  After the Tidal Disruption Event (TDE) of a star around a SuperMassive Black
Hole (SMBH), the bound stellar debris rapidly forms an accretion disk. If the
accretion disk is not aligned with the spinning SMBH's equatorial plane, the
disk will be driven into Lense-Thirring precession around the SMBH's spin axis,
possibly affecting the TDE's light curve. We carry out an eigenmode analysis of
such a disk to understand how the disk's warp structure, precession, and
inclination evolution are influenced by the disk's and SMBH's properties. We
find an oscillatory warp may develop as a result of strong non-Keplarian motion
near the SMBH. The global disk precession frequency matches the Lense-Thirring
precession frequency of a rigid disk around a spinning black hole within a
factor of a few when the disk's accretion rate is high, but deviates
significantly at low accretion rates. Viscosity aligns the disk with the SMBH's
equatorial plane over timescales of days to years, depending on the disk's
accretion rate, viscosity, and SMBH's mass. We also examine the effect of
fall-back material on the warp evolution of TDE disks, and find that the
fall-back torque aligns the TDE disk with the SMBH's equatorial plane in a few
to tens of days for the parameter space investigated. Our results place
constraints on models of TDE emission which rely on the changing disk
orientation with respect to the line of sight to explain observations.
