Research Information System
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.462, no.2, pp.1577-1590, 2016 (SCI-Expanded)
So-called scaling relations based on oscillation frequencies have the potential to reveal the mass and radius of solar-like oscillating stars. In the derivation of these relations, it is assumed that the first adiabatic exponent at the surface (Gamma(1s)) of such stars is constant. However, by constructing interior models for the mass range 0.8-1.6 M-circle dot, we show that Gamma(1s) is not constant at stellar surfaces for the effective temperature range with which we deal. Furthermore, the well-known relation between large separation and mean density also depends on Gamma(1s). Such knowledge is the basis for our aim of modifying the scaling relations. There are significant differences between masses and radii found from modified and conventional scaling relations. However, a comparison of predictions of these relations with the non-asteroseismic observations of Procyon A reveals that new scaling relations are effective in determining the mass and radius of stars. In the present study, solar-like oscillation frequencies of 89 target stars (mostly Kepler and CoRoT) were analysed. As well as two new reference frequencies (nu(min1) and nu(min2)) found in the spacing of solar-like oscillation frequencies of stellar interior models, we also take into account nu(min0). In addition to the frequency of maximum amplitude, these frequencies have a very strong diagnostic potential in the determination of fundamental properties. The present study applies the derived relations from the models to the solar-like oscillating stars, and computes their effective temperatures using purely asteroseismic methods. There are in general very close agreements between effective temperatures from asteroseismic and nonasteroseismic (spectral and photometric) methods. For the Sun and Procyon A, for example, the agreement is almost total.