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Effect of coronal loop structure on wave heating by phase mixing

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Pagano_2020_Effect_of_coronal_loop_A_A_AAM.pdf (1.039Mb)
Date
11/2020
Author
Pagano, Paolo
De Moortel, Ineke
Morton, Richard
Funder
European Research Council
Science & Technology Facilities Council
Grant ID
647214
ST/S000402/1
Keywords
QB Astronomy
QC Physics
T-NDAS
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Abstract
Context. The mechanism(s) behind coronal heating still elude(s) direct observation and modelling of viable theoretical processes and the subsequent effect on coronal structures is one of the key tools available to assess possible heating mechanisms. Wave-heating via phase-mixing of Magnetohydrodynamics (MHD) transverse waves has been proposed as a possible way to convert magnetic energy into thermal energy but increasingly, MHD models suggest this is not a sufficiently efficient mechanism. Aims. We model heating by phase-mixing of transverse MHD waves in various configurations, to investigate whether certain circumstances can enhance the heating sufficiently to sustain the million degree solar corona and to assess the impact of the propagation and phase-mixing of transverse MHD waves on the structure of the boundary shell of coronal loops. Methods. We use 3D MHD simulations of a pre-existing density enhancement in magnetised medium and a boundary driver to trigger the propagation of transverse waves with the same power spectrum as measured by the Coronal Multi-Channel Polarimeter (COmP). We consider different density structures, boundary conditions at the non-drive footpoint, characteristics of the driver, and different forms of magnetic resistivity. Results. We find that different initial density structures significantly affect the evolution of the boundary shell and that some driver configurations can enhance the heating generated from the dissipation ofthe MHD waves. In particular, drivers coherent on a larger spatial scale and higher dissipation coefficients can generate significant heating, although it is still insufficient to balance the radiative losses in this setup. Conclusions. We conclude that while phase-mixing of transverse MHD waves is unlikely to sustain the thermal structure of the corona, there are configurations that allow for an enhanced efficiency of this mechanism. We provide possible signatures to identify the presence of such configurations, such as the location of where the heating is deposited along the coronal loop.
Citation
Pagano , P , De Moortel , I & Morton , R 2020 , ' Effect of coronal loop structure on wave heating by phase mixing ' , Astronomy & Astrophysics , vol. 643 , A73 . https://doi.org/10.1051/0004-6361/202039209
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/202039209
ISSN
0004-6361
Type
Journal article
Rights
Copyright © 2020 ESO. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://doi.org/10.1051/0004-6361/202039209.
Description
Funding: UK Science and Technology Facilities Council (Consolidated Grant ST/K000950/1), the European Union Horizon 2020 research and innovation programme (grant agreement No. 647214) and the Research Council of Norway through its Centres of Excellence scheme, project number 262622. R.J. Morton is grateful for support from the UKRI Future Leader Fellowship (RiPSAW - MR/T019891/1) and STFC (ST/T000384/1).
Collections
  • University of St Andrews Research
URI
http://hdl.handle.net/10023/20597

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