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Non-thermal broadening of coronal lines in a 3D MHD loop model
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dc.contributor.author | Breu, Cosima Alexandra | |
dc.contributor.author | Peter, Hardi | |
dc.contributor.author | Solanki, Sami Khan | |
dc.contributor.author | Cameron, Robert | |
dc.contributor.author | De Moortel, Ineke | |
dc.date.accessioned | 2024-05-24T16:30:07Z | |
dc.date.available | 2024-05-24T16:30:07Z | |
dc.date.issued | 2024-05 | |
dc.identifier | 300388568 | |
dc.identifier | ba1d0572-b969-4780-ac3f-7f75398d1cd0 | |
dc.identifier | 85191899572 | |
dc.identifier.citation | Breu , C A , Peter , H , Solanki , S K , Cameron , R & De Moortel , I 2024 , ' Non-thermal broadening of coronal lines in a 3D MHD loop model ' , Monthly Notices of the Royal Astronomical Society , vol. 530 , no. 2 , pp. 2361–2377 . https://doi.org/10.1093/mnras/stae899 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | ORCID: /0000-0002-1452-9330/work/160317084 | |
dc.identifier.uri | https://hdl.handle.net/10023/29927 | |
dc.description | Funding: This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 695075). The research leading to these results has received funding from the UK Science and Technology Facilities Council (consolidated grant ST/W001195/1). Ineke De Moortel received funding from the Research Council of Norway through its Centres of Excellence scheme, project number 262622. | en |
dc.description.abstract | Observed spectral profiles of emission lines from the corona are found to have widths exceeding the thermal line width. To investigate the physical mechanism, we run a 3D MHD model of a single, straightened loop in which we partially resolve turbulent motions that form in response to the driving by self-consistently evolving magneto-convection in the photosphere. The convective motions shear and twist the magnetic field lines, leading to heating. From the model we synthesize spectral profiles of emission lines forming at temperatures around and above 1 MK. The coronal heating process generates a range of velocity amplitudes and directions structured on a scale much smaller than the resolving power of current instruments, leading to a broadening of the spectral lines. Our model includes the mass exchange between corona and chromosphere, thus we also capture flows parallel to the loop axis. We find that the spectral lines show a non-thermal line broadening roughly consistent with observations for a viewing angle perpendicular to the axis. The broadening through field-parallel flows is comparable, although slightly smaller. The line broadening is independent of the instrument resolution for a perpendicular line-of-sight. We can connect the non-thermal line broadening to heating events and flows. While small-scale velocities along the line-of-sight are mainly responsible for the broadening observed perpendicular to the loop, chromospheric evaporation is important for the line broadening observed along the loop. The model reproduces observed values for non-thermal line widths. In the model these result from continuous driving by magnetoconvection, without imposing driving motions or starting from an already braided field. | |
dc.format.extent | 4441615 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Sun: corona | en |
dc.subject | Sun: magnetic field | en |
dc.subject | Magnetohydrodyanmics (MHD) | en |
dc.subject | QB Astronomy | en |
dc.subject | Physics and Astronomy(all) | en |
dc.subject | RR-NDAS | en |
dc.subject.lcc | QB | en |
dc.title | Non-thermal broadening of coronal lines in a 3D MHD loop model | 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 | 10.1093/mnras/stae899 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/W001195/1 | en |
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