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The composition of Jupiter and the primordial distribution of the heavyelements are determined by its formation history. As a result, in order toconstrain the primordial internal structure of Jupiter the growth of the coreand the deposition and settling of accreted planetesimals must be followed indetail. In this paper we determine the distribution of the heavy elements inproto-Jupiter and determine the mass and composition of the core. We find thatwhile the outer envelope of proto-Jupiter is typically convective and has anhomogeneous composition, the innermost regions have compositional gradients. Inaddition, the existence of heavy elements in the envelope leads to much higherinternal temperatures (several times 10$^4$ K) than in the case of ahydrogen-helium envelope. The derived core mass depends on the actualdefinition of the core: if the core is defined as the region in which theheavy-element mass fraction is above some limit (say 0.5), then it can be muchmore massive ($\sim$ 15 M$_{\oplus}$) and more extended (10\% of the planet'sradius) than in the case where the core is just the region with 100\% heavyelements. In the former case Jupiter's core also consists of hydrogen andhelium. Our results should be taken into account when constructing internalstructure models of Jupiter and when interpreting the upcoming data from the{\it Juno} (NASA) mission.

Jupiter's formation and its primordial internal structure