Thermal Processing of Solids Encountering a Young Jovian Core

Abstract

Jupiter's enhancement in nitrogen relative to hydrogen when compared to the Sun has been interpreted as evidence that its early formation occurred beyond the N${}_2$ snowline ($\sim$ 20-40 AU). However, the rapid growth necessary to form Jupiter before the dissipation of the solar nebula would lead to the forming planet's core reaching very high temperatures ($>$1000 K), which would lead to it warming its surroundings. Here, we explore the effects of a luminous planetary core on the solids that it ultimately accretes. We find that a critical transition occurs where very hot (rapidly accreting) cores drive off volatiles prior to accretion, while cool cores (slowly accreting) are able to inherit volatile rich solids. Given Jupiter's nitrogen enrichment, if it formed beyond the N${}_2$ snowline, its core could not have accreted solids at a rate above 10${}^{-10}$ M${}_{\odot }$ yr${}^{-1}$. Our results suggest that either Jupiter formed in more distal regions of the solar nebula, or nitrogen loss was suppressed, either by its incorporation in more refractory carriers or because it was trapped within ices which devolatilized at higher temperatures.

Accepted to the Astrophysical Journal, 11 pages, 5 figures

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Cited by in corpus (5)

• Atmospheric Recyling of Volatiles by Pebble-Accreting Planets
• Chemical footprints of giant planet formation. Role of planet accretion in shaping the C/O ratio of protoplanetary disks
• Enrichment of Jupiter's atmosphere by late planetesimal bombardment
• Three-dimensional transport of solids in a protoplanetary disk containing a growing giant planet
• Locked In Ice: how Pebble Drift and Volatile Entrapment can Significantly Impact Carbon and Oxygen Ratios in Evolving Protoplanetary Discs