  We present solutions for the accretion disks and boundary layers in
pre-main-sequence stars undergoing FU Orionis outbursts. These solutions differ
from earlier disk solutions in that they include a self-consistent treatment of
the boundary layer region. In a previous paper (Popham 1996), we showed that
these stars should stop accreting angular momentum once they spin up to modest
rotation rates. Here we show that for reasonable values of $\alpha$, these low
angular momentum accretion rate solutions fit the spectra and line profiles
observed in FU Orionis objects better than solutions with high rates of angular
momentum accretion. We find solutions which fit the observations of FU Orionis
and V1057 Cygni. These solutions have mass accretion rates of 2 and $1 \times
10^{-4} \msyr$, stellar masses of 0.7 and $0.5 \msun$, and stellar radii of
5.75 and $5.03 \rsun$, respectively. They also have modest stellar rotation
rates $8-9 \xss$, comparable to the observed rotation rates of T Tauri stars,
and angular momentum accretion rates of zero. This supports our earlier
suggestion that FU Orionis outbursts may regulate the rotation rates of T Tauri
stars.
