2015A&A...575A..66N


C.D.S. - SIMBAD4 rel 1.7 - 2019.07.21CEST22:07:53

2015A&A...575A..66N - Astronomy and Astrophysics, volume 575A, 66-66 (2015/3-1)

Search for magnetic fields in particle-accelerating colliding-wind binaries.

NEINER C., GRUNHUT J., LEROY B., DE BECKER M. and RAUW G.

Abstract (from CDS):

Some colliding-wind massive binaries, called particle-accelerating colliding-wind binaries (PACWB), exhibit synchrotron radio emission, which is assumed to be generated by a stellar magnetic field. However, no measurement of magnetic fields in these stars has ever been performed. We aim at quantifying the possible stellar magnetic fields present in PACWB to provide constraints for models. We gathered 21 high-resolution spectropolarimetric observations of 9 PACWB available in the ESPaDOnS, Narval and HarpsPol archives. We analysed these observations with the least squares deconvolution method. We separated the binary spectral components when possible. No magnetic signature is detected in any of the 9 PACWB stars and all longitudinal field measurements are compatible with 0 G. We derived the upper field strength of a possible field that could have remained hidden in the noise of the data. While the data are not very constraining for some stars, for several stars we could derive an upper limit of the polar field strength of the order of 200 G. We can therefore exclude the presence of strong or moderate stellar magnetic fields in PACWB, typical of the ones present in magnetic massive stars. Weak magnetic fields could however be present in these objects. These observational results provide the first quantitative constraints for future models of PACWB.

Abstract Copyright:

Journal keyword(s): stars: magnetic field - stars: early-type - binaries: spectroscopic - stars: general

Simbad objects: 11

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Number of rows : 11

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 * del Ori Al* 05 32 00.40009 -00 17 56.7424 0.96 2.02 2.41 2.32 2.54 B0III+O9V 733 0
2 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 727 0
3 * 15 Mon Be* 06 40 58.65963 +09 53 44.7229 3.360 4.400 4.640   4.88 O7V+B1.5/2V 733 0
4 HD 93250 * 10 44 45.0270200315 -59 33 54.681395850 6.73 8.12 7.50 8.38   O4III(fc) 284 0
5 * eta Car Em* 10 45 03.5362075818 -59 41 04.053436648 6.37 6.82 6.21 4.90 4.41 OBepec 2136 0
6 HD 151804 s*b 16 51 33.7215112148 -41 13 49.928887100 4.45 5.29 5.22     O8Iaf 346 0
7 HD 152408 s*b 16 54 58.50567 -41 09 03.0964 5.17 5.92 5.77 7.00   O8Iape 342 0
8 HD 152804 * 16 56 55.2894582535 -31 59 23.335260337   8.79 8.68     B7III/IV 7 0
9 * 9 Sgr Em* 18 03 52.4455370104 -24 21 38.639393923 5.08 5.97 5.97 5.72 5.70 O4V((f))z 507 0
10 HD 167971 s*b 18 18 05.8954978252 -12 14 33.324312346 7.89 8.27 7.50 6.68 6.279 O8Iaf(n)+O4/5 264 0
11 HD 190918 WR* 20 05 57.3242972785 +35 47 18.153743699 6.11 6.88 6.75     WN5+O9I 333 0

    Equat.    Gal    SGal    Ecl

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2019.07.21-22:07:53

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