  Only a tiny fraction ~ 1% of stellar tidal disruption events (TDE) generate
powerful relativistic jets evidenced by luminous hard X-ray and radio
emissions. We propose that a key property responsible for both this
surprisingly low rate and a variety of other observations is the typically
large misalignment {\psi} between the orbital plane of the star and the spin
axis of the supermassive black hole (SMBH). Such misaligned disk/jet systems
undergo Lense-Thirring precession together about the SMBH spin axis. We find
that TDE disks precess sufficiently rapidly that winds from the accretion disk
will encase the system on large scales in a quasi-spherical outflow. We derive
the critical jet efficiency {\eta} > {\eta}crit for both aligned and misaligned
precessing jets to successfully escape from the disk-wind ejecta. As {\eta}crit
is higher for precessing jets, less powerful jets only escape after alignment
with the SMBH spin. Alignment can occur through magneto-spin or hydrodynamic
mechanisms, which we estimate occur on typical timescales of weeks and years,
respectively. The dominant mechanism depends on {\eta} and the orbital
penetration factor \b{eta}. Hence depending only on intrinsic parameters of the
event {{\psi},{\eta},\b{eta}}, we propose that each TDE jet can either escape
prior to alignment, thus exhibiting erratic X-ray light curve and two-component
radio afterglow (e.g., Swift J1644+57) or escape after alignment. Relatively
rapid magneto-spin alignments produce relativistic jets exhibiting X-ray
power-law decay and bright afterglows (e.g., AT2022cmc), while long
hydrodynamic alignments give rise to late jet escape and delayed radio flares
(e.g., AT2018hyz).
