Semiconvection in stars of about 1 solar mass

Details Semiconvection in stars of about 1 solar mass Semiconvection in stars of about 1 solar mass

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....54..631g&link_type=abstract

Astronomy and Astrophysics, vol. 54, no. 2, Jan. 1977, p. 631-634.

Astronomy and Astrophysics

Astrophysics

10

Convective Heat Transfer, Stellar Evolution, Stellar Luminosity, Stellar Models, Stellar Temperature, Chemical Composition, Eigenvalues, Eigenvectors, Temperature Gradients

Scientific paper

The paper studies the vibrational stability of low-order g(plus) modes of high degree of spherical surface harmonics in stars of 1, 1.1, and 1.5 solar masses during core hydrogen burning. Such stars have a small convective core surmounted in some models by a small region where the temperature gradient is larger than the adiabatic value. Most of these models have been found to be stable, instabilities occurring only in two models of the 1.1-solar-mass sequence. If these instabilities are responsible for the formation of semiconvective zones as suggested by Kato (1964), the present results show that such zones will not necessarily form each time a superadiabatic zone exists and that they will indeed develop only in a small mass range and during a short fraction of the main-sequence lift time.

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