Abstract
In the last section we left the newly born star while it was still contracting in hydrostatic, but not yet thermal, equilibrium. Essential features of this contraction can already be understood by assuming simple homologous changes. It will turn out that the fate of such a sphere is mainly determined by the equation of state.
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Notes
- 1.
Since the dash-dotted line in Fig. 28.1 gives the impression of delineating a hill, this kind of figure is sometimes called Thomas-mountain after H.-C. Thomas who first used it to illustrate the evolution of homologously contracting stellar cores.
- 2.
An isochrone is the locus of stellar models of identical age, but different mass in the Hertzsprung–Russell diagram.
References
Cignoni, M., Sabbi, E., Nota, A., Tosi, M., Degl’Innocenti, S., Prada Moroni, P.G., Angeretti, L., Carlson, L.R., Gallagher, J., Meixner, M., Sirianni, M., Smith, L.J. (2009): Astron. J. 137, 3668
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© 2012 Springer-Verlag Berlin Heidelberg
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Kippenhahn, R., Weigert, A., Weiss, A. (2012). Pre-Main-Sequence Contraction. In: Stellar Structure and Evolution. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-30304-3_28
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DOI: https://doi.org/10.1007/978-3-642-30304-3_28
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