Abstract
In previous chapters we examined physical processes that occur near a star’s surface (atomic excitation, ionization, absorption) and in the interior (nuclear fusion). Now we unite them in detailed models of stars. We use the models to analyze the structure of stars during the main stage of life when they burn hydrogen to generate the heat and pressure that balance gravity. We then consider what happens when the hydrogen fuel runs out. As we will see, old stars begin burning heavier nuclei and working their way up the periodic table of the elements. How far a star gets depends on its mass: stars with masses below about 8 M ⊙ reach carbon and oxygen before experiencing a relatively meek death; stars with masses above about 8 M ⊙, by contrast, create all the heavier elements and then literally go out with a bang.
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Notes
- 1.
The situation is similar to water boiling, although that case is slightly more complicated because it involves the formation of air bubbles.
- 2.
Recall from Sect. 16.1.2 that this equation applies to an ideal gas in hydrostatic equilibrium.
- 3.
Strictly speaking, some matter gets converted to energy, but that is a small fraction of the total.
- 4.
- 5.
Carroll and Ostlie [2] discuss stellar evolution at a similar technical level but in more detail.
- 6.
A little energy is available from radioactive decay of nickel-56 into cobalt-56 and then into iron-56, but it is not enough to support the star.
- 7.
- 8.
In addition, there were supernovae that were probably type Ia seen in the years 1006, 1572 (“Tycho’s supernova”), and 1604 (“Kepler’s supernova”).
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Keeton, C. (2014). Stellar Structure and Evolution. In: Principles of Astrophysics. Undergraduate Lecture Notes in Physics. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-9236-8_16
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