WD1032+011, an inflated brown dwarf in an old eclipsing binary with a white dwarf

被引：29

作者：

Casewell, S. L. ^{[1
]}

Belardi, C. ^{[1
]}

Parsons, S. G. ^{[2
]}

Littlefair, S. P. ^{[2
]}

Braker, I. P. ^{[1
]}

Hermes, J. J. ^{[3
]}

Debes, J. ^{[4
]}

Vanderbosch, Z. ^{[5
,6
]}

Burleigh, M. R. ^{[1
]}

Gansicke, B. T. ^{[7
]}

Dhillon, V. S. ^{[2
,8
]}

Marsh, T. R. ^{[7
]}

Winget, D. E. ^{[5
,6
]}

Winget, K., I ^{[5
,6
]}

机构：

[1] Univ Leicester, Sch Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England

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

[3] Boston Univ, Dept Astron, Boston, MA 02215 USA

[4] Space Telescope Sci Inst, Baltimore, MD 21218 USA

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

[6] McDonald Observ, Ft Davis, TX 79734 USA

[7] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[8] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 497卷 / 03期

基金：

美国国家科学基金会;

关键词：

binaries: eclipsing; brown dwarfs; white dwarfs; SUBSTELLAR COMPANION; ATMOSPHERE; PHOTOMETRY;

D O I：

10.1093/mnras/staa1608

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the discovery of only the third brown dwarf known to eclipse a non-accreting white dwarf. Gaia parallax information and multicolour photometry confirm that the white dwarf is cool (9950 +/- 150 K) and has a low mass (0.45 +/- 0.05 M-circle dot), and spectra and light curves suggest the brown dwarf has a mass of 0.067 +/- 0.006 M-circle dot (70M(Jup)) and a spectral type of L5 +/- 1. The kinematics of the system show that the binary is likely to be a member of the thick disc and therefore at least 5-Gyr old. The high-cadence light curves show that the brown dwarf is inflated, making it the first brown dwarf in an eclipsing white dwarf-brown dwarf binary to be so.

引用

页码：3571 / 3580

页数：10

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