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

Tidal migration of hot Jupiters: introducing the impact of gravity wave dissipation