The eccentric short-period orbit of the supergiant fast X-ray transient HD 74194 (=LM Vel)

被引：19
|
作者：
Gamen, R. [1 ]
Barba, R. H. [2 ]
Walborn, N. R. [3 ]
Morrell, N. I. [4 ]
Arias, J. I. [2 ]
Maiz Apellaniz, J. [5 ]
Sota, A. [6 ]
Alfaro, E. J. [6 ]
机构：
[1] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, Inst Astrofis La Plata, CCT La Plata CONICET, RA-1900 La Plata, Buenos Aires, Argentina
[2] Univ La Serena, Dept Fis, La Serena, Chile
[3] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[4] Carnegie Observ, Las Campanas Observ, La Serena, Chile
[5] CSIC INTA, Ctr Astrobiol, Madrid 28691, Spain
[6] Inst Astrofis Andalucia CSIC, Granada 18008, Spain
来源：
ASTRONOMY & ASTROPHYSICS | 2015年 / 583卷
关键词：
binaries: spectroscopic; stars: early-type; stars: individual: HD 74194; IGR J08408-4503; NEUTRON-STAR; GALACTIC O; SPECTROSCOPIC SURVEY; MASS-DISTRIBUTION; SWIFT; BINARIES; PARAMETERS; CATALOG; SYSTEMS;
D O I：
10.1051/0004-6361/201527140
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Aims. We present the first orbital solution for the O-type supergiant star HD 74194, which is the optical counterpart of the supergiant fast X-ray transient IGR J08408-4503. Methods. We measured the radial velocities in the optical spectrum of HD 74194, and we determined the orbital solution for the first time. We also analysed the complex Ha profile. Results. HD 74194 is a binary system composed of an O-type supergiant and a compact object in a short-period (P = 9.5436 +/- 0.0002 d) and high-eccentricity (e = 0.63 +/- 0.03) orbit. The equivalent width of the Ha line is not modulated entirely with the orbital period, but seems to vary in a superorbital period (P = 285 +/- 10 d) nearly 30 times longer than the orbital one.
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页数：5
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