Vibrational stability of first generation stars

Details Vibrational stability of first generation stars Vibrational stability of first generation stars

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...103..390i&link_type=abstract

Astronomy and Astrophysics, vol. 103, no. 2, Nov. 1981, p. 390-392. Research supported by the Scientific and Technical Research

Astronomy and Astrophysics

Astrophysics

12

Adiabatic Conditions, Main Sequence Stars, Stellar Evolution, Stellar Models, Stellar Oscillations, Vibration Mode, Chemical Composition, Critical Mass, Galactic Evolution, Helium, Hydrogen, Stellar Mass, Stellar Structure, Stellar Temperature

Scientific paper

The vibrational stability towards radial oscillations of homogeneous main sequence stars initially composed of 80 percent of hydrogen and 20 percent of helium in mass and no metals is studied. During the pre-main sequence phase, enough carbon is accumulated to trigger the CN-cycle. The critical mass for vibrational stability is found to be 123 solar masses.

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