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In this paper we investigate theoretical pulsation models for the delta Scutistar 44 Tau. The star was monitored during several multisite campaigns whichconfirmed the presence of radial and nonradial oscillations. Moreover, itsexceptionally low rotational velocity makes 44 Tau particulary interesting foran asteroseismic study. Due to the measured log g value of 3.6 +/- 0.1, mainsequence and post-main sequence models have to be considered. We perform modeidentification based on photometric and spectroscopic data. A nonadiabaticpulsation code is used to compute models that fit the identified modes. Theinfluence of different opacity tables and element mixtures on the results istested. The observed frequencies of 44 Tau can be fitted in both the mainsequence and the post-main sequence evolutionary stage. Post-main sequencemodels are preferable as they fulfill almost all observational constraints (fitof observed frequencies, position in the HRD and instability range). Thesemodels can be obtained with normal chemical composition which is in agreementwith recent spectroscopic measurements. The efficiency of envelope convection(in the framework of the mixing-length theory) is predicted to be very low in44 Tau. We show that the results are sensitive to the choice between the OPALand OP opacities. While the pulsation models of 44 Tau computed with OPopacities are considerably too cool and too faint, the use of OPAL opacitiesresults in models within the expected temperature and luminosity range.

An asteroseismic study of the Delta Scuti star 44 Tau