Abstract
The stars are huge gas spheres, hundred 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
Clayton, D. D. (1968/1983): Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York/University of Chicago Press, Chicago)
Novotny, E. (1973): Introduction to Stellar Atmospheres and Interiors (Oxford University Press, New York).
Schwarzschild, M. (1958/1965): Structure and Evolution of the Stars (Princeton University Press, Princeton/Dover, New York)
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© 1996 Springer-Verlag Berlin Heidelberg
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Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (1996). Stellar Structure. In: Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (eds) Fundamental Astronomy. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-03215-2_11
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DOI: https://doi.org/10.1007/978-3-662-03215-2_11
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