Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



  history
ID: 447991.0, MPI für Astronomie / Publikationen_mpia
The disk and environment of a young Altair analog: SAO 206462
Authors:Grady, C. A.; Schneider, G.; Sitko, M. L.; Williger, G. M.; Hamaguchi, K.; Brittain, S. D.; Ablordeppey, K.; Apai, D.; Beerman, L.; Carpenter, W. J.; Collins, K. A.; Fukagawa, M.; Hammel, H. B.; Henning, Th; Hines, D.; Kimes, R.; Lynch, D. K.; Pearson, R.; Russell, R. W.; Ménard, F.; Silverstone, M.; Smith, P.; Troutman, M.; Wilner, D.; Woodgate, B.
Language:English
Publisher:AIP, Springer
Place of Publication:New York
Date of Publication (YYYY-MM-DD):2009
Title of Proceedings:Cool Stars, Stellar Systems and the Sun
Start Page:385
End Page:388
Title of Series:AIP Conference Proceedings
Volume (in Series):1094
Name of Conference/Meeting:15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
Review Status:not specified
Audience:Experts Only
Abstract / Description:Proto-planetary and transitional disks which are detected in scattered light provide a critical test of the interpretation of circumstellar disks based on the IR spectral energy distribution (SED) alone. The disk inclination to the line-of-sight, outter radius, and surface brightness (SB) maps or radial SB distributions provided by spatially resolved imaging remove most of the degeneracies inherent in fitting IR SEDs without such observational constraints. We have imaged the disk of SAO 206462 (HD 135344 B) in 1.1 and 1.6 mum scattered light with HST/NICMOS and can trace the essentially face-on disk out to 1.05''. The cavity detected in sub-mm observations lies entirely under the NICMOS coronagraphic spot, a result consistent with the SED fitting if the star is at d = 140 pc. The SED had previously been classified as a Meeus Group I SED and interpreted as arising in a flared disk. Neither the 1.1 nor the 1.6 mum radial surface brightness profiles are consistent with a flared disk. A FUSE FUV spectrum demonstrates the presence of excess light in this system, confirming the accretion rate estimated from Brgamma. Collectively, these data strengthen the interpretation of this system as a transitional disk.
Free Keywords:stars; circumstellar matter; stellar rotation
Comment of the Author/Creator:Date: 2009, February 1, 2009
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISBN:978-0735406278 [ID No:1]
URL:http://adsabs.harvard.edu/abs/2009AIPC.1094..385G [ID No:2]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.