Metal loading of giant gas planets

Abstract

One of many challenges in forming giant gas planets via Gravitational disc Instability model (GI) is an inefficient radiative cooling of the pre-collapse fragments. Since fragment contraction times are as long at $10^5-10^7$ years, the fragments may be tidally destroyed sooner than they contract into gas giant planets. Here we explore the role of "pebble accretion" onto the pre-collapse giant planets and find an unexpected result. Despite larger dust opacity at higher metallicities, addition of metals actually accelerates -- rather than slows down -- collapse of high opacity, relatively low mass giant gas planets ($M_p$ below a few Jupiter masses). A simple analytical theory that explains this result exactly in idealised simplified cases is presented. The theory shows that planets with the central temperature in the range between $\sim$ 1000 to 2000K are especially sensitive to pebble accretion: addition of just $\sim 5$ to 10 % of metals by weight is sufficient to cause their collapse. These results show that dust grain physics and dynamics is essential for an accurate modelling of self-gravitating disc fragments and their near environments in the outer massive and cold protoplanetary discs.

published as 2015MNRAS.446..459N

References in corpus (5)

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Cited by in corpus (6)

• Dawes Review. The tidal downsizing hypothesis of planet formation
• Positive metallicity correlation for coreless giant planets
• The Effect of Protoplanetary Disk Cooling Times on the Formation of Gas Giant Planets by Gravitational Instability
• Pebble accretion in self-gravitating protostellar discs
• The paradox of youth for ALMA planet candidates
• Formation of Orion Fingers