Vibrational stability of an evolved 5-solar-mass star towards higher-order g-modes

Details Vibrational stability of an evolved 5-solar-mass star towards higher-order g-modes Vibrational stability of an evolved 5-solar-mass star towards higher-order g-modes

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...263..137d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 263, no. 1-2, p. 137-146.

Statistics

Computation

2

B Stars, Stellar Evolution, Stellar Models, Stellar Oscillations, Variable Stars, Vibration Mode, Computational Astrophysics, Hydrogen, Stellar Convection, Stellar Mass

Scientific paper

The vibrational stability towards low-degree higher-order nonradial g(+)-modes has been studied for an evolutionary model of a 5 solar mass star near the end of central hydrogen burning, for the oscillations with periods in the range of one to three days found in mid-B variables. The stability analysis is performed on the basis of the quasi-isentropic approximation. The effects of convection are neglected. The model with log10 T(eff) = 4.17 and log10 L/L(solar) = 2.93 is shown to be vibrationally unstable towards the second-degree mode g(+)38 with a period of 1.57 days. The main cause of the driving is the kappa-mechanism in the He II ionization zone.

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