The closest extremely low-mass white dwarf to the Sun

被引:6
|
作者
Kawka, Adela [1 ]
Simpson, Jeffrey D. [2 ]
Vennes, Stephane [3 ]
Bessell, Michael S. [4 ]
Da Costa, Gary S. [4 ]
Marino, Anna F. [5 ,6 ]
Murphy, Simon J. [7 ]
机构
[1] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia
[2] UNSW Sydney, Sch Phys, Sydney, NSW 2052, Australia
[3] Australian Natl Univ, Inst Math Sci, Canberra, ACT 0200, Australia
[4] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
[5] Univ Padua, Dipartmento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy
[6] CISAS, Ctr Ateneo Studi & Attivita Spaziali Giuseppe Col, Via Venezia 15, I-35131 Padua, Italy
[7] Univ New South Wales, Sch Sci, Canberra, ACT 2600, Australia
基金
澳大利亚研究理事会; 欧盟地平线“2020”;
关键词
binaries: close; stars: individual: 2MASS J050051.85-093054.9; white dwarfs; SPECTRAL-ANALYSIS; KEPLER;
D O I
10.1093/mnrasl/slaa068
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the orbit and properties of 2MASS J050051.85-093054.9, establishing it as the closest (d approximate to 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with T-eff approximate to 10 500 K, log g approximate to 5.9, and, following evolutionary models, has a mass of approximate to 0.17 M-circle dot. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite (TESS) photometric time series reveals an orbital period of approximate to 9.5 h. Its high velocity amplitude (K approximate to 144 km s(-1)) produces a measurable Doppler beaming effect in the TESS light curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500-0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.
引用
收藏
页码:L129 / L134
页数:6
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