ACCURATE MASSES FOR THE PRIMARY AND SECONDARY IN THE ECLIPSING WHITE DWARF BINARY NLTT 11748

被引：20
作者：
Kilic, Mukremin [1 ]
Prieto, Carlos Allende [2 ]
Brown, Warren R. [1 ]
Agueeros, M. A. [3 ]
Kenyon, S. J. [1 ]
Camilo, Fernando [3 ]
机构：
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[2] Inst Astrofis Canarias, Tenerife 38205, Spain
[3] Columbia Univ, Dept Astron, New York, NY 10027 USA
来源：
ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 721卷 / 02期
基金：
美国国家科学基金会;
关键词：
stars: individual (NLTT 11748); stars: low-mass; white dwarfs; STARS; DISCOVERY; EVOLUTION; COMPANION; HELIUM;
D O I：
10.1088/2041-8205/721/2/L158
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We measure the radial velocity curve of the eclipsing detached white dwarf binary NLTT 11748. The primary exhibits velocity variations with a semi-amplitude of 273 km s(-1) and an orbital period of 5.641 hr. We do not detect any spectral features from the secondary star or any spectral changes during the secondary eclipse. We use our composite spectrum to constrain the temperature and surface gravity of the primary to be T(eff) = 8690 +/- 140 K and log g = 6.54 +/- 0.05, which correspond to a mass of 0.18 M(circle dot). For an inclination angle of 89 degrees.9 derived from the eclipse modeling, the mass function requires a 0.76 M(circle dot) companion. The merger time for the system is 7.2 Gyr. However, due to the extreme mass ratio of 0.24, the binary will most likely create an AM CVn system instead of a merger.
引用
收藏
页码：L158 / L162
页数：5
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