Abstract
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).
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© 1990 Springer-Verlag Berlin Heidelberg
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Kippenhahn, R., Weigert, A. (1990). Chemical Evolution on the Main Sequence. In: Stellar Structure and Evolution. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-61523-8_30
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DOI: https://doi.org/10.1007/978-3-642-61523-8_30
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-540-58013-3
Online ISBN: 978-3-642-61523-8
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