dc.contributor.author | Ali, A | |
dc.contributor.author | Harries, TJ | |
dc.contributor.author | Douglas, TA | |
dc.date.accessioned | 2018-07-23T10:28:53Z | |
dc.date.issued | 2018-04-21 | |
dc.description.abstract | We simulate a self-gravitating, turbulent cloud of 1000 M⊙ with photoionization and radiation pressure feedback from a 34 M⊙ star. We use a detailed Monte Carlo radiative transfer scheme alongside the hydrodynamics to compute photoionization and thermal equilibrium with dust grains and multiple atomic species. Using these gas temperatures, dust temperatures, and ionization fractions, we produce self-consistent synthetic observations of line and continuum emission. We find that all material is dispersed from the (15.5 pc)3 grid within 1.6 Myr or 0.74 free-fall times. Mass exits with a peak flux of 2 × 10−3 M⊙ yr−1, showing efficient gas dispersal. The model without radiation pressure has a slight delay in the breakthrough of ionization, but overall its effects are negligible. 85 per cent of the volume, and 40 per cent of the mass, become ionized – dense filaments resist ionization and are swept up into spherical cores with pillars that point radially away from the ionizing star. We use free–free emission at 20 cm to estimate the production rate of ionizing photons. This is almost always underestimated: by a factor of a few at early stages, then by orders of magnitude as mass leaves the volume. We also test the ratio of dust continuum surface brightnesses at 450 and 850 µm to probe dust temperatures. This underestimates the actual temperature by more than a factor of 2 in areas of low column density or high line-of-sight temperature dispersion; the
HII
region cavity is particularly prone to this discrepancy. However, the probe is accurate in dense locations such as filaments. | en_GB |
dc.description.sponsorship | We thank the referee, Alejandro Raga, for helpful comments. We also thank Thomas Haworth and David Acreman for useful discussions. AA is funded by an STFC studentship. TJH and TAD are funded by STFC Consolidated Grant ST/M00127X/1. The calculations for this paper were performed on the DiRAC Complexity system at the University of Leicester and the DiRAC Data Centric system at Durham University. These form part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). Complexity is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grants ST/K0003259/1 and ST/M006948/1. Data Centric is funded by a BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grants ST/K00087X/1 and ST/P002307/1, DiRAC Operations grant ST/K003267/1, and Durham University. We also used the University of Exeter Supercomputer, Zen, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital fund of BIS, and the University of Exeter. | en_GB |
dc.identifier.citation | Vol. 477 (4), pp. 5422 - 5436 | en_GB |
dc.identifier.doi | 10.1093/mnras/sty1001 | |
dc.identifier.uri | http://hdl.handle.net/10871/33524 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press | en_GB |
dc.relation.url | https://doi.org/10.24378/exe.1163 | en_GB |
dc.rights | © 2018 The Author(s) | en_GB |
dc.subject | hydrodynamics | en_GB |
dc.subject | radiative transfer | en_GB |
dc.subject | stars: massive | en_GB |
dc.subject | ISM: clouds | en_GB |
dc.subject | H II regions | en_GB |
dc.title | Modelling massive star feedback with Monte Carlo radiation hydrodynamics: photoionization and radiation pressure in a turbulent cloud (article) | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2018-07-23T10:28:53Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the final version of the article. Available from Oxford University Press via the DOI in this record. | en_GB |
dc.description | The dataset associated with this article is located in ORE at: https://doi.org/10.24378/exe.1163 | en_GB |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |