  Various interactions affect the population of close-in planets. Among them,
the tidal and magnetic interactions drive orbital decay and star-planet angular
momentum exchange, leading to stellar spin-up. As a result of the above
processes, a planet may initiate the mass transfer to the host star once it
encounters the Roche limit. Another mechanism providing substantial mass loss
is associated with the atmospheric escape caused by photoevaporation followed
by orbital expansion, which is thought to be important for hot Neptunes and
super-Earths. Thus, the fraction of the initial number of hot Jupiters may
transform into lower-mass planets through the Roche-lobe overflow (RLO) phase
and continue secular evolution under the effect of photoevaporation. In the
present paper, we compile the latest prescriptions for tidal and magnetic
migration and mass-loss rates to explore the dynamics of hot Jupiter systems.
We study how the implemented interactions shape the orbital architecture of
Jovian planets and whether their impact is enough to reproduce the
observational sample. Our models suggest that the tidal interaction is able to
generate the upper boundary of the hot Jupiter population in the
mass-separation diagram. To recreate the sub-Jovian desert, we need to make
additional assumptions regarding the RLO phase or the influence of the
protoplanetary disc's inner edge on the initial planetary location. According
to our estimates, 12-15% of hot Jupiters around solar-mass stars have been
engulfed or become lower-mass planets. 0.20-0.25% of the present-day giant
planet population undergoes decay intense enough to be detected with modern
facilities.
