  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).
