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dc.contributor.authorSchartmann, M.
dc.contributor.authorKrause, Martin
dc.contributor.authorBurkert, A.
dc.date.accessioned2017-04-20T16:00:56Z
dc.date.available2017-04-20T16:00:56Z
dc.date.issued2011-07-21
dc.identifier.citationSchartmann , M , Krause , M & Burkert , A 2011 , ' Radiation feedback on dusty clouds during Seyfert activity ' , Monthly Notices of the Royal Astronomical Society , vol. 415 , no. 1 , pp. 741-752 . https://doi.org/10.1111/j.1365-2966.2011.18751.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11087953
dc.identifier.otherPURE UUID: fe7dd083-0c66-4fc6-9285-e898a47bc25f
dc.identifier.otherBibtex: urn:51da05c2186dab3ce061b8e01b0a138c
dc.identifier.otherScopus: 79960140191
dc.identifier.otherORCID: /0000-0002-9610-5629/work/63687353
dc.identifier.urihttp://hdl.handle.net/2299/18000
dc.descriptionM. Schartmann, M. Krause, and A. Burkert, 'Radiation feedback on dusty clouds during Seyfert activity', Monthly Notices of the Royal Astronomical Society, Vol. 415 (1): 741-752, first published online 8 July 2011. The version of record is available online at doi: :10.1111/j.1365-2966.2011.18751.x. Published by Oxford University Press on behalf of the Royal Astronomical Society. © 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS.
dc.description.abstractWe investigate the evolution of dusty gas clouds falling into the centre of an active Seyfert nucleus. 2D high-resolution radiation hydrodynamics simulations are performed to study the fate of single clouds and the interaction between two clouds approaching the active galactic nucleus. We find three distinct phases of the evolution of the cloud: (i) formation of a lenticular shape with dense inner rim caused by the interaction of gravity and radiation pressure (the lense phase); (ii) formation of a clumpy sickle-shaped structure as the result of a converging flow (the clumpy sickle phase) and (iii) a filamentary phase caused by a rapidly varying optical depth along the sickle. Depending on the column density of the cloud, it will either be pushed outwards or its central (highest column density) parts move inwards, while there is always some material pushed outwards by radiation pressure effects. The general dynamical evolution of the cloud can approximately be described by a simple analytical model.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjecthydrodynamics, radiative transfer, ISM: clouds, dust, extinction, ISM: structure, galaxies: Seyfert
dc.titleRadiation feedback on dusty clouds during Seyfert activityen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.18751.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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