
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[[Image:Core collapse scenario.svg|thumb|Gravitational collapse of a massive star, resulting in a [[Type II supernova]]]]

'''Gravitational collapse''' is the contraction of an [[astronomical object]] due to the influence of its own [[gravity]], which tends to draw matter inward toward the [[center of gravity]].<ref>{{cite book|last1=Pilchin|first1=Lev Eppelbaum, Izzy Kutasov, Arkady|title=Applied geothermics|date=2013|publisher=Springer Berlin Heidelberg|location=Berlin, Heidelberg|isbn=9783642340239|page=2|edition=Aufl. 2014}}</ref> Gravitational collapse is a fundamental mechanism for structure formation in the universe. Over time an initial, relatively smooth distribution of [[matter]], after sufficient [[Accretion (astrophysics)|accretion]], may collapse to form pockets of higher density, such as [[star]]s or [[black hole]]s.

[[Star formation]] involves a gradual gravitational collapse of [[interstellar medium]] into clumps of [[molecular cloud]]s and potential [[protostar]]s. The compression caused by the collapse raises the temperature until [[thermonuclear fusion]] occurs at the center of the star, at which point the collapse gradually comes to a halt as the outward [[Thermal expansion|thermal pressure]] balances the gravitational forces. The star then exists in a state of [[dynamic equilibrium]]. During the star's evolution a star might collapse again and reach several new states of equilibrium.