We have modeled the emission in She first-overtone rotation-vibration
bands of CO from accretion disks and neutral winds. We compare our mod
els with high-resolution spectra of five objects: DG Tau, SVS 13, WL 1
6, NGC 2024 IRS 2, and S106 IRS 4. The emission from accretion disks w
ith accretion rates of similar to 10(-8) to 10(-7) M. yr(-1) successfu
lly reproduce the fluxes, the profiles, and the optical depths of the
observed spectra. We also find for several objects that the data are b
est reproduced by the disk model, with higher K-band extinctions to th
e central star than those measured by other methods. A simple wind mod
el can also account for the flux and line profile in a number of cases
, but fails to reproduce the high optical depth obtained by fitting lo
w-resolution data. Furthermore, unreasonably high mass-loss rates are
needed to reproduce the flux. However, if there are sources of heating
in the wind preventing it from cooling adiabatically, the CO emission
region is larger and lower mass-loss rates may be accommodated.