The VLT-FLAMES Tarantula Survey: Multiplicity and Dynamics of the Massive Stars in 30 Dor

被引：0

作者：

Sana, H. ^{[1
]}

Dunstall, P. R. ^{[2
]}

Henault-Brunet, V. ^{[3
]}

Walborn, N. R. ^{[4
]}

de Koter, A. ^{[1
,5
]}

de Mink, S. E. ^{[4
]}

Dufton, P. L.

Evans, C. J. ^{[6
]}

Maiz Apellaniz, J. ^{[7
]}

Taylor, W. D. ^{[3
]}

Vink, J. S. ^{[8
]}

机构：

[1] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands

[2] Queens Univ Belfast, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland

[3] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

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

[5] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands

[6] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[7] CSIC, Inst Astroffs Andalucia, E-18008 Granada, Spain

[8] Armagh Observ, Armagh BT61 9DG, North Ireland

来源：

FOUR DECADES OF RESEARCH ON MASSIVE STARS | 2012年 / 465卷

关键词：

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中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first results on the multiplicity and dynamics of the OB star population in 30 Dor obtained in the framework of the VLT-FLAMES Tarantula Survey. Based on their radial velocity (RV) variations, we have identified over 100 O-type and about 160 B-type spectroscopic binaries. The observed spectroscopic binary fraction for the O and B stars in our sample is of the order 30-35%. Preliminary considerations on the binary detection rate suggest a true spectroscopic binary fraction of the order of 50%. The overall RV dispersion (sigma(RV)) of the O stars in the complete sample is about 10 km s(-1) but we note that the NGC 2060 and NGC 2070 regions show slightly different dynamical properties. We identified 17 O-type runaway candidates that show deviating RVs. One third of these candidates are On/nn/nnn stars, indicating a large rotational velocity. We show that the fast rotators have different RV properties than the average of the sample and are distributed throughout the field. This suggests a link between large rotation rate and peculiar RVs and, ultimately, the runaway phenomenon. Using the O stars observed within 25 ''(sigma 6 pc) from the core of R136, we obtain a preliminary upper limit of 7.5 kin s(-1) sigma(dyn). Given that this value has yet to be corrected down for contributions of non-detected long period binaries, this indicates that R136 is possibly a dynamically stable cluster.

引用

页码：284 / +

页数：3

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