  It has recently been suggested that gravitomagnetic precession of the inner
part of the accretion disk, possibly driven by radiation torques, may be
responsible for some of the quasi-periodic X-ray brightness oscillations (QPOs)
at 20 - 300 Hz, observed in some low-mass binary systems containing accreting
neutron stars and black hole candidates. We have explored warp modes of
geometrically thin disks in the presence of gravitomagnetic and radiation
torques.
  We have found a family of overdamped, low-frequency gravitomagnetic (LFGM)
modes with precession frequencies lower than a certain critical frequency
\omega_{crit}, which is ~ 1 Hz for a compact object of solar mass. A radiation
warping torque can cause a few of the lowest-frequency LFGM modes to grow with
time, but even a strong radiation warping torque has essentially no effect on
the LFGM modes with frequencies > 10^{-4} Hz.
  We have also discovered a second family of high-frequency gravitomagnetic
(HFGM) modes with precession frequencies that range from $\omega_{crit}$ up to
slightly less than the gravitomagnetic precession frequency $\omega_{gm,i}$ of
a particle at the inner edge of the disk, which is 30 Hz if the disk extends
inward to the innermost stable circular orbit around a compact object of 2
solar masses with dimensionless angular momentum cJ/GM^2 = 0.2. The
highest-frequency HFGM modes are very localized spiral corrugations of the
inner disk and are weakly damped, with Q values 2-50.
  We discuss the implications of our results for the observability of
Lense-Thirring precession in X-ray binaries.
