A brown dwarf mass donor in an accreting binary

被引：91

作者：

Littlefair, S. P. ^{[1
]}

Dhillon, V. S.

Marsh, T. R.

Gaensicke, Boris T.

Southworth, John

Watson, C. A.

机构：

[1] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England

[2] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

来源：

SCIENCE | 2006年 / 314卷 / 5805期

基金：

英国科学技术设施理事会;

关键词：

D O I：

10.1126/science.1133333

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

A long-standing and unverified prediction of binary star evolution theory is the existence of a population of white dwarfs accreting from substellar donor stars. Such systems ought to be common, but the difficulty of finding them, combined with the challenge of detecting the donor against the light from accretion, means that no donor star to date has a measured mass below the hydrogen burning limit. We applied a technique that allowed us to reliably measure the mass of the unseen donor star in eclipsing systems. We were able to identify a brown dwarf donor star, with a mass of 0.052 +/- 0.002 solar mass. The relatively high mass of the donor star for its orbital period suggests that current evolutionary models may underestimate the radii of brown dwarfs.

引用

页码：1578 / 1580

页数：3

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