Internal rotation and buoyancy travel time of 60 gamma Doradus stars from uninterrupted TESS light curves spanning 352 days
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Description:<br> Electronic versions of Table A.1 and A.2 from the Appendix of<br> Garcia et al. (2022b), as well as all analysed g-mode period-spacing<br> patterns from this work. Abstract:<br> Context. Gamma Doradus (hereafter gamma Dor) stars are gravity-mode<br> pulsators whose periods carry information about the internal structure of<br> the star. These periods are especially sensitive to the internal rotation<br> and chemical mixing, two processes that are currently not well constrained<br> in the theory of stellar evolution.<br> Aims. We aim to identify the pulsation modes and deduce the internal<br> rotation and buoyancy travel time for 106 gamma Dor stars observed<br> by the TESS mission in its southern continuous viewing zone (hereafter<br> S-CVZ). We rely on 140 previously detected period-spacing patterns, that is,<br> series of (near-)consecutive pulsation mode periods.<br> Methods. We used the asymptotic expression to compute gravity-mode<br> frequencies for ranges of the rotation rate and buoyancy travel time that<br> cover the physical range in γ Dor stars. Those frequencies were fitted to<br> the observed period-spacing patterns by minimizing a custom cost function.<br> The effects of rotation were evaluated using the traditional approximation<br> of rotation, using the stellar pulsation code GYRE.<br> Results. We obtained the pulsation mode identification, internal rotation<br> and buoyancy travel time for 60 TESS gamma Dor stars. For the remaining 46<br> targets, the detected patterns are either too short or contained too many<br> missing modes for unambiguous mode identification, and longer light curves<br> are required. For the successfully analysed stars, we found that<br> period-spacing patterns from 1-yr long TESS light curves can constrain the<br> internal rotation and buoyancy travel time to a precision of 0.03 d^{−1} and<br> 400s, respectively, which is about half as precise as literature results<br> based on 4-yr Kepler light curves of gamma Dor stars.
