OO Dra: an Algol-type binary formed through an extremely helium-poor mass accretion revealed by asteroseismology

Abstract

Based on the two-minutes TESS data, we analyzed intrinsic oscillations of the primary component and identified seven confident independent $\delta$ Scuti frequencies ($f_1$, $f_2$, $f_3$, $f_4$, $f_7$, $f_{11}$, and $f_{12}$). Both of single-star evolutionary models and mass-accreting models are computed to reproduce the $\delta$ Scuti freqiencies. Fitting results of them match well with each other. The stellar parameters of the primary star yielded by asteroseismology are $M$ = $1.92_{-0.02}^{+0.10}$ $M_{\odot }$, $Z$ = 0.011${}_{-0.001}^{+0.006}$, $R$ = $2.068_{-0.007}^{+0.050}$ $R_{\odot }$, $\log g$ = $4.090_{-0.002}^{+0.010}$, $T_{\mathrm{eff}}$ = $8346_{-320}^{+244}$ K, $L$ = $18.65_{-2.82}^{+3.31}$ $L_{\odot }$, which match well with the dynamic ones by the binary model. Furthermore, our asteroseismic results show that OO Dra is another Algol system that has just undergone the rapid mass-transfer stage. Fitting results of single-star evlutionary models indicate that the pulsator is helium-poor star with an age of 8.22${}_{-1.33}^{+0.12}$ Myr, and the further mass-accreting models show that the primary star looks like an almost unevolved star formed by an extremely helium-poor mass accretion in Case A evolutionary scenario.

25 pages, 8 figures, 7 tables. accepted for publication by ApJ. arXiv admin note: text overlap with arXiv:2004.09916

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