The complex asteroseismology of SX Phoenicis
Abstract
This paper presented a seismic analysis of the prototype SX Phoenicis, and was aimed at fitting the two radial-mode frequencies and the corresponding values of the bolometric flux amplitude (the parameter $f$), whose empirical values were derived from multi-coulor photometric observations. A seismic model that meets those conditions is of low mass (M=1.05 M_⊙), has moderately effective convection in the outer layers and described by the mixing-length parameter $\alpha_{\rm MLT} \approx 0.7$, and a microturbulent velocity in the atmospheres of about $\xi_{\rm t}\approx 8 \kms$. These seismic studies of a star like SX Phe are very important for deriving constraints on outer-layer convection because the object is borderline between very effective and ineffective convection.
- Publication:
-
Stars and their Variability Observed from Space
- Pub Date:
- 2020
- DOI:
- 10.48550/arXiv.1912.00405
- arXiv:
- arXiv:1912.00405
- Bibcode:
- 2020svos.conf...81D
- Keywords:
-
- Stars: evolution;
- atmospheres;
- asteroseismology;
- convection;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 5 pages, 2 figures, Proceedings of the Vienna Conference "Stars and their Variability, )bserved from Space"