St Andrews Research Repository

St Andrews University Home
View Item 
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  •   St Andrews Research Repository
  • University of St Andrews Research
  • University of St Andrews Research
  • University of St Andrews Research
  • View Item
  • Login
JavaScript is disabled for your browser. Some features of this site may not work without it.

Diversity in the outcome of dust radial drift in protoplanetary discs

Thumbnail
View/Open
Laibe_2014_A_A_Diversity.pdf (306.1Kb)
Date
01/05/2014
Author
Pinte, C.
Laibe, G.
Funder
European Research Council
Grant ID
Keywords
Circumstellar matter
Protoplanetary disks
Stars: formation
Radiative transfer
Methods: analytical
Methods: numerical
QB Astronomy
Metadata
Show full item record
Altmetrics Handle Statistics
Altmetrics DOI Statistics
Abstract
The 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.
Citation
Pinte , C & Laibe , G 2014 , ' Diversity in the outcome of dust radial drift in protoplanetary discs ' , Astronomy & Astrophysics , vol. 565 , A129 . https://doi.org/10.1051/0004-6361/201220545
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201220545
ISSN
0004-6361
Type
Journal article
Rights
© ESO, 2014
Description
C. 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.
Collections
  • University of St Andrews Research
URL
http://www.scopus.com/inward/record.url?eid=2-s2.0-84901617680&partnerID=8YFLogxK
URI
http://hdl.handle.net/10023/5270

Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.

Advanced Search

Browse

All of RepositoryCommunities & CollectionsBy Issue DateNamesTitlesSubjectsClassificationTypeFunderThis CollectionBy Issue DateNamesTitlesSubjectsClassificationTypeFunder

My Account

Login

Open Access

To find out how you can benefit from open access to research, see our library web pages and Open Access blog. For open access help contact: openaccess@st-andrews.ac.uk.

Accessibility

Read our Accessibility statement.

How to submit research papers

The full text of research papers can be submitted to the repository via Pure, the University's research information system. For help see our guide: How to deposit in Pure.

Electronic thesis deposit

Help with deposit.

Repository help

For repository help contact: Digital-Repository@st-andrews.ac.uk.

Give Feedback

Cookie policy

This site may use cookies. Please see Terms and Conditions.

Usage statistics

COUNTER-compliant statistics on downloads from the repository are available from the IRUS-UK Service. Contact us for information.

© University of St Andrews Library

University of St Andrews is a charity registered in Scotland, No SC013532.

  • Facebook
  • Twitter