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dc.contributor.authorSmilgys, Romas
dc.contributor.authorBonnell, Ian A.
dc.date.accessioned2016-06-06T14:30:12Z
dc.date.available2016-06-06T14:30:12Z
dc.date.issued2016-06-21
dc.identifier.citationSmilgys , R & Bonnell , I A 2016 , ' Star formation in Galactic flows ' Monthly Notices of the Royal Astronomical Society , vol. 459 , no. 2 , pp. 1985-1992 . https://doi.org/10.1093/mnras/stw791en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 243134005
dc.identifier.otherPURE UUID: cdbc8082-e312-4e39-b859-e1a2bc5464c0
dc.identifier.otherRIS: urn:2CB31368E476D84743CEE12B612AC5AD
dc.identifier.otherScopus: 84974625384
dc.identifier.urihttp://hdl.handle.net/10023/8938
dc.descriptionRS and IAB acknowledges funding from the European Research Council for the FP7 ERC advanced grant project ECOGAL. This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure.en
dc.description.abstractWe investigate the triggering of star formation in clouds that form in Galactic scale flows as the interstellar medium passes through spiral shocks. We use the Lagrangian nature of smoothed particle hydrodynamics simulations to trace how the star-forming gas is gathered into self-gravitating cores that collapse to form stars. Large-scale flows that arise due to Galactic dynamics create shocks of the order of 30 km s−1 that compress the gas and form dense clouds (n > several × 102 cm−3) in which self-gravity becomes relevant. These large-scale flows are necessary for creating the dense physical conditions for gravitational collapse and star formation. Local gravitational collapse requires densities in excess of n > 103 cm−3 which occur on size scales of ≈1 pc for low-mass star-forming regions (M < 100 M⊙), and up to sizes approaching 10 pc for higher mass regions (M > 103 M⊙). Star formation in the 250 pc region lasts throughout the 5 Myr time-scale of the simulation with a star formation rate of ≈10−1 M⊙ yr−1 kpc−2. In the absence of feedback, the efficiency of the star formation per free-fall time varies from our assumed 100 per cent at our sink accretion radius to values of <10−3 at low densities.en
dc.format.extent8en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stw791en
dc.subjectStars: formationen
dc.subjectStars: luminosity function, mass functionen
dc.subjectGalaxies: star formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleStar formation in Galactic flowsen
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/stw791
dc.description.statusPeer revieweden


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