On the Near‐Infrared Size of Vega | Zendy

David R. Ciardi | Zendy; Gerald van Belle | Zendy; Rachel Akeson | Zendy; R. R. Thompson | Zendy; Elizabeth A. Lada | Zendy; Steve B. Howell | Zendy

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On the Near‐Infrared Size of Vega

Author(s) -

David R. Ciardi,

Gerald van Belle,

Rachel Akeson,

R. R. Thompson,

Elizabeth A. Lada,

Steve B. Howell

Publication year - 2001

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/322345

Subject(s) - vega , debris disk , debris , physics , astrophysics , atmosphere (unit) , infrared , flux (metallurgy) , circumstellar disk , stellar atmosphere , interferometry , astronomy , stars , planetary system , meteorology , materials science , metallurgy

Near-infrared (2.2 um) long baseline interferometric observations of Vega are presented. The stellar disk of the star has been resolved, and the data have been fitted with a limb darkened stellar disk of diameter Theta_{LD} = 3.28 +/- 0.01 mas. The derived effective temperature is T_eff = 9553 +/- 111 K. However, the residuals resulting from the stellar disk model appear to be significant and display organized structure. Instrumental artifacts, stellar surface structure, stellar atmosphere structure, and extended emission/scattering from the debris disk are discussed as possible sources of the residuals. While the current dataset cannot uniquely determine the origin of the residuals, the debris disk is found to be the most likely source. A simple debris disk model, with 3-6% of Vega's flux emanating from the disk at r < 4 AU, can explain the residuals

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