  We present new high resolution (R=18,000) near-infrared spectroscopic
observations of a sample of classical FU Orionis stars (FUors) and other young
stars with FUor characteristics that are sources of Herbig-Haro flows. Spectra
are presented for the region 2.203 - 2.236 microns which is rich in absorption
lines sensitive to both effective temperatures and surface gravities of stars.
Both FUors and FUor-like stars show numerous broad and weak unidentified
spectral features in this region. Spectra of the 2.280 - 2.300 micron region
are also presented, with the 2.2935 micron v=2-0 CO absorption bandhead being
clearly the strongest feature seen in the spectra all FUors and Fuor-like
stars. A cross-correlation analysis shows that FUor and FUor-like spectra in
the 2.203 - 2.236 micron region are not consistent with late-type dwarfs,
giants, nor embedded protostars. The cross-correlations also show that the
observed FUor-like Herbig-Haro energy sources have spectra that are
substantively similar to those of FUors. Both object groups also have similar
near-infrared colors. The large line widths and double-peaked nature of the
spectra of the FUor-like stars are consistent with the established accretion
disk model for FUors, also consistent with their near-infrared colors. It
appears that young stars with FUor-like characteristics may be more common than
projected from the relatively few known classical FUors.
