Chemical Evolution on the Main Sequence
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In the main-sequence phase, the large energy losses from a star’s surface are compensated by the energy production of hydrogen burning (see §18.5.1). These reactions release nuclear binding energy by converting hydrogen into helium. This chemical evolution of the star concerns primarily its central region, since the energy sources are strongly concentrated towards the centre (§22.2).
KeywordsMain Sequence Stellar Mass Envelope Curve Hydrogen Burning Evolutionary Track
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