Orbital solution and fundamental parameters of σ Scorpii

被引：19

作者：

North, J. R. ^{[1
]}

Davis, J. ^{[1
]}

Tuthill, P. G. ^{[1
]}

Tango, W. J. ^{[1
]}

Robertson, J. G. ^{[1
]}

机构：

[1] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2007年 / 380卷 / 03期

关键词：

techniques : interferometric; binaries : spectroscopic; stars : fundamental parameters; stars : individual : sigma Sco; stars : variables : other;

D O I：

10.1111/j.1365-2966.2007.12188.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The first orbital solution for the spectroscopic pair in the multiple star system sigma Scorpii, determined from measurements with the Sydney University Stellar Interferometer, is presented. The primary component is of beta Cephei variable type and has been one of the most intensively studied examples of its class. The orbital solution, when combined with radial velocity results found in the literature, yields a distance of 174(-18)(+23) pc, which is consistent with, but more accurate than the Hipparcos value. For the primary component we determine 18.4 +/not superset of 5.4 M-circle dot, -4.12 +/not superset of 0.34 mag and 12.7 +/not superset of 1.8 R-circle dot for the mass, absolute visual magnitude and radius, respectively. A B1 dwarf spectral type and luminosity class for the secondary is proposed from the mass determination of 11.9 +/not superset of 3.1 M-circle dot and the estimated system age of 10 Myr.

引用

页码：1276 / 1284

页数：9

共 44 条

[1] High-precision elements of double-lined spectroscopic binaries from combined interferometry and spectroscopy -: Application to the β Cephei star β Centauri [J].