An Approximation for the Capture Radius of Gaseous Protoplanets

Abstract

Determining the heavy-element accretion rate of growing giant planets is crucial for understanding their formation and bulk composition. The solid (heavy-element) accretion rate should be carefully modeled during the various stages of giant planet formation and therefore, the planetary capture radius must be determined. In some simulations that model the heavy-element accretion rate, such as in N-body simulations, the presence of the gaseous envelope is either neglected, or treated in an over-simplified manner. In this paper, we present an approximation for the capture radius that does not require the numerical solution of the stellar structure equations. Our approximation for the capture radius works extremely well for various planetesimal sizes and compositions. We show that the commonly assumed constant density assumption for inferring the capture radius leads to a large error in the calculated capture radius and we therefore suggest that our approximation should be implemented in future simulations.

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Cited by in corpus (5)

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• A low accretion efficiency of planetesimals formed at planetary gap edges
• Heavy-element Accretion by Proto-Jupiter in a Massive Planetesimal Disk, Revisited
• The infrared colors of 51 Eridani b: micrometereoid dust or chemical disequilibrium?