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.
KeywordsBurning Nickel Convection Helium Photodissociation
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- Clayton, D. D. (1968/1983): Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York/University of Chicago Press, Chicago)Google Scholar
- Novotny, E. (1973): Introduction to Stellar Atmospheres and Interiors (Oxford University Press, New York)Google Scholar
- Schwarzschild, M. (1958/1965): Structure and Evolution of the Stars (Princeton University Press, Princeton/Dover, New York)Google Scholar