Far Ultraviolet Spectroscopic Explorer observations of the stellar winds of two O7 supergiants in the magellanic clouds

被引：28

作者：

Fullerton, AW

Crowther, PA

De Marco, O

Hutchings, JB

Bianchi, L

Brownsberger, KR

Massa, DL

Morton, DC

Rachford, BL

Snow, TP

Sonneborn, G

Tumlinson, J

Willis, AJ

机构：

[1] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada

[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21286 USA

[3] UCL, Dept Phys & Astron, London WC1E 6BT, England

[4] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V8X 4M6, Canada

[5] Osserv Astron Torino, I-10025 Pino Torinese, TO, Italy

[6] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[7] NASA, Goddard Space Flight Ctr, Raytheon Infomat Technol Serv, Greenbelt, MD 20771 USA

[8] NASA, Goddard Space Flight Ctr, Sci Serv, Greenbelt, MD 20771 USA

[9] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL | 2000年 / 538卷 / 01期

基金：

美国国家航空航天局;

关键词：

stars : early-type; stars; individual; (Sk-67; degrees; 111; Sk; 80); winds; outflows;

D O I：

10.1086/312787

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We compare the stellar wind features in far-UV spectra of Sk -67 degrees 111, an O7 Ib(f) star in the LMC, with Sk 80, an O7 Iaf+ star in the SMC. The most striking differences are that Sk 80 has a substantially lower terminal velocity, much weaker O VI absorption, and stronger S IV emission. We have used line-blanketed, hydrodynamic, non-LTE atmospheric models to explore the origin of these differences. The Tar-UV spectra require systematically lower stellar temperatures than previous determinations for O7 supergiants derived from plane-parallel, hydrostatic models of photospheric line profiles. At these temperatures, the O VI in Sk -67 degrees 111 must be due primarily to shocks in the wind.

引用

页码：L43 / L46

页数：4

共 29 条

[1] Measuring the ionization of O star winds [J].