The VLT-FLAMES Tarantula Survey: Observational evidence for two distinct populations of massive runaway stars in 30 Doradus

被引：14

作者：

Sana, H. ^{[1
]}

Ramirez-Agudelo, O. H. ^{[2
]}

Henault-Brunet, V ^{[3
]}

Mahy, L. ^{[1
,21
]}

Almeida, L. A. ^{[4
,22
]}

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

Bestenlehner, J. M. ^{[6
]}

Evans, C. J. ^{[7
]}

Langer, N. ^{[8
]}

Schneider, F. R. N. ^{[9
,10
]}

Crowther, P. A. ^{[6
]}

de Mink, S. E. ^{[5
,11
]}

Herrero, A. ^{[12
]}

Lennon, D. J. ^{[12
]}

Gieles, M. ^{[13
,14
]}

Maiz Apellaniz, J. ^{[15
]}

Renzo, M. ^{[16
,17
]}

Sabbi, E. ^{[18
]}

van Loon, J. Th ^{[19
]}

Vink, J. S. ^{[20
]}

机构：

[1] Katholieke Univ Leuven, Inst Astron, Celestijnlaan 200D, B-3001 Leuven, Belgium

[2] German Aerosp Ctr DLR, Inst Protect Terr Infrastruct, Rathausallee 12, D-53757 St Augustin, Germany

[3] St Marys Univ, Dept Astron & Phys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[4] Univ Fed Rio Grande do Norte, Escola Ciencias & Tecnol, BR-59072970 Natal, RN, Brazil

[5] Univ Amsterdam, Anton Pannenkoek Astron Inst, NL-1090 GE Amsterdam, Netherlands

[6] Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England

[7] European Space Agcy ESA, ESA Off, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[8] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[9] Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany

[10] Heidelberg Univ, Astron Rech Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[11] Max Planck Inst Astrophys, Karl Schwarschild Str 1, D-85748 Garching, Germany

[12] Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38200, Spain

[13] ICREA, Pg Lluis Co 23, Barcelona 08010, Spain

[14] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti Franques 1, Barcelona 08028, Spain

[15] Ctr Astrobiol INTA, Campus ESAC,Camino Bajo del Castillo S-N, Madrid, Spain

[16] Flatiron Inst, Ctr Computat Astrophys, New York, NY 10010 USA

[17] Columbia Univ, Dept Phys, New York, NY 10027 USA

[18] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[19] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England

[20] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland

[21] Royal Observ Belgium, Av Circulaire 3, B-1180 Uccle, Belgium

[22] Univ Estado Rio Grande do Norte, Programa Posgrad Fis, BR-59610210 Mossoro, Brazil

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 668卷

基金：

欧洲研究理事会; 加拿大自然科学与工程研究理事会;

关键词：

stars: early-type; stars: massive; binaries: spectroscopic; stars: rotation; stars: kinematics and dynamics; galaxies: star clusters: individual: 30 Dor; O-TYPE; ORIGIN; VELOCITIES; FREQUENCY; EVOLUTION; CLUSTER; MODELS; EXCESS;

D O I：

10.1051/0004-6361/202244677

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The origin of massive runaway stars is an important unsolved problem in astrophysics. Two main scenarios have been proposed, namely: dynamical ejection or release from a binary at the first core collapse. However, their relative contribution remains heavily debated. Aims. Taking advantage of two large spectroscopic campaigns towards massive stars in 30 Doradus, we aim to provide observational constraints on the properties of the O-type runaway population in the most massive active star-forming region in the Local Group. Methods. We used radial velocity measurements of the O-type star populations in 30 Doradus obtained by the VLT-FLAMES Tarantula Survey and the Tarantula Massive Binary Monitoring to identify single and binary O-type runaways. Here, we discuss the rotational properties of the detected runaways and qualitatively compare the observations with expectations of ejection scenarios. Results. We identified 23 single and one binary O-type runaway objects, most of them located outside the main star-forming regions in 30 Doradus. We find an overabundance of rapid rotators (v(e) sin i>200 km s(-1)) among the runaway population, thus providing an explanation for the observed overabundance of rapidly rotating stars in the 30 Doradus field. Considerations of the projected rotation rates and runaway line-of-sight velocities reveal a conspicuous absence of rapidly rotating (v(e) sin i>210 km s(-1)), fast-moving (v(los)>60 km s(-1)) runaway stars in our sample, strongly suggesting the presence of two different populations of runaway stars: a population of rapidly spinning but slowly moving runaway stars and a population of fast-moving but slowly rotating ones. These are detected with a ratio close to 2:1 in our sample. Conclusions. We argue that slowly moving but rapidly spinning runaway stars result from binary ejections, while rapidly moving but slowly spinning runaways could result from dynamical ejections. Given that detection biases will more strongly impact the slow-moving runaway population, our results suggest that the binary evolution scenario dominates the current massive runaway star population in 30 Doradus.

引用

页数：7

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