Journal
ASTRONOMICAL JOURNAL
Volume 140, Issue 6, Pages 1838-1849Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-6256/140/6/1838
Keywords
circumstellar matter; stars: emission-line, Be; stars: individual (zeta Tau); techniques: interferometric
Categories
Funding
- National Science Foundation [AST-0606861, AST-0352723, AST-0707927, AST-0807577, AST-0606958, AST-0908253]
- University of Michigan
- NASA [NNH09AK731]
- GSU College of Arts and Sciences
- W.M. Keck Foundation
- NASA Exoplanet Science Institute
- David and Lucile Packard Foundation
- Georgia State University
- Direct For Mathematical & Physical Scien [0807577] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [0807577] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009080] Funding Source: National Science Foundation
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We present interferometric observations of the Be star zeta Tau obtained using the MIRC beam combiner at the CHARA Array. We resolved the disk during four epochs in 2007-2009. We fit the data with a geometric model to characterize the circumstellar disk as a skewed elliptical Gaussian and the central Be star as a uniform disk. The visibilities reveal a nearly edge-on disk with an FWHM major axis of similar to 1.8 mas in the H band. The non-zero closure phases indicate an asymmetry within the disk. Interestingly, when combining our results with previously published interferometric observations of zeta Tau, we find a correlation between the position angle of the disk and the spectroscopic V/R ratio, suggesting that the tilt of the disk is precessing. This work is part of a multi-year monitoring campaign to investigate the development and outward motion of asymmetric structures in the disks of Be stars.
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