Asteroseismology of the ZZ Ceti star KUV 11370+4222

被引：18
|
作者：
Su, J. [1 ,2 ,3 ]
Li, Y. [1 ,2 ]
Fu, J. -N. [4 ]
Li, C. [4 ]
机构：
[1] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China
[2] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China
[3] Univ Chinese Acad Sci, Beijing 100049, Peoples R China
[4] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 437卷 / 03期
基金：
中国国家自然科学基金;
关键词：
stars: individual: KUV 11370+4222; stars: oscillations; white dwarfs; BISYSTEM OSCILLATION-THEORY; STELLAR ASTROPHYSICS MESA; WHITE-DWARF STARS; INSTABILITY STRIP; EVOLUTION; VARIABLES; MODULES; PLANETS;
D O I：
10.1093/mnras/stt2069
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
KUV 11370+4222 is a ZZ Ceti star discovered in 1996, which has not been observed since then. We performed observations for KUV 11370+4222 in 2010 January. From the Fourier transform spectrum of the light curves, 10 independent modes are detected. We searched for the best-fitting model by using the observed periods to match the model periods and obtained it with the total mass of 0.625 M-circle dot, the effective temperature of 10 950 K, and the helium mass fraction and hydrogen mass fraction of 10(-2.2) and 10(-4.0), respectively. We have found a triplet of frequency split by rotation, which are l = 1 modes. Using the frequency shifts, we estimate a rotation period of 5.56 +/- 0.08 h. Besides it, another l = 1 mode is identified. The other observed periods are identified as l = 2 modes. At last we investigated the property of the mode trapping.
引用
收藏
页码：2566 / 2576
页数：11
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