Dust growth and planet formation by disc fragmentation

Abstract

It is often argued that gravitational instability of realistic protoplanetary discs is only possible at distances larger than $\sim 50$ au from the central star, requiring high disc masses and accretion rates, and that therefore disc fragmentation results in the production of brown dwarfs rather than gas giant planets. However, the effects of dust growth on opacity can be very significant but have not been taken into account systematically in the models of fragmenting discs. We employ dust opacity that depends on both temperature and maximum grain size to evaluate analytically the properties of a critically fragmenting protoplanetary disc. We find that dust growth may promote disc fragmentation at disc radii as small as $\sim 30$ au. As a result, the critical disc masses and accretion rates are smaller, and the initial fragment masses are in the gas giant planet mass regime. While this suggests that formation of gas giant planets by disc fragmentation may be more likely than usually believed, we caution that numerical models of the process are needed to evaluate the effects not taken into account here, e.g., dust grain mobility and fragment evolution after disc fragmentation.

6 pages, 7 figures, accepted and published in MNRAS Letters

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