The Structure and Emission of the Accretion Shock in T Tauri Stars II: the Ultraviolet Continuum Emission

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Abstract
We compare accretion shock models with optical and ultraviolet spectra of pre-main sequence stars to (1) make the first determinations of accretion rates in intermediate mass T Tauri stars from continuum emission, and (2) derive improved estimates of accretion rates and extinctions for continuum T Tauri stars. Our method extends the shock models developed by Calvet and Gullbring to enable comparisons with optical and archival International Ultraviolet Explorer ultraviolet spectra. We find good agreement between the observations and the model predictions, supporting the basic model of magnetospheric accretion shocks as well as previous determinations of accretion rates and interstellar reddening for the low mass T Tauri stars. The accretion rates determined for the intermediate-mass T Tauri stars agree well with values obtained through other methods that use near-infrared hydrogen line strengths (Muzerolle et al. 1998).

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