  The terrestrial planets and the asteroids dominant in the inner asteroid belt
are water poor. However, in the protoplanetary disk the temperature should have
decreased below water condensation level well before the disk was
photoevaporated. Thus, the global water depletion of the inner Solar System is
puzling. We show that, even if the inner disk becomes cold, there cannot be
direct condensation of water. This is because the snowline moves towards the
Sun more slowly than the gas itself. The appearance of ice in a range of
heliocentric distances swept by the snowline can only be due to the radial
drift of icy particles from the outer disk. However, if a sufficiently massive
planet is present, the radial drift of particles is interrupted, because the
disk acquires a superKeplerian rotation just outside of the planetary orbit.
From this result, we propose that the precursor of Jupiter achieved about 20
Earth masses when the snowline was still around 3 AU. This effectively
fossilized the snowline at that location. Although cooling, the disk inside of
the Jovian orbit remained ice-depleted because the flow of icy particles from
the outer system was intercepted by the planet. This scenario predicts that
planetary systems without giant planets should be much more rich in water in
their inner regions than our system. We also show that the inner edge of the
planetesimal disk at 0.7AU, required in terrestrial planet formation models to
explain the small mass of Mercury and the absence of planets inside of its
orbit, could be due to the silicate condensation line, fossilized at the end of
the phase of streaming instability that generated the planetesimal seeds. Thus,
when the disk cooled, silicate particles started to drift inwards of 0.7AU
without being sublimated, but they could not be accreted by any pre-existing
planetesimals.
