The role of drag and gravity on dust concentration in a gravitationally unstable disc

Author:

Rowther Sahl123ORCID,Nealon Rebecca12ORCID,Meru Farzana12ORCID,Wurster James4ORCID,Aly Hossam56ORCID,Alexander Richard3ORCID,Rice Ken78ORCID,Booth Richard A9ORCID

Affiliation:

1. Centre for Exoplanets and Habitability, University of Warwick , Coventry CV4 7AL , UK

2. Department of Physics, University of Warwick , Coventry CV4 7AL , UK

3. School of Physics and Astronomy, University of Leicester , Leicester LE1 7RH , UK

4. Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy, University of St. Andrews , North Haugh, St Andrews, Fife KY16 9SS , UK

5. Faculty of Aerospace Engineering, Delft University of Technology , Kluyverweg 1, NL-2629 HS Delft , The Netherlands

6. Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut , Mönchhofstr. 12-14, D-69120 Heidelberg , Germany

7. SUPA, Institute for Astronomy, University of Edinburgh , Royal Observatory, Blackford Hill, Edinburgh EH9 2HJ , UK

8. Centre for Exoplanet Science, University of Edinburgh , Edinburgh, EH9 3FD , UK

9. School of Physics and Astronomy, University of Leeds , Leeds, LS2 9JT , UK

Abstract

ABSTRACT We carry out three-dimensional smoothed particle hydrodynamics simulations to study the role of gravitational and drag forces on the concentration of large dust grains (St > 1) in the spiral arms of gravitationally unstable protoplanetary discs, and the resulting implications for planet formation. We find that both drag and gravity play an important role in the evolution of large dust grains. If we include both, grains that would otherwise be partially decoupled will become well coupled and trace the spirals. For the dust grains most influenced by drag (with Stokes numbers near unity), the dust disc quickly becomes gravitationally unstable and rapidly forms clumps with masses between 0.15–6M⊕. A large fraction of clumps are below the threshold where runaway gas accretion can occur. However, if dust self-gravity is neglected, the dust is unable to form clumps, despite still becoming trapped in the gas spirals. When large dust grains are unable to feel either gas gravity or drag, the dust is unable to trace the gas spirals. Hence, full physics is needed to properly simulate dust in gravitationally unstable discs. Dust trapping of large grains in spiral arms of discs stable to gas fragmentation could explain planet formation in very young discs by a population of planetesimals formed due to the combined roles of drag and gravity in the earliest stages of a disc’s evolution. Furthermore, it highlights that gravitationally unstable discs are not just important for forming gas giants quickly, it can also rapidly form Earth mass bodies.

Funder

STFC

Royal Society

European Research Council

Horizon 2020

Publisher

Oxford University Press (OUP)

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