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dc.contributor.authorSnow, B
dc.contributor.authorDruett, MK
dc.contributor.authorHillier, A
dc.date.accessioned2023-09-11T09:59:40Z
dc.date.issued2023-08-25
dc.date.updated2023-09-11T08:06:39Z
dc.description.abstractExplosive phenomena are known to trigger a wealth of shocks in warm plasma environments, including the solar chromosphere and molecular clouds where the medium consists of both ionised and neutral species. Partial ionisation is critical in determining the behaviour of shocks, since the ions and neutrals locally decouple, allowing for substructure to exist within the shock. Accurately modelling partially ionised shocks requires careful treatment of the ionised and neutral species, and their interactions. Here we study a partially-ionised switch-off slow-mode shock using a multi-level hydrogen model with both collisional and radiative ionisation and recombination rates that are implemented into the two-fluid (PIP) code, and study physical parameters that are typical of the solar chromosphere. The multi-level hydrogen model differs significantly from MHD solutions due to the macroscopic thermal energy loss during collisional ionisation. In particular, the plasma temperature both post-shock and within the finite-width is significantly cooler that the post-shock MHD temperature. Furthermore, in the mid to lower chromosphere, shocks feature far greater compression then their single-fluid MHD analogues. The decreased temperature and increased compression reveal the importance of non-equilibrium ionised in the thermal evolution of shocks in partially ionised media. Since partially ionised shocks are not accurately described by the Rankine-Hugoniot shock jump conditions, it may be incorrect to use these to infer properties of lower atmospheric shocks.en_GB
dc.description.sponsorshipScience and Technology Facilities Council (STFC)en_GB
dc.description.sponsorshipFWOen_GB
dc.identifier.citationPublished online 25 August 2023en_GB
dc.identifier.doihttps://doi.org/10.1093/mnras/stad2585
dc.identifier.grantnumberST/R000891/1en_GB
dc.identifier.grantnumberST/V000659/1en_GB
dc.identifier.grantnumberG0B4521Nen_GB
dc.identifier.urihttp://hdl.handle.net/10871/133963
dc.identifierORCID: 0000-0002-4500-9805 (Snow, B)
dc.identifierORCID: 0000-0002-0851-5362 (Hillier, A)
dc.language.isoenen_GB
dc.publisherOxford University Press (OUP) / Royal Astronomical Societyen_GB
dc.relation.urlhttps://github.com/AstroSnow/PIPen_GB
dc.rights© The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.en_GB
dc.subjectShock wavesen_GB
dc.subjectPlasmasen_GB
dc.subject(magnetohydrodynamics) MHDen_GB
dc.subjectSun: chromosphereen_GB
dc.titlePartially-ionised two-fluid shocks with collisional and radiative ionisation and recombination - multi-level hydrogen modelen_GB
dc.typeArticleen_GB
dc.date.available2023-09-11T09:59:40Z
dc.identifier.issn0035-8711
dc.descriptionThis is the author accepted manuscript. The final version is available on open access from Oxford University Press via the DOI in this recorden_GB
dc.descriptionData availability: The simulation data from this study are available from BS upon reasonable request. The (PIP) code is available at https://github.com/AstroSnow/PIPen_GB
dc.identifier.eissn1365-2966
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen_GB
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_GB
rioxxterms.versionAMen_GB
rioxxterms.licenseref.startdate2023-08-25
rioxxterms.typeJournal Article/Reviewen_GB
refterms.dateFCD2023-09-11T09:56:19Z
refterms.versionFCDAM
refterms.dateFOA2023-09-11T09:59:43Z
refterms.panelBen_GB
refterms.dateFirstOnline2023-08-25


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© The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
Except where otherwise noted, this item's licence is described as © The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.