On p-mode oscillations in stars from 1 solar mass to 2 solar masses

Details On p-mode oscillations in stars from 1 solar mass to 2 solar masses On p-mode oscillations in stars from 1 solar mass to 2 solar masses

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..152..316a&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 152, no. 1, p. 316

Physics

Acoustic Frequencies, P Waves, S Waves, Stellar Evolution, Stellar Interiors, Stellar Mass, Stellar Oscillations, Frequency Discriminators, Helium, Seismic Waves, Stellar Luminosity

Scientific paper

The structure of stars more massive than about 1.2 solar masses is characterized by a convective core. We have studied the evolution with age and mass of acoustic frequencies of high radical order n and low degree l for models of stars of 1, 1.5 and 2 solar masses. Using a polynomial approximation for the frequency, the p-mode spectrum can be characterized by derived global asteroseismic coefficients, i.e. the mean separation nu0 is approximately equal to nun, l - nun - 1, l and the small frequency separation Delta nu0, 2 is approximately equal to nun, l = 0 - nun - 1, l = 2. The diagram (nu0, delta nu0, 2/nu0) plotted along the evolutionary tracks would help to separate the effects of age and mass. We study the sensitivity of these coefficients and other observable quantities, like the radius and luminosity, to stellar parameters in the vicinity of 1 solar mass and 2 solar masses; this sensitivity substantially depends on the stellar mass and must be taken into account for asteroseismic calibration of stellar clusters. Considering finally some rapid variations of the internal structure, we show that the second frequency difference delta2 nu = nu(subn, l) - 2 nun - 1, l + nun - 2, l exponent gamma in the He II ionization zone.

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