Disk-Loss and Disk Renewal Phases in Classical Be Stars III. Modeling Effects of Disk Structure

Details Disk-Loss and Disk Renewal Phases in Classical Be Stars III. Modeling Effects of Disk Structure Disk-Loss and Disk Renewal Phases in Classical Be Stars III. Modeling Effects of Disk Structure

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733922d&link_type=abstract

American Astronomical Society, AAS Meeting #217, #339.22; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

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 Classical Be stars, 60 Cygni and π Aquarii. During this time both stars underwent a transition from Be to B star, whereby they lost their circumstellar disks. Since the mechanism for feeding these disks is not known, observing these stars when they transition between a Be phase and a normal B star phase can help constrain what leads to the disk growth and dissipation. Here we analyze the detailed behavior of the intrinsic polarization, and detect loop-like structures caused by the rise and fall of the polarization Balmer Jump and continuum V-band polarization being mismatched temporally during polarimetric outbursts. We demonstrate how these clockwise loops provide a unique diagnostic of the inner regions of these disks. We also see polarization angle deviations from the mean, reported in paper I, which may be indicative of warps in the disk, blobs being injected into the disk, or spiral density waves. We incorporate several types of disk structure to a 3D NLTE Monte Carlo radiation transfer code, such as blobs, rings, and scale height variations, to explore the origins causing the observed PA variations as well as their effect on the Balmer jump vs V-band polarization loops.

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