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dc.contributor.authorPriestley, Felix D.
dc.contributor.authorWurster, James
dc.contributor.authorViti, Serena
dc.date.accessioned2019-10-25T11:30:07Z
dc.date.available2019-10-25T11:30:07Z
dc.date.issued2019-09
dc.identifier.citationPriestley , F D , Wurster , J & Viti , S 2019 , ' Ambipolar diffusion and the molecular abundances in pre-stellar cores ' , Monthly Notices of the Royal Astronomical Society , vol. 488 , no. 2 , pp. 2357-2364 . https://doi.org/10.1093/mnras/stz1869en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 262149971
dc.identifier.otherPURE UUID: c58d89f9-a719-493d-8f5f-d02d8274b79e
dc.identifier.otherBibtex: PriestleyWursterViti2019
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716930
dc.identifier.otherScopus: 85074475939
dc.identifier.urihttp://hdl.handle.net/10023/18771
dc.description.abstractWe investigate differences in the molecular abundances between magnetically super- and subcritical pre-stellar cores, performing three-dimensional non-ideal magnetohydrodynamical (MHD) simulations with varying densities and magnetic field strengths, and post-processing the results with a time-dependent gas–grain chemical code. Most molecular species show significantly more central depletion in subcritical models, due to the longer duration of collapse. However, the directly observable quantities – the molecule to hydrogen column density ratios – are generally too similar for observational data to discriminate between models. The profiles of N2H+ and HCO+ show qualitative differences between supercritical and subcritical models on scales of 0.01pc ⁠, which may allow the two cases to be distinguished. However, this requires knowledge of the hydrogen column density, which is not directly measureable, and predicted line intensity profiles from radiative transfer modelling are similar for these molecules. Other commonly observed species, such as HCN and CH3OH, have line intensity profiles that differ more strongly between models, and so are more promising as tracers of the mechanism of cloud collapse.
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz1869en
dc.subjectAstrochemistryen
dc.subjectMHDen
dc.subjectStars: formationen
dc.subjectISM: moleculesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleAmbipolar diffusion and the molecular abundances in pre-stellar coresen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz1869
dc.description.statusPeer revieweden
dc.identifier.urlhttp://orca.cf.ac.uk/id/eprint/124711en


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