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dc.contributor.authorLaibe, G.
dc.contributor.authorGonzalez, J.-F.
dc.contributor.authorMaddison, S.T.
dc.identifier.citationLaibe , G , Gonzalez , J-F & Maddison , S T 2014 , ' Growing dust grains in protoplanetary discs - I. radial drift with toy growth models ' , Monthly Notices of the Royal Astronomical Society , vol. 437 , no. 4 , pp. 3025-3036 .
dc.identifier.otherPURE: 147009214
dc.identifier.otherPURE UUID: bb524d05-a7d2-4126-9027-522ace1c30ff
dc.identifier.otherScopus: 84891360020
dc.identifier.otherWOS: 000329177100001
dc.descriptionSTM acknowledges the support of a Swinburne Special Studies Program. GL is grateful to the Australian Research Council for funding via Discovery project grant DP1094585 and acknowledges funding from the European Research Council for the FP7 ERC advanced grant project ECOGAL. JFG's research was conducted within the Lyon Institute of Origins under grant ANR-10-LABX-66.en
dc.description.abstractIn a series of papers, we present a comprehensive analytic study of the global motion of growing dust grains in protoplanetary discs, addressing both the radial drift and the vertical settling of the particles. Here we study how the radial drift of dust particles is affected by grain growth. In a first step, toy models in which grain growth can either be constant, accelerate or decelerate are introduced. The equations of motion are analytically integrable and therefore the grains dynamics is easy to understand. The radial motion of growing grains is governed by the relative efficiency of the growth and migration processes which is expressed by the dimensionless parameter Λ, as well as the exponents for the gas surface density and temperature profiles, denoted by p and q, respectively. When Λ is of the order of unity, growth and migration are strongly coupled, providing the most efficient radial drift. For the toy models considered, grains pile up when -p + q + 1/2 > 0. Importantly, we show the existence of a second process which can help discs to retain their solid materials. For accelerating growth, grains end up their migration at a finite radius, thus avoiding being accreted on to the central star.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectMethods: analyticalen
dc.subjectPlanets and satellites: formationen
dc.subjectProtoplanetary discsen
dc.subjectDust, extinctionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleGrowing dust grains in protoplanetary discs - I. radial drift with toy growth modelsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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