2019MNRAS.484.5834C


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST08:50:46

2019MNRAS.484.5834C - Mon. Not. R. Astron. Soc., 484, 5834-5844 (2019/April-3)

Investigating the origin of the spectral line profiles of the Hot Wolf-Rayet Star WR 2.

CHENE A.-N., ST-LOUIS N., MOFFAT A.F.J., SCHNURR O., CROWTHER P.A., WADE G.A., RICHARDSON N.D., BARANEC C., ZIEGLER C.A., LAW N.M., RIDDLE R., RATE G.A., ARTIGAU E., ALECIAN E. (The BinaMIcS collaboration)

Abstract (from CDS):

The hot WN star WR 2 (HD 6327) has been claimed to have many singular characteristics. To explain its unusually rounded and relatively weak emission line profiles, it has been proposed that WR 2 is rotating close to break-up with a magnetically confined wind. Alternatively, the line profiles could be explained by the dilution of WR 2's spectrum by that of a companion. In this paper, we present a study of WR 2 using near-infrared AO imaging and optical spectroscopy and polarimetry. Our spectra reveal the presence of weak photospheric absorption lines from a B 2.5-4V companion, which however contributes only 5-10 per cent to the total light, suggesting that the companion is a background object. Therefore, its flux cannot be causing any significant dilution of the WR star's emission lines. The absence of intrinsic linear continuum polarization from WR 2 does not support the proposed fast rotation. Our Stokes V spectrum was not of sufficient quality to test the presence of a moderately strong organized magnetic field but our new modelling indicates that to confine the wind the putative magnetic field must be significantly stronger than was previously suggested sufficiently strong as to make its presence implausible.

Abstract Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: individual: WR 2 - stars: magnetic fields - stars: rotation - stars: winds, outflows - stars: Wolf-Rayet

Simbad objects: 16

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Number of rows : 16

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 * bet Cas dS* 00 09 10.68518 +59 08 59.2120 2.73 2.61 2.27 1.97 1.77 F2III 493 0
2 HD 4004 WR* 00 43 28.3971235391 +64 45 35.383738645 10.28 10.718 10.138     WN4-s 175 0
3 Ass Cas OB 1 As* 01 00 +61.5           ~ 38 0
4 TYC 4017-1829-2 * 01 05 22.9735156679 +60 25 05.071633942           ~ 1 0
5 HD 6327 WR* 01 05 23.0143603 +60 25 18.965197   11.49 11.33     WN2-w 104 0
6 * phi Cas s*y 01 20 04.9146181556 +58 13 53.812633124 6.15 5.66 4.98 4.34 3.78 F0Ia 252 0
7 V* CC Cas bL* 03 14 05.3362562931 +59 33 48.488947721 7.07 7.56 7.08     O8.5III(n)((f)) 264 0
8 HD 21447 * 03 30 00.1834708229 +55 27 06.513970075 5.160 5.140 5.090 5.01 5.02 A1Va 121 0
9 HD 32109 WR* 04 55 31.3419672483 -67 30 02.683822100 12.893 13.46 13.81 13.95 13.512 WN4b 68 0
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14325 1
11 Brey 42 WR* 05 30 02.4528094820 -68 45 18.387450916 14.146 14.939 15.201   15.213 WN3b 28 0
12 Brey 70a WR* 05 37 35.7057107734 -69 08 40.253264123 17.387 17.957 16.924   16.324 WN4b/WCE 24 0
13 HD 269908 WR* 05 38 27.7012451364 -69 29 58.547130741 14.243 14.40 14.29 14.59 14.230 WN4b 39 0
14 HD 50896 WR* 06 54 13.0440847499 -23 55 42.020318514 5.74 6.63 6.91 7.74   WN4b 735 0
15 * zet Pup BY* 08 03 35.04754 -40 00 11.3321 0.89 1.98 2.25 2.36 2.58 O4I(n)fp 1083 1
16 HD 211564 WR* 22 16 24.0322637172 +55 37 36.763974776   11.72 11.61     WN3(h)-w 110 0

    Equat.    Gal    SGal    Ecl

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2019.10.21-08:50:46

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