dc.creator | Latter, Henrik Nils | |
dc.creator | Rosca, Roxana | |
dc.date.accessioned | 2016-09-26 | |
dc.date.accessioned | 2018-11-24T23:19:30Z | |
dc.date.available | 2016-12-21T11:37:17Z | |
dc.date.available | 2018-11-24T23:19:30Z | |
dc.date.issued | 2017-01-11 | |
dc.identifier | https://www.repository.cam.ac.uk/handle/1810/261682 | |
dc.identifier.uri | http://repository.aust.edu.ng/xmlui/handle/123456789/3463 | |
dc.description.abstract | In protoplanetary discs the aerodynamical friction between particles and gas induces a variety of instabilities that facilitate planet formation. Of these we examine the so-called ‘secular gravitational instability’ (SGI) in the two-fluid approximation, deriving analytical expressions for its stability criteria and growth rates. Concurrently, we present a physical explanation of the instability that shows how it manifests upon an intermediate range of lengthscales exhibiting geostrophic balance in the gas component. The two-fluid SGI is completely quenched within a critical disc radius, as large as 10 au and 30 au for centimetre- and millimetre-sized particles, respectively, although establishing robust estimates is hampered by uncertainties in the parameters (especially the strength of turbulence) and deficiencies in the razor-thin disc model we employ. It is unlikely, however, that the SGI is relevant for well-coupled dust. We conclude by applying these results to the question of planetesimal formation and the provenance of large-scale dust rings. | |
dc.language | en | |
dc.publisher | Oxford University Press | |
dc.publisher | Monthly Notices of the Royal Astronomical Society | |
dc.subject | instabilities | |
dc.subject | planets and satellites: formation | |
dc.subject | protoplanetary discs | |
dc.title | On dust–gas gravitational instabilities in protoplanetary discs | |
dc.type | Article | |