![]() 1990, Stellar Structure and Evolution (Berlin: Springer-Verlag). 1968, Principles of Stellar Structure, in two volumes (New York: Gordon and Breach) 1986, The Penguin Dictionary of Modern Humorous Quotations (London: Penguin Books Ltd.). This process is experimental and the keywords may be updated as the learning algorithm improves. These keywords were added by machine and not by the authors. The vast majority of stars spend most of their active lives in such an equilibrium state, and it is only the gradual transmutation of elements by the fusion process that eventually causes their structure to change in some marked way. The power so produced then gradually leaks out through the remaining bulk of the star and finally gives rise to the radiation we see streaming off the surface. In the deep interior of a star these temperatures are measured in (at least) millions of degrees Kelvin and, in most instances, are sufficiently high to initiate the thermonuclear fusion of light nuclei. The reason for this relative tranquility is that stars are, on the whole, very stable objects in which self-gravitational forces are delicately balanced by steep internal pressure gradients. ![]() This is certainly true from a personal or historical perspective and, from fossil evidence, we can extend this to a roughly three-billion-year span for the sun. ![]() You will find that they appear to do nothing much at all except shine steadily. If you want to gain an important insight into what makes stars work, go out and look at them for a few nights.
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