The balance between the outward pressure from nuclear fusion and radiation in a star's core and the inward gravitational force trying to collapse the star. This equilibrium maintains a star's stable size and structure throughout most of its lifetime.
From Greek 'hydro' meaning water (extended to fluids in general), 'statikos' meaning causing to stand or stationary, and Latin 'aequilibrium' meaning equal balance. The concept was developed from fluid mechanics and applied to stellar structure in the early 20th century.
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