http://arxiv.org/abs/2305.06840
To decipher complex patterns of gravity-mode period spacings observed for intermediate-mass main-sequence stars is an important step toward the better understanding of the structure and dynamics in the deep radiative region of the stars. In this study, we apply JWKB approximation to derive a semi-analytical expression of the g-mode period spacing pattern, for which the gradient in the Brunt-V\”ais\”al\”a frequency is taken into account. The formulation includes a term $P^{-1} B_{\star}$, where $P$ and $B_{\star}$ represent the g-mode period and degree of the structural variation, the latter of which especially is related to the steepness of the gradient of the Brunt-V\”ais\”al\”a frequency. Tests with 1-dimensional stellar models show that the semi-analytical expression derived in this study is useful for inferring the degree of the structural variation $B_{\star}$ with accuracy of $\sim 10\,\%$ in the case of relatively massive intermediate-mass models with the mass $M$ larger than $3 \,M_{\odot}$. The newly formulated expression will possibly allow us to put further constraints on, e.g., mixing processes inside intermediate-mass main-sequence g-mode pulsators such as $\beta$ Cep, SPB, and $\gamma$ Dor stars that have been principal targets in asteroseismology.
Y. Hatta
Fri, 12 May 23
50/53
Comments: 20 pages, 15 figures, 1 table, accepted for publication in ApJ