On the dynamics and survival of fractal clouds in galactic winds

dc.contributor.authorBanda-Barragan, W. E.
dc.contributor.authorZertuche, F. J.
dc.contributor.authorFederrath, Christoph
dc.contributor.authorGarcia Del Valle, J.
dc.contributor.authorBruggen, M.
dc.contributor.authorWagner, A. Y.
dc.date.accessioned2020-07-27T00:08:20Z
dc.date.available2020-07-27T00:08:20Z
dc.date.issued2019-04-13
dc.date.updated2020-04-19T08:26:52Z
dc.description.abstractRecent observations suggest that dense gas clouds can survive even in hot galactic winds. Here we show that the inclusion of turbulent densities with different statistical properties has significant effects on the evolution of wind-swept clouds. We investigate how the initial standard deviation of the lognormal density field influences the dynamics of quasi-isothermal clouds embedded in supersonic winds. We compare uniform, fractal solenoidal, and fractal compressive cloud models in both 3D and 2D hydrodynamical simulations. We find that the processes of cloud disruption and dense gas entrainment are functions of the initial density distribution in the cloud. Fractal clouds accelerate, mix, and are disrupted earlier than uniform clouds. Within the fractal cloud sample, compressive clouds retain high-density nuclei, so they are more confined, less accelerated, and have lower velocity dispersions than their solenoidal counterparts. Compressive clouds are also less prone to Kelvin–Helmholtz and Rayleigh–Taylor instabilities, so they survive longer than solenoidal clouds. By comparing the cloud properties at the destruction time, we find that dense gas entrainment is more effective in uniform clouds than in either of the fractal clouds, and it is more effective in solenoidal than in compressive models. In contrast, mass loading into the wind is more efficient in compressive cloud models than in uniform or solenoidal models. Overall, wide density distributions lead to inefficient entrainment, but they facilitate mass loading and favour the survival of very dense gas in hot galactic winds.en_AU
dc.description.sponsorshipThis numerical work was supported by the Deutsche Forschungsgemeinschaft (DFG) via grant BR2026125 and by the Australian National Computational Infrastructure and the Pawsey Supercomputing Centre via grant ek9, with funding from the Australian Government and the Government of Western Australia, in the framework of the National Computational Merit Allocation Scheme and the ANU Allocation Scheme. CF acknowledges funding provided by the Australian Research Council (Discovery Projects DP170100603 and Future Fellowship FT180100495), the Australia–Germany Joint Research Cooperation Scheme (UA-DAAD), theLeibniz Rechenzentrum, and the Gauss Centre for Supercomputing (grants pr32lo, pr48pi, and GCS Large-scale project 10391), and the Partnership for Advanced Computing in Europe (PRACE grant pr89mu).en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0035-8711en_AU
dc.identifier.urihttp://hdl.handle.net/1885/206602
dc.language.isoen_AUen_AU
dc.provenancehttp://v2.sherpa.ac.uk/id/publication/24618..."Publisher's version can be made open access on institutional repository" from SHERPA/RoMEO site (as at 27/7/20).en_AU
dc.publisherBlackwell Publishing Ltden_AU
dc.relationhttp://purl.org/au-research/grants/arc/DP170100603en_AU
dc.relationhttp://purl.org/au-research/grants/arc/FT180100495en_AU
dc.rights© 2019 The Author(s)en_AU
dc.sourceMonthly Notices of the Royal Astronomical Societyen_AU
dc.subjecthydrodynamicsen_AU
dc.subjectturbulenceen_AU
dc.subjectmethods: numericalen_AU
dc.subjectISM: cloudsen_AU
dc.subjectgalaxies: ISMen_AU
dc.subjectgalaxies: starbursten_AU
dc.titleOn the dynamics and survival of fractal clouds in galactic windsen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Accessen_AU
dcterms.dateAccepted2019-04-09
local.bibliographicCitation.issue4en_AU
local.bibliographicCitation.lastpage4544en_AU
local.bibliographicCitation.startpage4526en_AU
local.contributor.affiliationBanda-Barragan, W. E., Universitat Hamburgen_AU
local.contributor.affiliationZertuche, F. J., Universidad Tecnologica Equinoccialen_AU
local.contributor.affiliationFederrath, Christoph, College of Science, ANUen_AU
local.contributor.affiliationGarcia Del Valle, J., Universidad Tecnica de Ambatoen_AU
local.contributor.affiliationBruggen, M., University of Hamburgen_AU
local.contributor.affiliationWagner, A. Y., University of Tsukubaen_AU
local.contributor.authoremailu5575624@anu.edu.auen_AU
local.contributor.authoruidFederrath, Christoph, u5575624en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020104 - Galactic Astronomyen_AU
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciencesen_AU
local.identifier.ariespublicationu3102795xPUB3556en_AU
local.identifier.citationvolume486en_AU
local.identifier.doi10.1093/mnras/stz1040en_AU
local.identifier.scopusID2-s2.0-85068007260
local.identifier.uidSubmittedByu3102795en_AU
local.publisher.urlhttps://academic.oup.com/en_AU
local.type.statusPublished Versionen_AU

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