What physical state maintains a star against collapse, determined by mass-dictated fusion rate?

Hydrostatic equilibrium

The mass of a star fundamentally determines the immense gravitational pressure exerted inward at its core. To prevent this overwhelming gravitational force from causing the star to collapse catastrophically, an outward pressure must be generated. This outward pressure and heat are supplied by the nuclear fusion reactions occurring deep within the core. The sustained balance between the inward crushing force of gravity and the outward pressure generated by sustained nuclear fusion defines the crucial condition known as hydrostatic equilibrium. This equilibrium is the stable state in which a star spends the majority of its existence, and maintaining it requires that the internal fusion rate precisely matches the energy demands imposed by the star's total mass.