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Magnetospheric accretion models for T Tauri stars. 1: Balmer line profiles without rotationWe argue that the strong emission lines of T Tauri stars are generally produced in infalling envelopes. Simple models of infall constrained to a dipolar magnetic field geometry explain many peculiarities of observed line profiles that are difficult, if not impossible, to reproduce with wind models. Radiative transfer effects explain why certain lines can appear quite symmetric while other lines simultaneously exhibit inverse P Cygni profiles, without recourse to complicated velocity fields. The success of the infall models in accounting for qualitative features of observed line profiles supports the proposal that stellar magnetospheres disrupt disk accretion in T Tauri stars, that true boundary layers are not usually present in T Tauri stars, and that the observed 'blue veiling' emission arises from the base of the magnetospheric accretion column.
Document ID
19950034858
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hartmann, Lee
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA United States)
Hewett, Robert
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA United States)
Calvet, Nuria
(Centro de Investigaciones de Astronomia Merida, Venezuela)
Date Acquired
August 16, 2013
Publication Date
May 10, 1994
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 426
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
95A66457
Funding Number(s)
CONTRACT_GRANT: NAGW-2919
CONTRACT_GRANT: NSF INT-92-03015
Distribution Limits
Public
Copyright
Other

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