Complex asteroseismology of SX Phoenicis

Abstract

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, $M=1.05M_{\odot }$, has moderately effective convection in the outer layers, described by the mixing length parameter ${\alpha }_{\mathrm{MLT}}\approx 0.7$, and the microturbulent velocity in the atmospheres of about ${\xi }_{\mathrm{t}}\approx 8$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.

5 pages, 2 figures, Proceedings of the Vienna Conference "Stars and their Variability, )bserved from Space"

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