Show simple item record

Files in this item


Item metadata

dc.contributor.authorPinte, C.
dc.contributor.authorLaibe, G.
dc.identifier.citationPinte , C & Laibe , G 2014 , ' Diversity in the outcome of dust radial drift in protoplanetary discs ' , Astronomy & Astrophysics , vol. 565 , A129 .
dc.identifier.otherPURE: 143964808
dc.identifier.otherPURE UUID: edda98b2-afab-4953-8e0c-3233b0262132
dc.identifier.otherScopus: 84901617680
dc.identifier.otherWOS: 000336730900129
dc.descriptionC. Pinte acknowledges funding from the European Commission’s FP7 (contract PERG06-GA-2009-256513) and the Agence Nationale pour la Recherche of France (contract ANR-2010-JCJC-0504-01). G. Laibe is grateful to the Australian Research Council for funding (contract DP1094585) and acknowledges funding from the European Research Council for the FP7 ERC advanced grant project ECOGAL.en
dc.description.abstractThe growth of dust particles into planet embryos needs to circumvent the "radial-drift barrier", i.e. the accretion of dust particles onto the central star by radial migration. The outcome of the dust radial migration is governed by simple criteria between the dust-to-gas ratio and the exponents p and q of the surface density and temperature power laws. The transfer of radiation provides an additional constraint between these quantities because the disc thermal structure is fixed by the dust spatial distribution. To assess which discs are primarily affected by the radial-drift barrier, we used the radiative transfer code MCFOST to compute the temperature structure of a wide range of disc models, stressing the particular effects of grain size distributions and vertical settling. We find that the outcome of the dust migration process is very sensitive to the physical conditions within the disc. For high dust-to-gas ratios (≳ 0.01) and/or flattened disc structures (H/R ≲ 0.05), growing dust grains can efficiently decouple from the gas, leading to a high concentration of grains at a critical radius of a few AU. Decoupling of grains from gas can occur at a large fraction (>0.1) of the initial radius of the particle, for a dust-to-gas ratio greater than ≈0.05. Dust grains that experience migration without significant growth (millimetre and centimetre-sized) are efficiently accreted for discs with flat surface density profiles (p <0.7) while they always remain in the disc if the surface density is steep enough (p > 1.2). Between (0.7 <p <1.2), both behaviours may occur depending on the exact density and temperature structures of the disc. Both the presence of large grains and vertical settling tend to favour the accretion of non-growing dust grains onto the central object, but it slows down the migration of growing dust grains. If the disc has evolved into a self-shadowed structure, the required dust-to-gas ratio for dust grains to stop their migration at large radius become much smaller, of the order of 0.01. All the disc configurations are found to have favourable temperature profiles over most of the disc to retain their planetesimals.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2014en
dc.subjectCircumstellar matteren
dc.subjectProtoplanetary disksen
dc.subjectStars: formationen
dc.subjectRadiative transferen
dc.subjectMethods: analyticalen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.titleDiversity in the outcome of dust radial drift in protoplanetary discsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

This item appears in the following Collection(s)

Show simple item record