  New high-resolution spectra of FU Ori, obtained with the HIRES spectrograph
at the Keck I telescope in 2003-2006, make it possible to compare the optical
line profiles with those predicted by the self-luminous accretion disk model. A
dependence of line width on excitation potential and on wavelength, expected
for a Keplerian disk, is definitely not present in the optical region, nor is
the line duplicity due to velocity splitting. The absorption lines observed in
the optical region of FU Ori must originate in or near the central object, and
here their profiles are shown to be those expected of a rigidly rotating
object. They can be fitted by a rapidly rotating (v sin i = 70 km/s)
high-luminosity G-type star having a large dark polar spot, with axis inclined
toward the line of sight. Over these years, the radial velocity of FU Ori has
remained constant to within +/-0.3 km/s, so there is no indication that the
star is a spectroscopic binary. These results apply to the optical region
($\lambda< 8800$ \AA); more distant, cooler regions of the disk contribute in
the infrared.
