Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
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2024
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| _version_ | 1866910664309604352 |
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| author | Ding, Xu Ji, KaiFan Song, ZhiMing Liu, NianPing Xiong, JianPing Cheng, QiYuan Wang, ChuanJun Wang, JinLiang Wang, DeQing He, ShouSheng |
| author_facet | Ding, Xu Ji, KaiFan Song, ZhiMing Liu, NianPing Xiong, JianPing Cheng, QiYuan Wang, ChuanJun Wang, JinLiang Wang, DeQing He, ShouSheng |
| contents | TIC 157365951 has been classified as a $δ$ Scuti type by the International Variable Star Index (VSX). Through the spectra from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and its light curve, we further discovered that it is a binary system. This binary system comprises a red dwarf star and a compact star. Through the spectral energy distribution (SED) fitting, we determined the mass of the red dwarf star as $M_1 = 0.31 \pm 0.01 M_{\odot}$ and its radius as $R_1 = 0.414 \pm 0.004 R_{\odot}$. By fitting the double-peaked H${\rm α}$ emission, we derived the mass ratio of $q = 1.76 \pm 0.04 $, indicating a compact star mass of $M_2 = 0.54 \pm 0.01 M_{\odot}$. Using Phoebe to model the light curve and radial velocity curve for the detached binary system, we obtained a red dwarf star mass of $M_1 = 0.29 \pm 0.02 M_{\odot}$, a radius of $R_1 = 0.39 \pm 0.04 R_{\odot}$, and a Roche-lobe filling factor of $f = 0.995\pm0.129$, which is close to the $f=1$ expected for a semi-detached system. The Phoebe model gives a compact star mass $M_2 = 0.53 \pm 0.05 M_{\odot}$. Constraining the system to be semidetached gives $M_1 = 0.34 \pm 0.02 M_{\odot}$, $R_1 = 0.41 \pm 0.01 R_{\odot}$, and $M_2 = 0.62 \pm 0.03 M_{\odot}$. The consistency of the models is encouraging. The value of the Roche-lobe filling factor suggests that there might be ongoing mass transfer. The compact star mass is as massive as a typical white dwarf. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2410_18518 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star Ding, Xu Ji, KaiFan Song, ZhiMing Liu, NianPing Xiong, JianPing Cheng, QiYuan Wang, ChuanJun Wang, JinLiang Wang, DeQing He, ShouSheng Solar and Stellar Astrophysics TIC 157365951 has been classified as a $δ$ Scuti type by the International Variable Star Index (VSX). Through the spectra from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and its light curve, we further discovered that it is a binary system. This binary system comprises a red dwarf star and a compact star. Through the spectral energy distribution (SED) fitting, we determined the mass of the red dwarf star as $M_1 = 0.31 \pm 0.01 M_{\odot}$ and its radius as $R_1 = 0.414 \pm 0.004 R_{\odot}$. By fitting the double-peaked H${\rm α}$ emission, we derived the mass ratio of $q = 1.76 \pm 0.04 $, indicating a compact star mass of $M_2 = 0.54 \pm 0.01 M_{\odot}$. Using Phoebe to model the light curve and radial velocity curve for the detached binary system, we obtained a red dwarf star mass of $M_1 = 0.29 \pm 0.02 M_{\odot}$, a radius of $R_1 = 0.39 \pm 0.04 R_{\odot}$, and a Roche-lobe filling factor of $f = 0.995\pm0.129$, which is close to the $f=1$ expected for a semi-detached system. The Phoebe model gives a compact star mass $M_2 = 0.53 \pm 0.05 M_{\odot}$. Constraining the system to be semidetached gives $M_1 = 0.34 \pm 0.02 M_{\odot}$, $R_1 = 0.41 \pm 0.01 R_{\odot}$, and $M_2 = 0.62 \pm 0.03 M_{\odot}$. The consistency of the models is encouraging. The value of the Roche-lobe filling factor suggests that there might be ongoing mass transfer. The compact star mass is as massive as a typical white dwarf. |
| title | Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2410.18518 |