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dc.contributor.authorRosotti, G.~P.
dc.contributor.authorde Juan Ovelar, M.
dc.contributor.authorHubber, D.~A.
dc.contributor.authorKruijssen, J.~M.~D.
dc.contributor.authorErcolano, B.
dc.contributor.authorWalch, S.
dc.contributor.authorDale, James
dc.date.accessioned2017-07-21T14:56:56Z
dc.date.available2017-07-21T14:56:56Z
dc.date.issued2014-07-01
dc.identifier.citationRosotti , G P , de Juan Ovelar , M , Hubber , D A , Kruijssen , J M D , Ercolano , B , Walch , S & Dale , J 2014 , ' Protoplanetary disc evolution affected by star-disc interactions in young stellar clusters ' , Monthly Notices of the Royal Astronomical Society , vol. 441 , no. 3 , pp. 2094-2110 . https://doi.org/10.1093/mnras/stu679
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11151086
dc.identifier.otherPURE UUID: dd13411e-c47f-452a-9a82-232437b9ae3b
dc.identifier.otherBibtex: urn:a54c1279ea07028ada85854f9fd82d96
dc.identifier.otherScopus: 84903194151
dc.identifier.otherORCID: /0000-0001-5252-5771/work/62751048
dc.identifier.urihttp://hdl.handle.net/2299/19042
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractMost stars form in a clustered environment. Therefore, it is important to assess how this environment influences the evolution of protoplanetary discs around young stars. In turn, this affects their ability to produce planets and ultimately life. We present here for the first time 3D smoothed particle hydrodynamics/N-body simulations that include both the hydrodynamical evolution of the discs around their natal stars, as well as the dynamics of the stars themselves. The discs are viscously evolving, accreting mass on to the central star and spreading. We find penetrating encounters to be very destructive for the discs as in previous studies, although the frequency of such encounters is low. We also find, however, that encounter influence the disc radii more strongly than other disc properties such as the disc mass. The disc sizes are set by the competition between viscous spreading and the disruptive effect of encounters. As discs spread, encounters become more and more important. In the regime of rapid spreading, encounters simply truncate the discs, stripping the outer portions. In the opposite regime, we find that the effect of many distant encounters is able to limit the disc size. Finally, we predict from our simulations that disc sizes are limited by encounters at stellar densities exceeding ∼2–3 × 103 pc−2.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectaccretion, accretion discs, hydrodynamics, protoplanetary discs
dc.titleProtoplanetary disc evolution affected by star-disc interactions in young stellar clustersen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stu679
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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