Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4309d&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #43.09; Bulletin of the American Astronomical Society, Vol. 24, p.798
Astronomy and Astrophysics
Astronomy
Scientific paper
The current model of accreting T Tauri stars is that of a centrally condensed, optically revealed, object within a circumstellar disk. However, aspects of the T Tauri spectra, including the high velocity inverse P Cygni profiles observed in some YY Orionis stars, indicate that there is more to the picture. Recent estimates of magnetic field strengths associated with these stars give reason to believe that accretion may be magnetically dominated close to the star. If this is the case the disk will be disrupted close to the star and accretion follows the field lines, where differential rotation results in the 'twisting up' of the field lines. This configuration may well explain the observed spectra. After the work of Ghosh, Lamb and Pethick (1977) on accretion onto rotating magnetic neutron stars, I derived an improved, self-consistent velocity and density fields within the magnetosphere as a function of four parameters, the stellar angular velocity, the accretion rate, the angular momentum and the energy of the flow. Limits are placed on these parameters through observations as well as boundary conditions with the Keplerian disk. With this model determining the velocity and density fields, synthetic line profiles for the neutral sodium resonance doublet have been generated using radiation transfer techniques within the Sobolev approximation. This will be extended to include Lyman, Balmer, and Paschen lines from hydrogen. These theoretical spectra will then be compared to those observed in T Tauri stars. It is expected that the relationship between the spectral diagnostics and the theoretical modelling will define strong constraints on mass transport and accretion processes in T Tauri stars, providing an improved interpretation of their observational features, such as the inverse P Cygni profiles, which are poorly understood.
Calvet Nuria
Daugherty Debra A.
Hartmann Lee
Hewett Robert
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