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Mass loss from pre-main-sequence accretion disks. I - The accelerating wind of FU OrionisWe present evidence that the wind of the pre-main-sequence object FU Orionis arises from the surface of the luminous accretion disk. A disk wind model calculated assuming radiative equilibrium explains the differential behavior of the observed asymmetric absorption-line profiles. The model predicts that strong lines should be asymmetric and blueshifted, while weak lines should be symmetric and double-peaked due to disk rotation, in agreement with observations. We propose that many blueshifted 'shell' absorption features are not produced in a true shell of material, but rather form in a differentially expanding wind that is rapidly rotating. The inference of rapid rotation supports the proposal that pre-main-sequence disk winds are rotationally driven.
Document ID
19930037604
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Calvet, Nuria
(Centro de Investigaciones de Astronomia Merida, Venezuela)
Hartmann, Lee
(NASA Headquarters Washington, DC United States)
Kenyon, Scott J.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 16, 2013
Publication Date
January 10, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 402
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A21601
Funding Number(s)
CONTRACT_GRANT: NAGW-511
Distribution Limits
Public
Copyright
Other

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