2008/02/01 by I. Dekany, I. Dékány, G. Kovács +14 · 1 citation
Physics and Astronomy · #Adiabatic process #Astrophysics #Astrophysics and Star Formation Studies #Consistency (knowledge bases) #Gamma-ray bursts and supernovae #Geometry #Globular cluster #Mode (computer interface) #Physics #RR Lyrae variable #Radiative transfer #Stars #Stellar evolution #Stellar, planetary, and galactic studies #Thermodynamics #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13060.x
Accepted for publication by MNRAS on 2008 February 01. The paper contains 4 figures and 8 tables
arxiv created 2008/02/01 · openalex publication_date 2008/03/29 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We derive the basic physical parameters of the field double-mode RR Lyrae star BS Com from its observed periods and the requirement of consistency between the pulsational and evolutionary constraints. By using the current solar-scaled horizontal branch evolutionary models of Pietrinferni et al. and our linear non-adiabatic purely radiative pulsational models, we get M/M⊙= 0.698 ± 0.004, log(L/L⊙) = 1.712 ± 0.005, Teff= 6840 ± 14 K, [Fe/H]=−1.67 ± 0.01, where the errors are standard deviations assuming uniform age distribution along the full range of uncertainty in age. The last two parameters are in a good agreement with the ones derived from the observed BVIC colours and the updated atlas9 stellar atmosphere models. We get Teff= 6842 ± 10 K, [Fe/H]=−1.58 ± 0.11, where the errors are purely statistical ones. It is remarkable that the derived parameters are nearly independent of stellar age at early evolutionary stages. Later stages, corresponding to the evolution towards the asymptotic giant branch, are most probably excluded because the required high temperatures are less likely to satisfy the constraints posed by the colours. We also show that our conclusions are only weakly sensitive to non-linear period shifts predicted by current hydrodynamical models.