Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23...13o&link_type=abstract
Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 13-14
Other
Scientific paper
The star HD 45166 has been observed since 1922 but its orbital period has not yet been found. Its classification has been varying along the years about the idea that it is a peculiar Wolf-Rayet star. For this reason we included this star as a candidate to the class of V Sge stars. High-resolution spectroscopic observations, done at LNA and ESO, show that the spectrum is quite rich. We determined that HD 45166 is a double spectroscopic binary with an orbital period of 1.596 +/- 0.003 days, presenting an eccentricity of e = 0.18 +/- 0.08. In addition, the emission lines present at least two other periods, of 5 hours and of 15 hours which, we suggest, are caused by non-radial oscillations detected in the wind but originated on the surface of the primary star. The secondary star has a B8 V spectral type and, therefore, should have mass about M2 = 4 M¤. Given the radial velocity amplitudes, we determined the mass of the hot star as being M1 = 3.5 +/- 0.7 M¤ and the inclination angle of the system, i = 0.77° +/- 0.09°. The hot component is probably in the phase of central Helium burning. As the eccentricity of the orbit is non zero, the Roche lobes increase and decrease in size as a function of the orbital phase. At periastron, the secondary star fills its Roche lobe and transfers matter to the hot star. This mass transfer is associated to transient jets, which are observed as two satellite emissions with v = +/- 1380 km/s in the line of He II 4686Å. With the characteristics described in this work we confirm that the best form of classifying HD 45166 is as a qWR, that is, a "quasi" Wolf-Rayet or a low-mass WR, with a B8 V companion.
Oliveira Alexandre S.
Steiner Joao Evangelista
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