Magnetically induced termination of giant planet formation

Abstract

Here a physical model for terminating giant planet formation is outlined and compared to other methods of late-stage giant planet formation. As has been pointed out before, gas accreting into a gap and onto the planet will encounter the planetary dynamo-generated magnetic field. The planetary magnetic field produces an effective cross section through which gas is accreted. Gas outside this cross section is recycled into the protoplanetary disk, hence only a fraction of mass that is accreted into the gap remains bound to the planet. This cross section inversely scales with the planetary mass, which naturally leads to stalled planetary growth late in the formation process. We show that this method naturally leads to Jupiter-mass planets and does not invoke any artificial truncation of gas accretion, as has been done in some previous population synthesis models. The mass accretion rate depends on the radius of the growing planet after the gap has opened, and we show that so-called hot-start planets tend to become more massive than cold-start planets. When this result is combined with population synthesis models, it might show observable signatures of cold-start versus hot-start planets in the exoplanet population.

8 pages, 3 figures, accepted for publication in Astronomy & Astrophysics

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• Global Models of Planet Formation and Evolution
• On the Terminal Rotation Rates of Giant Planets
• Composition of Early Planetary Atmospheres I: Connecting Disk Astrochemistry to the Formation of Planetary Atmospheres
• Grain opacity and the bulk composition of extrasolar planets. I. Results from scaling the ISM opacity
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• Emission line variability of young 10-30 Mjup companions : I. The case of GQ Lup b and GSC 06214-00210 b
• Vertical gas accretion impacts the carbon-to-oxygen ratio of gas giant atmospheres
• A Theoretical Framework for the Mass Distribution of Gas Giant Planets forming through the Core Accretion Paradigm
• Formation of Planetary Populations II: Effects of Initial Disk Size & Radial Dust Drift
• Analytic Approach to the Late Stages of Giant Planet Formation
• Planet formation in the PDS 70 system: Constraining the atmospheric chemistry of PDS 70b and c
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• Connecting planet formation and astrochemistry: C/O and N/O of warm giant planets and Jupiter-analogs