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Observational signatures of transverse magnetohydrodynamic waves and associated dynamic instabilities in coronal flux tubes

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Date
22/02/2017
Author
Antolin, Patrick
De Moortel, Ineke
Doorsselaere, Tom Van
Yokoyama, Takaaki
Funder
Science & Technology Facilities Council
Science & Technology Facilities Council
European Research Council
Grant ID
N/A
ST/N000609/1
647214
Keywords
Magnetohydrodynamics (MHD)
Sun: activity
Sun: corona
Sun: filaments, prominences
Sun: oscillations
QB Astronomy
QC Physics
NDAS
BDC
R2C
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Abstract
Magnetohydrodynamic (MHD) waves permeate the solar atmosphere and constitute potential coronal heating agents. Yet, the waves detected so far may be but a small subset of the true existing wave power. Detection is limited by instrumental constraints but also by wave processes that localize the wave power in undetectable spatial scales. In this study, we conduct 3D MHD simulations and forward modeling of standing transverse MHD waves in coronal loops with uniform and non-uniform temperature variation in the perpendicular cross-section. The observed signatures are largely dominated by the combination of the Kelvin–Helmholtz instability (KHI), resonant absorption, and phase mixing. In the presence of a cross-loop temperature gradient, we find that emission lines sensitive to the loop core catch different signatures compared to those that are more sensitive to the loop boundary and the surrounding corona, leading to an out-of-phase intensity and Doppler velocity modulation produced by KHI mixing. In all of the considered models, common signatures include an intensity and loop width modulation at half the kink period, a fine strand-like structure, a characteristic arrow-shaped structure in the Doppler maps, and overall line broadening in time but particularly at the loop edges. For our model, most of these features can be captured with a spatial resolution of 0″33 and a spectral resolution of 25 km s−1, although we do obtain severe over-estimation of the line width. Resonant absorption leads to a significant decrease of the observed kinetic energy from Doppler motions over time, which is not recovered by a corresponding increase in the line width from phase mixing and KHI motions. We estimate this hidden wave energy to be a factor of 5–10 of the observed value.
Citation
Antolin , P , De Moortel , I , Doorsselaere , T V & Yokoyama , T 2017 , ' Observational signatures of transverse magnetohydrodynamic waves and associated dynamic instabilities in coronal flux tubes ' , Astrophysical Journal , vol. 836 , no. 2 , 219 , pp. 1-23 . https://doi.org/10.3847/1538-4357/aa5eb2
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/aa5eb2
ISSN
0004-637X
Type
Journal article
Rights
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/aa5eb2
Description
This research has received funding from the UK Science and Technology Facilities Council and the European Union Horizon 2020 research and innovation programme (grant agreement No. 647214), and also from JSPS KAKENHI Grant Numbers 25220703 (PI: S. Tsuneta) and 15H03640 (PI: T. Yokoyama). T.V.D. was supported by FWO Vlaanderen’s Odysseus programme, GOA-2015-014 (KU Leuven) and the IAP P7/08 CHARM (Belspo).
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/10256

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