Growth of Jupiter: Enhancement of Core Accretion by a Voluminous Low-Mass Envelope
Gennaro D'Angelo, Stuart J. Weidenschilling, Jack J. Lissauer, Peter, Bodenheimer

TL;DR
This study models Jupiter's early formation, showing how a low-mass envelope significantly accelerates core growth through enhanced accretion of planetesimals, leading to a more massive core than without an envelope.
Contribution
It introduces a detailed calculation of Jupiter's formation considering dust coagulation, planetesimal size distribution, and envelope effects, highlighting the role of a voluminous low-mass envelope in core accretion.
Findings
Core mass reaches 7.3 Earth masses in 4x10^5 years.
Envelope growth surpasses core growth after initial formation.
Envelope presence increases accretion efficiency of planetesimals.
Abstract
We present calculations of the early stages of the formation of Jupiter via core nucleated accretion and gas capture. The core begins as a seed body of about 350 kilometers in radius and orbits in a swarm of planetesimals whose initial radii range from 15 meters to 50 kilometers. The evolution of the swarm accounts for growth and fragmentation, viscous and gravitational stirring, and for drag-assisted migration and velocity damping. During this evolution, less than 9% of the mass is in planetesimals smaller than 1 kilometer in radius; < ~25% is in planetesimals with radii between 1 and 10 kilometers; and < ~7% is in bodies with radii larger than 100 kilometers. Gas capture by the core substantially enhances the size-dependent cross-section of the planet for accretion of planetesimals. The calculation of dust opacity in the planet's envelope accounts for coagulation and sedimentation of…
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