A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS
By Y. Touhami, D. Gies, G. Schaefer, H. Mcalister, S. Ridgway, N. Richardson, R. Matson, E. Grundstrom, T. T. ten Brummelaar, P. J. Goldfinger and 4 more. 2013
213 citations recorded by the source corpus.
We report on a high angular resolution survey of circumstellar disks around 24 northern sky Be stars. The K-band continuum survey was made using the CHARA Array long baseline interferometer (baselines of 30–331 m). The interferometric visibilities were corrected for the flux contribution of stellar companions in those cases where the Be star is a member of a known binary or multiple system. For those targets with good (u, v) coverage, we used a four-parameter Gaussian elliptical disk model to fit the visibilities and to determine the axial ratio, position angle, K-band photospheric flux contribution, and angular diameter of the disk's major axis. For the other targets with relatively limited (u, v) coverage, we constrained the axial ratio, inclination angle, and/or disk position angle where necessary in order to resolve the degeneracy between possible model solutions. We also made fits of the ultraviolet and infrared spectral energy distributions (SEDs) to estimate the stellar angular diameter and infrared flux excess of each target. The mean ratio of the disk diameter (measured in K-band emission) to stellar diameter (from SED modeling) is 4.4 among the 14 cases where we reliably resolved the disk emission, a value which is generally lower than the disk size ratio measured in the higher opacity Hα emission line. We estimated the equatorial rotational velocity from the projected rotational velocity and disk inclination for 12 stars, and most of these stars rotate close to or at the critical rotational velocity.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/2f0510912a2243d5d82e859ebaeef38177d7e109
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In Astronomy and Astrophysics
Citations in the corpus
- Classical Be stars (2013, background): “However, spectropolarimetric observations by Vink et al. (2009) and the original experience of Be stars as a fairly inhomogeneous class suggest caution in ascribing such a nature to all of them, in particular for the earlier subtypes.”