Be stars are rapidly rotating B-type stars that eject mass into a circumstellar disk. The ionized gas in the disk is a source of hydrogen bound-free and free-free emission that becomes progressively stronger at longer wavelengths, so that in many cases the disk flux is comparable to the stellar flux in the near-infrared. The disks are large enough to be resolved by long baseline infrared interferometers. We present initial results using the Michigan Infrared Combiner (MIRC) at the CHARA Array on Mount Wilson to observe the Be star Zeta Tau. We computed simple geometric models that account for the asymmetry we detect in the disk. Our long term goal is to continue a multi-year monitoring campaign to follow the outward motions of disk enhancements from close to the star (in H-band) to farther out (in K-band and H-alpha). This work will be complemented by spectroscopy of the emission lines to investigate the development of asymmetric structures, such as spiral arms, in the disks.
Imaging the Disk of Zeta Tau Using the CHARA Array. Available from: http://www.researchgate.net/publication/252767955_Imaging_the_Disk_of_Zeta_Tau_Using_the_CHARA_Array [accessed Aug 27, 2015].
|Title of host publication||American Astronomical Society Meeting Abstracts 213|
|Publication status||Published - 1 Jan 2009|
|Name||Bulletin of the American Astronomical Society|