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Magnetospheric accretion models for T Tauri stars. 1: Balmer line profiles without rotation
Hartmann, Lee; Hewett, Robert; Calvet, Nuria
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, US), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, US), AC(Centro de Investigaciones de Astronomia, Merida, Venezuela)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 2, p. 669-687 (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Balmer Series, Spectral Emission, Stellar Magnetic Fields, Stellar Magnetospheres, Stellar Mass Accretion, T Tauri Stars, Astronomical Models, Boundary Layers, Radiative Transfer, Stellar Envelopes, Stellar Physics
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We 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.

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