  Hot stars with hot Jupiters have a wide range of obliquities, while cool
stars with hot Jupiters tend to have low obliquities. An enticing explanation
for this pattern is tidal realignment of the cool host stars, although this
explanation assumes that obliquity damping occurs faster than orbital decay, an
assumption that needs further exploration. Here we revisit this tidal
realignment problem, building on previous work identifying a low-frequency
component of the time-variable tidal potential that affects the obliquity but
not the orbital separation. We adopt a recent empirically-based model for the
stellar tidal quality factor and its sharp increase with forcing frequency.
This leads to enhanced dissipation at low frequencies, and efficient obliquity
damping. We model the tidal evolution of 46 observed hot Jupiters orbiting cool
stars. A key parameter is the stellar age, which we determine in a homogeneous
manner for the sample, taking advantage of Gaia DR2 data. We explore a variety
of tidal histories and futures for each system, finding in most cases that the
stellar obliquity is successfully damped before the planet is destroyed. A
testable prediction of our model is that hot-Jupiter hosts with orbital periods
shorter than 2--3 days should have obliquities much smaller than $1^\circ$.
With the possible exception of WASP-19b, the predicted future lifetimes of the
planets range from $10^8$\,yr to more than $10^{10}$\,yr. Thus, our model
implies that these hot Jupiters are probably not in immediate danger of being
devoured by their host stars while they are on the main sequence.
