Exploring the physical properties of the Dor binary star RX Dra with photometry and asteroseismology
arXiv:2405.15940 · doi:10.1016/j.newast.2024.102234
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 =0.9026. 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 Dor pulsator in the main-sequence stage with a rotation period of about 5.7 days, rotating slower than the orbital motion. The fundamental parameters of two components are firstly estimated as follows: =1.53 M , = 1.38 M , =7240 K, =6747 K, =1.8288 R , = 1.3075 R , =8.2830 L and = 3.4145 L . 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 R.
arXiv comment13 pages,7 figures
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