Files in this item
An optimization principle for computing stationary MHD equilibria with solar wind flow
Item metadata
dc.contributor.author | Wiegelmann, Thomas | |
dc.contributor.author | Neukirch, Thomas | |
dc.contributor.author | Nickeler, Dieter | |
dc.contributor.author | Chifu, Iulia | |
dc.date.accessioned | 2020-11-10T17:30:10Z | |
dc.date.available | 2020-11-10T17:30:10Z | |
dc.date.issued | 2020-10 | |
dc.identifier | 270518517 | |
dc.identifier | 9a53bddf-2f4a-4466-b86f-faec1751e3fe | |
dc.identifier | 85094652525 | |
dc.identifier | 000589557800001 | |
dc.identifier.citation | Wiegelmann , T , Neukirch , T , Nickeler , D & Chifu , I 2020 , ' An optimization principle for computing stationary MHD equilibria with solar wind flow ' , Solar Physics , vol. 295 , no. 10 , 145 . https://doi.org/10.1007/s11207-020-01719-8 | en |
dc.identifier.issn | 0038-0938 | |
dc.identifier.other | ORCID: /0000-0002-7597-4980/work/83481718 | |
dc.identifier.uri | https://hdl.handle.net/10023/20942 | |
dc.description | TW acknowledges financial support by DLR-grant 50 OC 1701 and DFG-grant WI 3211/5-1. TN acknowledges financial support by the UK’s Science and Technology Facilities Council (STFC) via Consolidated Grant ST/S000402/1. The Astronomical Institute of the Czech Academy of Sciences is supported by the project RVO:67985815. IC acknowledges funding by DFG-grant WI 3211/5-1. | en |
dc.description.abstract | In this work we describe a numerical optimization method for computing stationary MHD-equilibria. The newly developed code is based on a nonlinearforce-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasma β and Alfvén Mach number MA are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where β and MA are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magneto-static models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe. | |
dc.format.extent | 14 | |
dc.format.extent | 2272049 | |
dc.language.iso | eng | |
dc.relation.ispartof | Solar Physics | en |
dc.subject | Magnetic fields, corona | en |
dc.subject | Magnetic fields, models | en |
dc.subject | Magnetohydrodynamics | en |
dc.subject | Velocity fields, solar wind | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | Astronomy and Astrophysics | en |
dc.subject | T-NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | An optimization principle for computing stationary MHD equilibria with solar wind flow | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. Applied Mathematics | en |
dc.identifier.doi | https://doi.org/10.1007/s11207-020-01719-8 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/2010.02945 | en |
dc.identifier.grantnumber | ST/S000402/1 | en |
This item appears in the following Collection(s)
Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.