2007A&A...469..707V


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.19CEST00:25:17

2007A&A...469..707V - Astronomy and Astrophysics, volume 469, 707-711 (2007/7-2)

Constraining GRB progenitor models by probing Wolf-Rayet wind geometries in the Large Magellanic Cloud.

VINK J.S.

Abstract (from CDS):

The favoured progenitors of long-duration gamma-ray bursts (GRBs) are rapidly rotating Wolf-Rayet (WR) stars. However, most Galactic WR stars are slow rotators, as stellar winds are thought to remove angular momentum. This poses a serious challenge to the collapsar model. Recent observations indicate that GRBs occur predominately in low metallicity (Z) environments, which may resolve the problem: lower Z leads to less mass loss, which may inhibit angular momentum removal, allowing WR stars to remain rotating rapidly until collapse. We wish to determine whether low Z WR stars rotate on average more rapidly than Galactic WR stars. We perform a Very Large Telescope (VLT) linear spectropolarimetry survey of WR stars in the low Z environment of the Large Magellanic Cloud (LMC) and compare our results with the Galactic sample of Harries et al. (1998MNRAS.296.1072H). We find that only 2 out of 13 (i.e. 15%) of LMC WR stars show line polarization effects, compared to a similarly low fraction of ∼15-20% for Galactic WR stars. The low incidence of line polarization effects in LMC WR stars suggests that the threshold metallicity where significant differences in WR rotational properties occur is below that of the LMC (Z∼0.5Z), possibly constraining GRB progenitor channels to this upper metallicity.

Abstract Copyright:

Journal keyword(s): stars: Wolf-Rayet - stars: early-type - techniques: polarimetric - gamma rays: bursts

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9091 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5375 1
3 Brey 15 WR* 05 05 08.4204405618 -70 22 45.124510417 13.572 14.47 14.62 14.81 14.714 WN3(h) 33 0
4 HD 269227 WR* 05 13 54.2798782060 -69 31 46.659015245 11.429 11.98 11.918 12.13 10.557 WN9/10+M2Ia 147 0
5 HD 269333 WR* 05 18 19.2101847037 -69 11 40.655834630 10.375 11.23 11.29 11.47 11.412 WN+BI 54 0
6 HD 35517 WR* 05 19 16.3520500120 -69 39 20.008292786 11.193 11.754 11.58 12.36 11.953 WC4+O5/6III/V+O 80 0
7 HD 269445 WR* 05 22 59.7854939490 -68 01 46.634598597 10.79 11.77 11.520 11.41 10.979 Ofpe/WN9 105 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14325 1
9 HD 36402 WR* 05 26 03.9637508160 -67 29 57.087055949   11.25 11.621 11.65   (WC) 130 0
10 HD 36521 WR* 05 26 30.241 -68 50 27.52   12.16 12.32 12.53   WC4+O6III/V+O 79 0
11 HD 269546 WR* 05 26 45.3199315750 -68 49 52.786974246 9.00 9.83 9.86 9.76 9.76 WN5b(h)+B3I 99 0
12 HD 269687 WR* 05 31 25.5247019885 -69 05 38.555025424 10.86 11.78 11.87 12.05   WN11h 92 0
13 HD 38029A WR* 05 36 54.633 -69 11 38.08           WC4 54 1
14 HD 38029 ** 05 36 55.17 -69 11 37.7 14.523 11.71 11.56 11.91 11.680 ~ 57 0
15 HD 38029B s*b 05 36 55.178 -69 11 37.47           B1Ia+ 54 1
16 HD 269891 WR* 05 37 49.0345689657 -69 05 08.219994930 11.791 9.447 11.39 11.55   WN6+B1Ia 62 0
17 RMC 139 WR* 05 38 42.3548071421 -69 04 58.201053806   12.04 11.94     O6.5Iafc+O6Iaf 84 0
18 HD 38282 WR* 05 38 53.3788120199 -69 02 00.896643506   10.98 11.11 11.26   WN5/6h+WN6/7h 145 1
19 HD 269928 WR* 05 38 57.0668705166 -69 06 05.660972436   12.02 11.94 12.00 11.58 WN6/7 115 0
20 V* FU Ori FU* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 685 1

    Equat.    Gal    SGal    Ecl

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2019.10.19-00:25:17

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