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The asteroid (4) Vesta, parent body of the Howardite-Eucrite-Diogenitemeteorites, is one of the first bodies that formed, mostly fromvolatile-depleted material, in the Solar System. The Dawn mission recentlyprovided evidence that hydrated material was delivered to Vesta, possibly in acontinuous way, over the last 4 Ga, while the study of the eucritic meteoritesrevealed a few samples that crystallized in presence of water and volatileelements. The formation of Jupiter and probably its migration occurred in theperiod when eucrites crystallized, and triggered a phase of bombardment thatcaused icy planetesimals to cross the asteroid belt. In this work, we study theflux of icy planetesimals on Vesta during the Jovian Early Bombardment and,using hydrodynamic simulations, the outcome of their collisions with theasteroid. We explore how the migration of the giant planet would affect thedelivery of water and volatile materials to the asteroid and we discuss ourresults in the context of the geophysical and collisional evolution of Vesta.In particular, we argue that the observational data are best reproduced if thebulk of the impactors was represented by 1-2 km wide planetesimals and ifJupiter underwent a limited (a fraction of au) displacement.

The Formation of Jupiter, the Jovian Early Bombardment and the Delivery of Water to the Asteroid Belt: The Case of (4) Vesta