Polarization variability due to clumps in the winds of Wolf-Rayet stars
Li, Q. ( Dept. of Astronomy of Beijing Normal University, 100875, China ); Cassinelli, J. P. ( Dept. of Astronomy of University of Wisconsin-Madison, 53711, USA ); Brown, J. C. ( School of Physics and Astronomy of University of Glasgow, G12 8QQ, Scotland ); Ignace, R. ( Dept. of Physics and Astronomy of Eastern Tennessee State University, 37614, USA ) show affiliations
STELLAR POLARIMETRY: FROM BIRTH TO DEATH. AIP Conference Proceedings, Volume 1429, pp. 168-171 (2012).
Published in May 2012
Wolf-Rayet (WR) stars are understood to have clumpy winds [1]. Robert et al. [2] found a statistical relation between the variations of the polarization and the scattering light intensity, R = σp/σphot ~ 0.05. To explain this result, we propose a model in which clumps are ejected from the surface of WR stars uniformly in space with a Gaussian time interval distribution. According to the observed R along with the subpeaks on the emission lines of WR stars, we can obtain the parameters of the velocity law index β, and of the clump ejection rate in a flow time N. Also, the fraction η of the total mass loss rate contained in the clumps can be found from the observed polarization.
(c) 2012: American Institute of Physics
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