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dc.contributor.authorKlaassen, P.~D.
dc.contributor.authorMottram, J.~C.
dc.contributor.authorJuhasz, A.
dc.contributor.authorDale, James
dc.date.accessioned2017-07-21T14:57:00Z
dc.date.available2017-07-21T14:57:00Z
dc.date.issued2014-06-11
dc.identifier.citationKlaassen , P D , Mottram , J C , Juhasz , A & Dale , J 2014 , ' Cloud disruption via ionized feedback: tracing pillar dynamics in Vulpecula ' , Monthly Notices of the Royal Astronomical Society , vol. 441 , no. 1 , pp. 656-663 . https://doi.org/10.1093/mnras/stu587
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11151110
dc.identifier.otherPURE UUID: c9b6b8ad-9ce7-4505-ac62-f8ebc8b3e172
dc.identifier.otherBibtex: urn:951ad5cebd262b26eceae17144ce6a6f
dc.identifier.otherScopus: 84899999660
dc.identifier.otherORCID: /0000-0001-5252-5771/work/62751046
dc.identifier.urihttp://hdl.handle.net/2299/19043
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.abstractThe major physical processes responsible for shaping and sculpting pillars in the clouds surrounding massive stars (i.e. the ‘Pillars of Creation’) are now being robustly incorporated into models quantifying the ionizing radiation from massive stars. The detailed gas dynamics within these pillars can now be compared with observations. Our goal is to quantify the gas dynamics in a pillar being sculpted by a nearby massive star. To do this, we use the CO, 13CO and C18O J = 1–0 emission towards a pillar in the Vulpecula Rift. These data are a combination of Combined Array for Research in Millimeter-Wave Astronomy and Five College Radio Astronomy Observatory observations providing high-resolution (∼5) imaging of large-scale pillar structures (>100 arcsec). We find that this cold (∼18 K), low-density (8 × 103 cm−3) material is fragmenting on Jeans scales, has very low velocity dispersions (∼0.5 km s−1), and appears to be moving away from the ionizing source. We are able to draw direct comparisons with three models from the literature, and find that those with lower velocity dispersions best fit our data, although the dynamics of any one model do not completely agree with our observations. We do, however, find that our observed pillar exhibits many of the characteristics expected from simulations.en
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectISM: clouds, ISM: kinematics and dynamics, ISM: structure, submillimetre: ISM
dc.titleCloud disruption via ionized feedback: tracing pillar dynamics in Vulpeculaen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2014-06-11
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stu587
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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