Abstract
HR 5235, better known as η Bootis, is a bright and well-known star for which very accurate observations have recently enabled Kjeldsen et al. (2003) and Carrier, Bouchy, and Eggenberger (2003) not only to confirm the presence of solar-like oscillations, but also to identify the excitation in the oscillation spectrum of several p-mode frequencies with harmonic degrees l = 0 – 2. Here we show how such observational success, through the calculation and the investigation of theoretical structure models and the comparison of the observed oscillation spectra with the predicted p-mode frequencies of oscillations, permits one to draw conclusions about the actual evolutionary state of this star and on the physical properties of its internal structure. The computation of the structure models is based on the use of updated global parameters and includes overshooting from the convective core. In particular, we consider the effect on the stellar structure, and hence on the theoretical frequencies, of employing different equations of state and different formalisms to describe the convective energy transport.
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Di Mauro, M.P., Christensen-Dalsgaard, J., Paternò, L. et al. Interpretation of the solar-like pulsational behaviour of η Bootis. Solar Physics 220, 185–198 (2004). https://doi.org/10.1023/B:SOLA.0000031379.44874.3e
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DOI: https://doi.org/10.1023/B:SOLA.0000031379.44874.3e