= Stellar evolution
{wiki}
<Stellar evolution> is the change of a <star>'s composition, structure and observable properties over time. <Nuclear fusion> changes the core's composition and available fuel; <gravity>, energy transport and mass loss then alter the <stellar radius>, <luminosity> and <effective temperature>. The initial <mass> strongly influences the sequence, but composition, rotation and <binary mass transfer> also matter.
The <evolution of a solar-mass star> connects the <main sequence> to giant phases and eventually a <white dwarf>. More massive <stars> can reach <stellar core collapse>. An evolutionary track in the <Hertzsprung-Russell diagram> makes these changes visible, while comparisons with coeval stellar populations test the predicted lifetimes. Two <stars> with similar present appearance can have different prior histories, especially after binary interaction.
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