Main category
Natural Sciences (Astrophysics and Astrononmy)
Abstract
Over 35 years ago, it was proposed that there exists diagnostic potential in combining the small
and large frequency separations for solar-like oscillators.
Since then, we have been spoilt with a plethora long-timeseries photometric light curves from
which individual stochastic oscillation modes can be extracted. These light curves allow the
separations to be determined en masse and in power spectra with relatively low signal-to-noise
ratios.
The small-frequency separation in low-mass main-sequence stars and in subgiants is sensitive
to the molecular weight gradient in the inner regions whilst the large-frequency separation is
indicative of the mean density of the star.
We investigate how accurately these parameters must be determined in order to place
constraints on stellar parameters such as mass and age. We discuss some difficulties
associated with calculating the necessary large grids of models (with different input physics)
as well as the degeneracy that exists in later evolutionary phases.
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