Abstract
The stars are huge gas spheres, hundreds of thousands or millions of times more massive than the Earth. A star such as the Sun can go on shining steadily for thousands of millions of years. This is shown by studies of the prehistory of the Earth, which indicate that the energy radiated by the Sun has not changed by much during the last four thousand million years. The equilibrium of a star must remain stable for such periods.
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Further Reading
Bowers, Deeming: Astrophysics I: Stars, Jones and Bartlett Publishers 1984.
Böhm-Vitense: Introduction to Stellar Astrophysics; Cambridge University Press, Vol. 1–3 1989–1992.
Clayton: Principles of Stellar Evolution and Nucleosynthesis,McGraw-Hill 1968.
Hansen, Kawaler: Stellar interiors, Physical principles, structure and evolution, Springer 1994.
Harpaz: Stellar Evolution,Peters Wellesley 1994.
Kippenhahn, Weigert: Stellar Structure and Evolution, Springer, 2nd ed. 1994.
Phillips: The physics of Stars,Manchester Phys. Ser. 1994, 2nd ed. 1999.
Taylor: The Stars: their structure and evolution,Cambridge University Press 1994.
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Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (2003). Stellar Structure. In: Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (eds) Fundamental Astronomy. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-05333-1_10
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DOI: https://doi.org/10.1007/978-3-662-05333-1_10
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