ON THE MULTIPLICITY OF THE ZERO-AGE MAIN-SEQUENCE O STAR HERSCHEL 36

被引：22

作者：

Arias, Julia I. ^{[1
]}

Barba, Rodolfo H. ^{[1
,2
]}

Gamen, Roberto C. ^{[3
,4
]}

Morrell, Nidia I. ^{[5
]}

Maiz Apellaniz, Jesus ^{[6
]}

Alfaro, Emilio J. ^{[6
]}

Sota, Alfredo ^{[6
]}

Walborn, Nolan R. ^{[7
]}

Moni Bidin, Christian ^{[8
]}

机构：

[1] Univ La Serena, Dept Fis, La Serena, Chile

[2] Consejo Nacl Invest Cient & Tecn, ICATE, San Juan, Argentina

[3] Consejo Nacl Invest Cient & Tecn, Inst Astrofis La Plata, La Plata, Buenos Aires, Argentina

[4] Univ Nac La Plata, Fac Cs Astron & Geofis, La Plata, Buenos Aires, Argentina

[5] Carnegie Observ, Campanas Observ, La Serena, Chile

[6] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain

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

[8] Univ Concepcion, Dept Astron, Concepcion, Chile

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 710卷 / 01期

关键词：

binaries: close; stars: early-type; stars: individual (Herschel 36); TIME-SERIES ANALYSIS; CLUSTER; M8;

D O I：

10.1088/2041-8205/710/1/L30

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the analysis of high-resolution optical spectroscopic observations of the zero-age main-sequence O star Herschel 36 spanning six years. This star is definitely a multiple system, with at least three components detected in its spectrum. Based on our radial-velocity (RV) study, we propose a picture of a close massive binary and a more distant companion, most probably in wide orbit about each other. The orbital solution for the binary, whose components we identify as O9 V and B0.5 V, is characterized by a period of 1.5415 +/- 0.0006 days. With a spectral type O7.5 V, the third body is the most luminous component of the system and also presents RV variations with a period close to 498 days. Some possible hypotheses to explain the variability are briefly addressed and further observations are suggested.

引用

页码：L30 / L34

页数：5

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