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Filament formation in wind-cloud interactions - I. Spherical clouds in uniform magnetic fields

Banda-Barrigan, Wladimir; Parkin, Elliott; Federrath, Christoph; Crocker, Roland; Bicknell, Geoffrey

Description

Filamentary structures are ubiquitous in the interstellar medium, yet their formation, internal structure, and longevity have not been studied in detail. We report the results from a comprehensive numerical study that investigates the characteristics, formation, and evolution of filaments arising from magnetohydrodynamic interactions between supersonic winds and dense clouds. Here, we improve on previous simulations by utilizing sharper density contrasts and higher numerical resolutions....[Show more]

dc.contributor.authorBanda-Barrigan, Wladimir
dc.contributor.authorParkin, Elliott
dc.contributor.authorFederrath, Christoph
dc.contributor.authorCrocker, Roland
dc.contributor.authorBicknell, Geoffrey
dc.date.accessioned2018-11-29T22:53:52Z
dc.date.available2018-11-29T22:53:52Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/152597
dc.description.abstractFilamentary structures are ubiquitous in the interstellar medium, yet their formation, internal structure, and longevity have not been studied in detail. We report the results from a comprehensive numerical study that investigates the characteristics, formation, and evolution of filaments arising from magnetohydrodynamic interactions between supersonic winds and dense clouds. Here, we improve on previous simulations by utilizing sharper density contrasts and higher numerical resolutions. By following multiple density tracers, we find that material in the envelopes of the clouds is removed and deposited downstream to form filamentary tails, while the cores of the clouds serve as footpoints and late-stage outer layers of these tails. Aspect ratios 12, subsonic velocity dispersions ∼0.1–0.3 of the wind sound speed, and magnetic field amplifications ∼100 are found to be characteristic of these filaments. We also report the effects of different magnetic field strengths and orientations. The magnetic field strength regulates vorticity production: sinuous filamentary towers arise in non-magnetic environments, while strong magnetic fields inhibit small-scale perturbations at boundary layers making tails less turbulent. Magnetic field components aligned with the direction of the flow favour the formation of pressure-confined flux ropes inside the tails, whilst transverse components tend to form current sheets. Softening the equation of state to nearly isothermal leads to suppression of dynamical instabilities and further collimation of the tail. Towards the final stages of the evolution, we find that small cloudlets and distorted filaments survive the break-up of the clouds and become entrained in the winds, reaching velocities ∼0.1 of the wind speed. Key words: MHD – methods: numerical – stars: winds, outflows – ISM: clouds – ISM: mag
dc.format.mimetypeapplication/pdf
dc.publisherBlackwell Publishing Ltd
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.titleFilament formation in wind-cloud interactions - I. Spherical clouds in uniform magnetic fields
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume455
dc.date.issued2016
local.identifier.absfor020102 - Astronomical and Space Instrumentation
local.identifier.ariespublicationu5058514xPUB12
local.type.statusPublished Version
local.contributor.affiliationBanda-Barrigan, Wladimir, College of Science, ANU
local.contributor.affiliationParkin, Elliott, College of Science, ANU
local.contributor.affiliationFederrath, Christoph, College of Science, ANU
local.contributor.affiliationCrocker, Roland, College of Science, ANU
local.contributor.affiliationBicknell, Geoffrey, College of Science, ANU
local.bibliographicCitation.issue2
local.bibliographicCitation.startpage1309
local.bibliographicCitation.lastpage1333
local.identifier.doi10.1093/mnras/stv2405
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2018-11-29T07:55:47Z
local.identifier.scopusID2-s2.0-84961140756
local.identifier.thomsonID000368007100013
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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