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We calculate heavy element enrichment in a Jupiter-mass protoplanet formed bydisk instability at various radial distances from the star, consideringdifferent disk masses and surface density distributions. Although the availablemass for accretion increases with radial distance (a) for disk solid surfacedensity (sigma) functions sigma=sigma_0*a^(-alpha) with alpha < 2, theaccretion timescale is significantly longer at larger radial distances.Efficient accretion is limited to the first ~ 1E5 years of planetary evolution,when the planet is extended and before gap opening and type II migration takeplace. The accreted mass is calculated for disk masses of 0.01, 0.05 and 0.1M_sun with alpha = 1/2, 1, and 3/2. We show that a Jupiter-mass protoplanet canaccrete 1 to 110 M_earth of heavy elements, depending on the disk properties.Our results explain the large variation in heavy element enrichment found inextra-solar giant planets. Since higher disk surface density is found to leadto larger heavy element enrichment, our model results are consistent with thecorrelation between heavy element enrichment and stellar metallicity. Ourcalculations also suggest that Jupiter could have formed at a larger radialdistance than its current location while still accreting the mass of heavyelements predicted by interior models. We conclude that in the disk instabilitymodel the final composition of a giant planet is strongly determined by itsformation environment. The heavy element abundance of a giant planet does notdiscriminate between its origin by either disk instability or core accretion.

Heavy Element Enrichment of a Jupiter-mass Protoplanet as a Function of Orbital Location