Exploring the physical properties of the $\gamma$ Dor binary star RX Dra with photometry and asteroseismology

TL;DR

This study models the binary star RX Dra using TESS data, identifying multiple g-mode frequencies, determining stellar parameters, and revealing the primary as a gamma Dor pulsator with a slower rotation than the orbit.

Contribution

First comprehensive modeling of RX Dra's light curve and g-mode frequencies, estimating stellar parameters and pulsation characteristics of both components.

Findings

Identified 16 dipole, 2 quadrupole, and 2 g-sextupole g-modes.

Determined primary as a gamma Dor pulsator in the main-sequence stage.

Estimated stellar parameters and convective core radius.

Abstract

We model the TESS light curve of the binary system RX Dra, and also first calculate a lot of theoretical models to fit the g-mode frequencies previously detected from the TESS series of this system. The mass ratio is determined to be $q$=0.9026$^{+0.0032}_{-0.0032}$. We newly found that there are 16 frequencies (F1-F7, F11-F20) identified as dipole g-modes, two frequencies (F21, F22) identified as quadrupole g-modes, and another two frequencies (F23, F24) identified as g-sextupole modes, based on these model fits. The primary star is newly determined to be a $\gamma$ Dor pulsator in the main-sequence stage with a rotation period of about 5.7$^{+0.7}_{-0.2}$ days, rotating slower than the orbital motion. The fundamental parameters of two components are firstly estimated as follows: $M_1$=1.53$^{+0.00}_{-0.17}$ M $_{\odot}$, $M_2$= 1.38$^{+0.18}_{-0.00}$ M $_{\odot}$, $T_1$=7240$^{+490}_{-44}$ K, $T_2$=6747$^{+201}_{-221}$ K, $R_1$=1.8288$^{+0.0260}_{-0.0959}$ R $_{\odot}$, $R_2$= 1.3075$^{+0.0450}_{-0.2543}$ R $_{\odot}$, $L_1$=8.2830$^{+1.8015}_{-0.6036}$ L $_{\odot}$ and $L_2$= 3.4145$^{+0.1320}_{-0.1843}$ L $_{\odot}$. Our results show that the secondary star is in the solar-like pulsator region of the H-R diagram, indicating that it could be a pulsating star of this type. Finally, the radius of the convective core of the primary star is estimated to be about 0.1403$^{+0.0206}_{-0.0000}$ R$_{\odot}$.