What dynamic stability maintains a main sequence star against gravitational collapse?

Answer

Hydrostatic equilibrium

The stability of a star during its long main sequence phase is governed by a perfect balance between two immense, opposing forces known as hydrostatic equilibrium. On one side is the relentless inward pull of gravity, generated by the star's massive self-weight, which constantly attempts to crush all the stellar material toward the center of mass. Counterbalancing this inward compression is the immense outward pressure generated by the energy release from thermonuclear fusion occurring deep within the stellar core. As long as these forces remain perfectly matched—the outward push exactly equaling the inward pull—the star maintains a stable size and temperature profile, defining the primary phase of its life. Any slight deviation from this balance triggers immediate self-correction mechanisms within the core, restoring equilibrium.

What dynamic stability maintains a main sequence star against gravitational collapse?

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