2005A&A...444..895S


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET14:17:54

2005A&A...444..895S - Astronomy and Astrophysics, volume 444, 895-904 (2005/12-4)

The qWR star HD 45166. I. Observations and system parameters.

STEINER J.E. and OLIVEIRA A.S.

Abstract (from CDS):

The binary star HD 45166 has been observed since 1922 but its orbital period has not yet been found. It is considered a peculiar Wolf-Rayet star, and its assigned classification has varied. For this reason we included the object as a candidate V Sge star and performed spectroscopy in order to search for its putative orbital period. High-resolution spectroscopic observations show that the spectrum, in emission and in absorption, is quite rich. The emission lines have great diversity of widths and profiles. The full widths at half maximum vary from 70km/s for the weakest lines up to 370km/s for the most intense ones. The hydrogen and helium lines are systematically broader than the CNO lines. Assuming that HD 45166 is a double-line spectroscopic binary, it presents an orbital period of P=1.596±0.003day, with an eccentricity of e=0.18±0.08. In addition, a search for periodicity using standard techniques reveals that the emission lines present at least two other periods, of 5 and 15 h. The secondary star has a spectral type of B7 V and, therefore, should have a mass of about M2=4.8M. Given the radial velocity amplitudes, we determined the mass of the hot (primary) star as M1=4.2±0.7M and the inclination angle of the system, i=0.77°±0.09°. As the eccentricity of the orbit is non zero, the Roche lobes increase and decrease as a function of the orbital phase. At periastron, the secondary star fills its Roche lobe. The distance to the star has been re-determined as d=1.3±0.2kpc and a color excess of E(B-V)=0.155±0.007 has been derived. This implies an absolute B magnitude of -0.6 for the primary star and -0.7 for the B7 star. We suggest that the discrete absorption components (DACs) observed in the ultraviolet with a periodicity similar to the orbital period may be induced by periastron events.

Abstract Copyright:

Journal keyword(s): techniques: spectroscopic - binaries: spectroscopic - stars: Wolf-Rayet

VizieR on-line data: <Available at CDS (J/A+A/444/895): table2.dat table3.dat table4.dat table5.dat>

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5868 1
2 HD 44498 * 06 22 22.5468492919 +08 19 36.455597968 8.16 8.76 8.82     B2.5V 19 0
3 HD 45166 WR* 06 26 19.1550467867 +07 58 28.071465236 9.05 9.81 9.88     WRpec+B8V 71 1
4 HD 102465 SB* 11 47 12.1012390115 -62 37 41.025185915   9.50 9.44     B9V 16 0
5 HD 103401 * 11 54 13.2076579007 -63 34 59.572832515   9.91 9.91     B5/7(V) 12 0
6 HD 104432 * 12 01 23.6453526091 -62 36 35.474210626   8.52 8.47     B9V 17 0
7 HD 104994 WR* 12 05 18.7203813373 -62 03 10.139083749 9.95 10.94 10.93 11.03   WN3p-w 156 0
8 V* WX Cen NL* 13 12 52.3763099360 -63 23 45.850925314   13.80 13.40     WN3h+WC4 44 0
9 WR 109 WR* 18 07 50.8974693468 -35 10 25.119230585           WN3 51 0
10 V* V Sge NL* 20 20 14.6910210608 +21 06 10.437296116   11.27 11.22 11.54   Be 201 0

    Equat.    Gal    SGal    Ecl

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2021.03.08-14:17:54

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