http://arxiv.org/abs/1912.00405
We present seismic analysis of the prototype SX Phoenicis that aims at fitting the two radial-mode frequencies and the corresponding values of the bolometric flux amplitude (the parameter $f$), whose empirical values are derived from multi-coulor photometric observations. Seismic model that meets these conditions is of low mass, $M=1.05 M_\odot$, has moderately effective convection in the outer layers, described by the mixing length parameter $\alpha_{\rm MLT} \approx 0.7$, and the microturbulent velocity in the atmospheres of about $\xi_{\rm t}\approx 8$km/s. Such seismic studies of stars like SX Phe are very important for deriving constraints on outer-layer convection, because the object is on the border between very effective and ineffective convection.
J. Daszyńska-Daszkiewicz, P. Walczak, A. Pamyatnykh, et. al.
Tue, 3 Dec 19
70/90
Comments: 5 pages, 2 figures, Proceedings of the Vienna Conference “Stars and their Variability, )bserved from Space”