中国科学院云南天文台机构知识库

Stellar age is an important quantity in astrophysics, which is useful for many fields both in the universe and galaxies. It cannot be determined by direct measurements, but can only be estimated or inferred. We attempt to find a useful indicator of stellar age, which is accurate from the zero-age main sequence to the tip of red giant branch for low-mass stars. Using the Yale Rotation and Evolution Code (YREC), a grid of stellar models has been constructed. Meanwhile, the frequency of maximum oscillations' power nu(max) and the large frequency separation Delta nu are calculated using the scaling relations. For the stars, the masses of which are from 0.8M(circle dot) to 2.8M(circle dot), we can obtain the nu(max) and stellar age by combing the scaling relations with the four sets of grid models (YREC, Dotter et al., Marigo et al., and YY isochrones). We find that nu(max) is tightly correlated and decreases monotonically with the age of the star from the main sequence to the red giant evolutionary stages. Moreover, we find that the line shapes of the curves in the Age versus nu(max) diagram, which is plotted by the four sets of grid models, are consistent for red giants with masses from 1.1 M-circle dot to 2.8 M-circle dot. For red giants, the differences of correlation coefficients between Age and nu(max) for different grid models are minor and can be ignored. Interestingly, we find two peaks that correspond to the subgiants and bump of red giants in the Age versus nu(max) diagram. By general linear least-squares, we make the polynomial fitting and deduce the relationship between log(Age) and log(nu(max)) in red giants' evolutionary state.