Gravity gathers material
Dense clumps can contract and become protostars.
Compression raises temperature
Gravitational energy is converted into thermal energy.
Fusion marks a major transition
When core conditions become hot and dense enough, hydrogen fusion can support a stable star.
Mass shapes the future
A star's mass strongly influences its temperature, lifetime and eventual fate.
Source trail: NASA: star basics
This page explains scientific concepts for general learning. It does not replace laboratory safety procedures, professional engineering guidance, or individualized medical advice.