Stability of G plus modes in a 30 solar-mass star

Details Stability of G plus modes in a 30 solar-mass star Stability of G plus modes in a 30 solar-mass star

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..39..463s&link_type=abstract

Astrophysics and Space Science, vol. 39, Feb. 1976, p. 463-475.

Astronomy and Astrophysics

Astrophysics

8

Dynamic Stability, Main Sequence Stars, Stellar Structure, Vibration Mode, Adiabatic Conditions, Asymptotic Methods, Hydrogen, Nuclear Fusion, Stellar Models

Scientific paper

The evolution of a Population I 30 solar-mass star has been computed during the Main Sequence phases without taking semi-convection into account. These models have a temperature gradient larger than the adiabatic value in the inhomogeneous region. The models have been tested for stability towards g plus modes of non-radial oscillations to see whether Kato's mechanism leads to an instability. Whereas the models are stable during the early Main Sequence phases, they become unstable for low enough central hydrogen abundance.

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