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Paper: Physical Properties of the Be Star Disks in h and χ Persei
Volume: 506, Bright Emissaries: Be Stars as Messengers of Star-Disk Physics
Page: 103
Authors: Boyer, A. N.; McSwain, M. V.
Abstract: We present new results in our on-going analysis of the B-type and Be star populations of the double open clusters h and χ Persei. As these clusters are rich in massive B-type and Be stars, they present an optimal location for studying the physical properties and variability of these disk structures. In previous analysis we have established physical properties, including V sin i, Teff, log gpolar, M, and R, for each B-type and Be star in our sample. In this work we continue our study of the cluster Be stars by examining the disk spectral energy distributions (SEDs) via observations from WEBDA, 2MASS, Spitzer, AKARI, and WISE. We also present multiple observations of Hα taken between 2009-2012 with the KPNO Coudé Feed, KPNO 2.1m, and WIRO telescopes. We use the Hα equivalent width model of Grundstrom & Gies and the infrared flux model of Touhami et al. to constrain the disk radii and densities for our Be star sample. Our results show a systematic, order of magnitude discrepancy between the disk densities predicted by the Grundstrom & Gies models, and those which appear to match with the observed infrared flux excess.
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