Warm (and hot) Jupiters (WJs/HJs) are Jovian-mass exoplanets orbiting
their host-stars on close in orbits (HJ separation: a<1; WJ: 0.1<a<1
AU). Such massive planets are thought to form far from their host star,
and later migrate inwards to their currently observed locations (CITE).
However, suggested disk migration and (tidal) high-eccentricity
migration models face major difficulties in reproducing HJ/WJs. Although
tidal migration models partially succeed in explaining the close-in HJs,
the wider orbits of WJs which put them beyond the influence of tides,
are difficult to explain in this context. Here we show that accounting
for the (currently neglected) pre - main-sequence (PMS) evolution of the
host stars fundamentally changes this picture. The larger radius of
early-stage PMS stars give rise to orders of magnitude stronger tidal
dissipation making tidal (high-eccentricity) migration effective at
significantly larger separations and shorter time. Moreover, the later
contraction of the PMS stars quenches the tidal effects, thereby
allowing for both initial fast tidal migration, and a later migration
"freeze-out", positioning the planet at intermediate distances from the
host-star and producing HJs/WJs-configurations inaccessible to
previously explored-scenarios. We conclude that the coupling of pre-MS
host-star evolution with planetary dynamics play is critical for
understanding the build-up of planetary systems and their architectures,
and can explain rapid production of both hot and warm Jupiters.