By R. Kippenhahn (auth.), Zdenék Kopal, Jürgen Rahe (eds.)
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Additional info for Binary and Multiple Stars as Tracers of Stellar Evolution: Proceedings of the 69th Colloquium of the International Astronomical Union, held in Bamberg, F.R.G., August 31 – September 3, 1981
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Helium is mixed to the surface but there is no change in the 12C and 14N abundances as for more massive stars. In the HR-diagram the star moves up the red giant branch (see Fig. 9) until finally helium 1S ignited. 3. However, Thomas at that time used neutrino rates which hav~ since been improved. 1, (Thomas 1970, see also Demarque, Men~el, 1971)). Figure 8r describes the events at and after the onset of helium burning. After the ignition of helium in the degenerate region a thermal runaway starts and a convective shell is formed.
A. ), Nonradial and nonlinear Stellar Pulsation, p. 22. J. 148, p. 481. A. A. ), Nonradial and Nonlinear Stellar Pulsation, p. 7. Hoffleit, D. , New Haven, Connecticut. J. 84, p. 1770. T. :1971, Astron. Astrophys. 12, p. 223. J. 221, p. 869. :1967, unpublished thesis. A. A. ), Nonradial and Nonlinear Stellar Pulsation, p. 60. Astrophys. 50, p. 435. ON THE INTERNAL STRUCTURE OF MAIN-SE0UENCE STARS Alvaro Gim€nez and Jos€ M. Garcia-Pelayo Instituto de Astrofisica de Andalucia. Apartado 2144. Granada.