  Fourteen models are calculated with the shock velocity ranging from 200 to
330 km s$^{-1}$ and pre-shock hydrogen nucleon density ranging from $2.5\times
10^{12}$ to $4\times 10^{13}$ cm$^{-3}$. Among them the summed emergent flux of
all spectral lines accounts for about 0.1-0.3 of the total veiling flux. The
hydrogen Balmer continuum accounts for 0.17-0.1, while a nearly constant
fraction close to 0.5 comes from emission produced by the stellar atmosphere.
The main results derived from the veiling continuum energy distributions are
two strong correlations: 1) the Balmer jump (BJ) increases as $F_K$, the shock
kinetic energy flux, decreases; 2) at a fixed fraction of surface coverage by
accretion shocks $r_{\lambda}$, the ratio of veiling to photospheric continuum
flux at wavelength $\lambda$, decreases as $F_K$ decreases. Using the BJ -
$F_K$ and $r_{4500}$ - $F_K$ relations, the observed excess continua of 10 T
Tauri stars are modelled. For BP Tau and 3 Orion stars our accretion
luminosities are higher than published values by a factor of a few. For the 6
Chamaeleon I stars our observed accretion luminosities are about 27 - 78\%
higher than corresponding published values. Comparison of model results on the
HeI $\lambda$5876$~$flux with observed data indicates that, while those stars
with dominant $\lambda$5876$~$narrow components can be readily accounted for by
the calculated models, those with much stronger broad components cannot, and
suggests that for the latter objects the bulk of their excess continua at
5876$~$do not originate from accretion shocks.
