Variable white dwarfs in TMTS: Asteroseismological analysis of a ZZ Ceti star, TMTS J17184064+2524314
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2024
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| author | Guo, Jincheng Chen, Yanhui Yang, Yonghui Wang, Xiaofeng Lin, Jie Ma, Xiao-Yu Xi, Gaobo Mo, Jun Filippenko, Alexei V. Brink, Thomas G. Zong, Weikai Yan, Huahui Zhao, Jingkun Zeng, Xiangyun Chen, Zhihao Esamdin, Ali Guo, Fangzhou Iskandar, Abdusamatjan Jiang, Xiaojun Li, Wenxiong Liu, Cheng Shi, Jianrong Song, Xuan Wang, Letian Xiang, Danfeng Yan, Shengyu Zhang, Jicheng |
| author_facet | Guo, Jincheng Chen, Yanhui Yang, Yonghui Wang, Xiaofeng Lin, Jie Ma, Xiao-Yu Xi, Gaobo Mo, Jun Filippenko, Alexei V. Brink, Thomas G. Zong, Weikai Yan, Huahui Zhao, Jingkun Zeng, Xiangyun Chen, Zhihao Esamdin, Ali Guo, Fangzhou Iskandar, Abdusamatjan Jiang, Xiaojun Li, Wenxiong Liu, Cheng Shi, Jianrong Song, Xuan Wang, Letian Xiang, Danfeng Yan, Shengyu Zhang, Jicheng |
| contents | The Tsinghua University-Ma Huateng Telescope for Survey (TMTS) has been constantly monitoring the northern sky since 2020 in search of rapidly variable stars. To find variable white dwarfs (WDs), the TMTS catalog is cross-matched with the WD catalog of Gaia EDR3, resulting in over 3000 light curves of WD candidates. The WD TMTS J17184064+2524314 (hereafter J1718) is the second ZZ~Ceti star discovered among these common sources. Based on the light curves from TMTS, follow-up photometric observations, and TESS, 10 periods and 3 combination periods are detected. A rotation period of $25.12\pm0.18$ hr is derived, according to the identified rotational splitting. Our spectroscopic observation indicates that this WD belongs to DA type with $T_{\rm eff}=11,670\pm604$ K, log $g=8.16\pm0.36$, $M = 0.70\pm0.23$ M$_{\odot}$, and age=$0.51\pm0.34$ Gyr. Based on core-parameterized asteroseismological model grids ($\geqslant$ 14 million), we derive a best-fit solution of $T_{\rm eff}=11,640\pm20$ K, log $g=8.267\pm0.008$, and $M = 0.750\pm0.005$ M$_{\odot}$ for J1718, consistent with the spectral fitting results. For this WD, the corresponding carbon and oxygen abundances in the core are 0.43 and 0.57, respectively. The distance derived from the intrinsic luminosity given by asteroseismology is $64\pm15$ pc, in accord with the distance of $70.1\pm0.2$ pc from Gaia DR3 within the uncertainties. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_14692 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Variable white dwarfs in TMTS: Asteroseismological analysis of a ZZ Ceti star, TMTS J17184064+2524314 Guo, Jincheng Chen, Yanhui Yang, Yonghui Wang, Xiaofeng Lin, Jie Ma, Xiao-Yu Xi, Gaobo Mo, Jun Filippenko, Alexei V. Brink, Thomas G. Zong, Weikai Yan, Huahui Zhao, Jingkun Zeng, Xiangyun Chen, Zhihao Esamdin, Ali Guo, Fangzhou Iskandar, Abdusamatjan Jiang, Xiaojun Li, Wenxiong Liu, Cheng Shi, Jianrong Song, Xuan Wang, Letian Xiang, Danfeng Yan, Shengyu Zhang, Jicheng Solar and Stellar Astrophysics The Tsinghua University-Ma Huateng Telescope for Survey (TMTS) has been constantly monitoring the northern sky since 2020 in search of rapidly variable stars. To find variable white dwarfs (WDs), the TMTS catalog is cross-matched with the WD catalog of Gaia EDR3, resulting in over 3000 light curves of WD candidates. The WD TMTS J17184064+2524314 (hereafter J1718) is the second ZZ~Ceti star discovered among these common sources. Based on the light curves from TMTS, follow-up photometric observations, and TESS, 10 periods and 3 combination periods are detected. A rotation period of $25.12\pm0.18$ hr is derived, according to the identified rotational splitting. Our spectroscopic observation indicates that this WD belongs to DA type with $T_{\rm eff}=11,670\pm604$ K, log $g=8.16\pm0.36$, $M = 0.70\pm0.23$ M$_{\odot}$, and age=$0.51\pm0.34$ Gyr. Based on core-parameterized asteroseismological model grids ($\geqslant$ 14 million), we derive a best-fit solution of $T_{\rm eff}=11,640\pm20$ K, log $g=8.267\pm0.008$, and $M = 0.750\pm0.005$ M$_{\odot}$ for J1718, consistent with the spectral fitting results. For this WD, the corresponding carbon and oxygen abundances in the core are 0.43 and 0.57, respectively. The distance derived from the intrinsic luminosity given by asteroseismology is $64\pm15$ pc, in accord with the distance of $70.1\pm0.2$ pc from Gaia DR3 within the uncertainties. |
| title | Variable white dwarfs in TMTS: Asteroseismological analysis of a ZZ Ceti star, TMTS J17184064+2524314 |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2401.14692 |