2010A&A...519A..33G


Query : 2010A&A...519A..33G

2010A&A...519A..33G - Astronomy and Astrophysics, volume 519, A33-33 (2010/9-1)

Massive runaway stars in the Large Magellanic Cloud.

GVARAMADZE V.V., KROUPA P. and PFLAMM-ALTENBURG J.

Abstract (from CDS):

The origin of massive field stars in the Large Magellanic Cloud (LMC) has long been an enigma. The recent measurements of large offsets (∼100km/s) between the heliocentric radial velocities of some very massive (O2-type) field stars and the systemic LMC velocity provides a possible explanation of this enigma and suggests that the field stars are runaway stars ejected from their birthplaces at the very beginning of their parent cluster's dynamical evolution. A straightforward way to prove this explanation is to measure the proper motions of the field stars and to show that they are moving away from one of the nearby star clusters or OB associations. This approach is, however, complicated by the long distance to the LMC, which makes accurate proper motion measurements difficult. We used an alternative approach for solving the problem (first applied for Galactic field stars), based on the search for bow shocks produced by runaway stars. The geometry of detected bow shocks would allow us to infer the direction of stellar motion, thereby determining their possible parent clusters. In this paper we present the results of a search for bow shocks around six massive field stars that have been proposed as candidate runaway stars. Using archival Spitzer Space Telescope data, we found a bow shock associated with one of our programme stars, the O2V((f*)) star BI237, which is the first-ever detection of bow shocks in the LMC. Orientation of the bow shock suggests that BI237 was ejected from the OB association LH82 (located at ≃120pc in projection from the star). A by-product of our search is the detection of bow shocks generated by four OB stars in the field of the LMC and an arc-like structure attached to the candidate luminous blue variable R81 (HD 269128). The geometry of two of these bow shocks is consistent with the possibility that their associated stars were ejected from the 30Doradus star-forming complex. We discuss implications of our findings for the problem of the origin of runaway stars and the early dynamical evolution of star clusters.

Abstract Copyright:

Journal keyword(s): stars: kinematics and dynamics - stars: individual: BI237 - open clusters and associations: individual: LH82 - open clusters and associations: individual: R136(HD 38268) - stars: individual: HD269128

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 KMHK 268 Cl* 04 55 23.890 -66 26 34.34           ~ 7 0
2 SK -66 16 * 04 55 29.4146271192 -66 23 12.244739964 11.605 12.361 12.461   11.908 O9.7Ib 12 0
3 [L72] LH 10-3061 * 04 56 42.5074945536 -66 25 18.217550208 12.699 13.595 13.491   13.405 ON2III(f*) 25 0
4 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 247 0
5 NGC 1763 As* 04 56 51.5 -66 24 25     9.40     ~ 160 3
6 [ELS2006] N11 026 * 04 56 52.5287243472 -66 19 56.230847832 12.646 13.405 13.580     O2.5III(f*) 14 0
7 Brey 10a WR* 04 57 27.4544617632 -67 39 02.864000880 12.213 13.314 13.496   13.564 O2If*/WN5 54 1
8 HD 269128 s*b 05 10 22.7893360416 -68 46 23.816621928 9.77 10.52 10.412 10.29 10.268 B2.5Ieq 99 0
9 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16168 1
10 SK -68 86 * 05 27 41.7281579112 -68 50 18.833216352   12.25 13.04     OB 4 0
11 KMHK 933 Cl* 05 28 03.480 -68 48 36.37   11.70 11.65     ~ 14 0
12 HD 269687 WR* 05 31 25.5247745448 -69 05 38.556251700 10.86 11.78 11.87 12.05   WN11h 104 0
13 HD 269810 Em* 05 35 13.8977747136 -67 33 27.542449260   12.08 12.22 12.53   O3III(f*) 101 0
14 LH 82 As* 05 35 14 -67 33.8           ~ 24 0
15 SK -69 206 * 05 35 35.9718223824 -69 07 06.552258708   12.99 12.82 12.99   OB 11 0
16 NGC 2040 As* 05 36 00.7 -67 34 57     11.47     ~ 55 1
17 BI 237 * 05 36 14.6333257920 -67 39 19.168082640 12.865 13.790 13.830   13.948 O2V(f*) 33 0
18 NAME 30 Dor 016 * 05 37 08.8778548584 -69 07 20.375080464 12.623 13.584 13.546   13.816 O2IIIf* 40 0
19 BI 253 * 05 37 34.4595697440 -69 01 10.178659452 12.765 13.650 13.669   13.742 O2V(f*) 43 0
20 SK -68 137 * 05 38 24.6792593784 -68 52 32.951140752 12.243 13.274 13.346   13.242 OB 39 0
21 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1114 2
22 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1873 1
23 SK -69 279 Em* 05 41 44.6553703752 -69 35 14.905767516 12.079 12.787 12.842 13.03 12.619 OB 48 0
24 SK -69 288 * 05 42 41.4653304576 -69 03 44.592021108   12.67 12.73     OB 5 0
25 KMHK 1274 As* 05 42 42 -69 03.7     11.05     ~ 28 0
26 M 29 OpC 20 23 46 +38 29.2   7.30 6.6     ~ 231 0
27 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 878 0
28 BD+43 3654 s*b 20 33 36.0795027528 +43 59 07.364004504   11.24 10.06     O4If 55 0
29 [CPR2002] A37 * 20 36 04.4996355240 +40 56 13.040299752           O5V((f)) 22 0
30 * lam Cep s*b 22 11 30.5765111040 +59 24 52.154264880 4.55 5.29 5.05 4.77 4.62 O6.5I(n)fp 666 1

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2022.08.18-02:44:34

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