Properties and asteroseismological analysis of a new ZZ ceti discovered by TMTS

Author:

Guo Jincheng1ORCID,Chen Yanhui2ORCID,Wang Xiaofeng13,Lin Jie3ORCID,Xi Gaobo3,Mo Jun3,Filippenko Alexei V4,Brink Thomas4,Ma Xiao-Yu5,Zong Weikai5,Yang Yong67ORCID,Zhao Jingkun67,Zeng Xiangyun8,Chen Zhihao3,Esamdin Ali9,Guo Fangzhou3,Iskandar Abdusamatjan9,Jiang Xiaojun67,Li Wenxiong10,Liu Cheng1,Shi Jianrong67,Song Xuan1,Wang Letian9,Xiang Danfeng3ORCID,Yan Shengyu3,Zhang Jicheng5,Yang Yonghui211

Affiliation:

1. Department of Scientific Research , Beijing Planetarium, Xizhimenwai Street, Beijing 100044, China

2. Institute of Astrophysics, Chuxiong Normal University , Chuxiong 675000, China

3. Physics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, China

4. Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA

5. Department of Astronomy, Beijing Normal University , Beijing 100875, China

6. Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, China

7. Department of Astronomy, University of Chinese Academy of Sciences , Beijing 100049, China

8. Center for Astronomy and Space Sciences, China Three Gorges University , Yichang 443000, China

9. Xinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi 830011, China

10. The School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, Israel

11. Faculty of Science, Kunming University of Science and Technology , Kunming 650093, China

Abstract

ABSTRACT Tsinghua University-Ma Huateng Telescope for Survey (TMTS) aims to discover rapidly evolving transients by monitoring the northern sky. The TMTS catalogue is cross-matched with the white dwarf (WD) catalogue of Gaia EDR3, and light curves of more than a thousand WD candidates are obtained so far. Among them, the WD TMTS J23450729+5813146 is one interesting common source. Based on the light curves from the TMTS and follow-up photometric observations, periods of 967.113, 973.734, 881.525, 843.458, 806.916, and 678.273 s are identified. In addition, the TESS observations suggest a 3.39-h period but this can be attributed to the rotation of a comoving M dwarf located within 3 arcsec. The spectroscopic observation indicates that this WD is DA type with Teff = 11 778 ± 617 K, log g = 8.38 ± 0.31, mass = 0.84 ± 0.20 M⊙, and age = 0.704 ± 0.377 Gyr. Asteroseismological analysis reveals a global best-fitting solution of Teff = 12 110 ± 10 K and mass = 0.760 ± 0.005 M⊙, consistent with the spectral fitting results, and oxygen and carbon abundances in the core centre are 0.73 and 0.27, respectively. The distance derived from the intrinsic luminosity given by asteroseismology is 93 parsec, which is in agreement with the distance of 98 parsec from Gaia DR3. Additionally, kinematic study shows that this WD is likely a thick-disc star. The mass of its zero-age main sequence is estimated to be 3.08 M⊙ and has a main sequence plus cooling age of roughly 900 Myr.

Funder

National Natural Science Foundation of China

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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