  We study the migration of hot Jupiters orbiting solar-type pre-main sequence
and main sequence stars under the effect of tidal dissipation. The explored
range of stellar mass extends from 0.6 to 1.3 $M_{\odot}$. We apply recently
developed prescriptions which allow us to explore the orbital evolution over
the wide parameter space. Three types of tides are considered: equilibrium
tide, inertial waves, and gravity waves. We combine the results of our
simulations with the observed distribution of stellar and planetary parameters
to evaluate the infall rate of hot Jupiters in the Milky Way galaxy. In
particular, we find that, for 11 - 21% of the initial hot Jupiter population,
coalescence occurs before the host star's main sequence termination. If the
planet is massive enough, such an event can potentially be accompanied by a
powerful transient detectable with new facilities. Orbital decay by itself can
be observed through transit-timing variation. However, the obtained coalescence
rate in the Galaxy is too low (340 - 650 events per million years) to make
positive predictions about the observational possibility. Potentially
identifiable decaying systems formed by a star corresponding to a given mass
interval might be too rare to be detected with the modern space telescopes,
like TESS, within a 10-year baseline. At the same time, the forthcoming
missions, like PLATO, look more promising in this regard.
