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dc.contributor.authorMaxted, N.
dc.contributor.authorRowell, G.
dc.contributor.authorDawson, B.
dc.contributor.authorBurton, M.
dc.contributor.authorNicholas, B.
dc.contributor.authorFukui, Y.
dc.contributor.authorWalsh, Andrew
dc.contributor.authorKawamura, A.
dc.contributor.authorHorachi, H.
dc.contributor.authorSano, H.
dc.date.accessioned2017-01-30T12:05:57Z
dc.date.available2017-01-30T12:05:57Z
dc.date.created2014-06-08T20:00:20Z
dc.date.issued2012
dc.identifier.citationMaxted, N. and Rowell, G. and Dawson, B. and Burton, M. and Nicholas, B. and Fukui, Y. and Walsh, A. et al. 2012. 3 to 12 millimetre studies of dense gas towards the western rim of supernova remnant RX J1713.7-3946. Monthly Notices of the Royal Astronomical Society. 422 (3): pp. 2230-2245.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/18107
dc.identifier.doi10.1111/j.1365-2966.2012.20766.x
dc.description.abstract

The young X-ray and gamma-ray-bright supernova remnant RX J1713.7−3946 (SNR G347.3−0.5) is believed to be associated with molecular cores that lie within regions of the most intense TeV emission. Using the Mopra telescope, four of the densest cores were observed using high critical density tracers such as CS(J= 1–0, J= 2–1) and its isotopologue counterparts, NH3(1,1) and (2,2) inversion transitions and N2H+(J= 1–0) emission, confirming the presence of dense gas ≥104 cm−3 in the region. The mass estimates for Core C range from 40 (from CS) to 80 M (from NH3 and N2H+), an order of magnitude smaller than published mass estimates from CO(J= 1–0) observations. We also modelled the energy-dependent diffusion of cosmic-ray protons accelerated by RX J1713.7-3946 into Core C, approximating the core with average density and magnetic field values. We find that for considerably suppressed diffusion coefficients (factors \chi=10^{-3} down to 10^ {-5} the galactic average), low energy cosmic-rays can be prevented from entering the inner core region. Such an effect could lead to characteristic spectral behaviour in the GeV to TeV gamma-ray and multi-keV X-ray fluxes across the core. These features may be measurable with future gamma-ray and multi-keV telescopes offering arcminute or better angular resolution, and can be a novel way to understand the level of cosmic-ray acceleration in RX J1713.7-3946 and the transport properties of cosmic-rays in the dense molecular cores.

dc.publisherOxford University Press
dc.subjectdiffusion
dc.subjectgamma-rays: ISM
dc.subjectISM: clouds
dc.subjectsupernovae: individual: RX J1713.7-3946
dc.subjectcosmic rays
dc.subjectmolecular data
dc.title3 to 12 millimetre studies of dense gas towards the western rim of supernova remnant RX J1713.7-3946
dc.typeJournal Article
dcterms.source.volume422
dcterms.source.startPage2230
dcterms.source.endPage2245
dcterms.source.issn0035-8711
dcterms.source.titleMonthly Notices of the Royal Astronomical Society
curtin.note

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. ©: 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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curtin.accessStatusOpen access


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