A 12 MINUTE ORBITAL PERIOD DETACHED WHITE DWARF ECLIPSING BINARY

被引：128

作者：

Brown, Warren R. ^{[1
]}

Kilic, Mukremin ^{[1
]}

Hermes, J. J. ^{[2
]}

Allende Prieto, Carlos ^{[3
,4
]}

Kenyon, Scott J. ^{[1
]}

Winget, D. E. ^{[2
]}

机构：

[1] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA

[2] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[3] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[4] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 737卷 / 01期

基金：

美国国家科学基金会;

关键词：

binaries: close; binaries: eclipsing; gravitational waves; stars: individual (SDSS J065133.338+284423.37); white dwarfs; AM CVN STARS; LIGHT CURVES; MASS-TRANSFER; DISCOVERY; SYSTEM; PULSAR;

D O I：

10.1088/2041-8205/737/1/L23

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have discovered a detached pair of white dwarfs (WDs) with a 12.75 minute orbital period and a 1315 km s(-1) radial velocity amplitude. We measure the full orbital parameters of the system using its light curve, which shows ellipsoidal variations, Doppler boosting, and primary and secondary eclipses. The primary is a 0.25 M-circle dot tidally distorted helium WD, only the second tidally distorted WD known. The unseen secondary is a 0.55 M-circle dot carbon-oxygen WD. The two WDs will come into contact in 0.9 Myr due to loss of energy and angular momentum via gravitational wave radiation. Upon contact the systems may merge (yielding a rapidly spinning massive WD), form a stable interacting binary, or possibly explode as an underluminous Type Ia supernova. The system currently has a gravitational wave strain of 10(-22), about 10,000 times larger than the Hulse-Taylor pulsar; this system would be detected by the proposed Laser Interferometer Space Antenna gravitational wave mission in the first week of operation. This system's rapid change in orbital period will provide a fundamental test of general relativity.

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