Abstract
Now we are ready to apply the physics we have learned toward understanding the structure and evolution of stars. Our approach to this will be to track the progress of a star like the sun on a standard H-R diagram as it passes through the various stages in its evolution. The sun is a relatively light weight star. Heavier stars will follow a somewhat different course, but the physical processes are essentially the same. For this purpose, we use the diagram in Fig. 19.1. The range of temperatures is quite large, therefore, it will be convenient to use a logarithmic temperature scale. For reference, we show the main-sequence on the diagram.
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© 1998 Springer Science+Business Media New York
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Seaborn, J.B. (1998). No More to Wonder What You Are…. In: Understanding the Universe. Springer, New York, NY. https://doi.org/10.1007/978-1-4612-0689-7_19
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DOI: https://doi.org/10.1007/978-1-4612-0689-7_19
Publisher Name: Springer, New York, NY
Print ISBN: 978-1-4612-6868-0
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