Hostname: page-component-78c5997874-dh8gc Total loading time: 0 Render date: 2024-11-19T08:30:34.329Z Has data issue: false hasContentIssue false
  • English
  • Français

Disk-loss and disk-renewal phases in classical Be stars – II. Detailed analysis of spectropolarimetric data

Published online by Cambridge University Press:  12 July 2011

Zachary H. Draper ,
John P. Wisniewski ,
Karen S. Bjorkman ,
Jon E. Bjorkman ,
Xavier Haubois ,
Alex C. Carciofi  and
Marilyn R. Meade
Zachary H. Draper
Affiliation:
Department of Astronomy, University of Washington, email: zhd@u.washington.edu, jwisnie@u.washington.edu
John P. Wisniewski
Affiliation:
Department of Astronomy, University of Washington, email: zhd@u.washington.edu, jwisnie@u.washington.edu
Karen S. Bjorkman
Affiliation:
Ritter Observatory, Department of Physics & Astronomy, University of Toledo
Jon E. Bjorkman
Affiliation:
Ritter Observatory, Department of Physics & Astronomy, University of Toledo
Xavier Haubois
Affiliation:
IAG, Universidade de Sao Paulo
Alex C. Carciofi
Affiliation:
IAG, Universidade de Sao Paulo
Marilyn R. Meade
Affiliation:
Space Astronomy Lab, University of Wisconsin-Madison
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In Wisniewski et al. (2010), paper I, we analyzed 15 years of spectroscopic and spectropolarimetric data from the Ritter and Pine Bluff Observatories of 2 Be stars, 60 Cygni and π Aquarii, when a transition from Be to B star occurred. Here we analyze the intrinsic polarization, where we observe loop-like structures caused by the rise and fall of the polarization Balmer Jump and continuum V-band polarization being mismatched temporaly with polarimetric outbursts. We also see polarization angle deviations from the mean, reported in paper I, which may be indicative of warps in the disk, blobs injected at an inclined orbit, or spiral density waves. We show our ongoing efforts to model time dependent behavior of the disk to constrain the phenomena, using 3D Monte Carlo radiative transfer codes.

Keywords

circumstellar matterstars: individual (π Aquarii, 60 Cygni)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 388 - 389
Copyright
Copyright © International Astronomical Union 2011

References

Carciofi, A. C. & Bjorkman, J. E. 2006, ApJ, 639, 1081Google Scholar
de Wit, W. J., Lamers, H. J. G. L. M., Marquette, J. B., & Beaulieu, J. P. 2006, A&A, 456, 1027Google Scholar
Wisniewski, J. P., Draper, Z. H., Bjorkman, K. S., Meade, M. R. et al. 2010, ApJ, 709, 1306 (paper I)Google Scholar