Coronal Heating by MHD Waves
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Coronal Heating by MHD Waves Tom Van Doorsselaere1 · Abhishek K. Srivastava2 · Patrick Antolin3 · Norbert Magyar4 · Soheil Vasheghani Farahani5 · Hui Tian6,7 · Dmitrii Kolotkov4,8 · Leon Ofman9,10 · Mingzhe Guo11,1 · Iñigo Arregui12,13 · Ineke De Moortel14,15 · David Pascoe1
Received: 14 July 2020 / Accepted: 12 November 2020 © Springer Nature B.V. 2020
Abstract The heating of the solar chromosphere and corona to the observed high temperatures, imply the presence of ongoing heating that balances the strong radiative and thermal conduction losses expected in the solar atmosphere. It has been theorized for decades that the required heating mechanisms of the chromospheric and coronal parts of the active regions, quiet-Sun, and coronal holes are associated with the solar magnetic fields. However, the exact physical process that transport and dissipate the magnetic energy which ultimately leads to the solar plasma heating are not yet fully understood. The current understanding Oscillatory Processes in Solar and Stellar Coronae Edited by Valery M. Nakariakov, Dipankar Banerjee, Bo Li, Tongjiang Wang, Ivan Zimovets and Maurizio Falanga
B T. Van Doorsselaere
[email protected]
1
Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B bus 2400, 3001 Leuven, Belgium
2
Department of Physics, Indian Institute of Technology (BHU), Varanasi 221005, India
3
Department of Mathematics, Physics and Electrical Engineering, Northumbria University, Newcastle Upon Tyne, NE1 8ST, UK
4
Centre for Fusion, Space and Astrophysics, Physics Department, University of Warwick, Coventry CV4 7AL, UK
5
Department of Physics, Tafresh University, Tafresh 39518 79611, Iran
6
School of Earth and Space Sciences, Peking University, Beijing 100871, China
7
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
8
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk 664033, Russia
9
Department of Physics, Catholic University of America, Washington, DC, USA
10
NASA Goddard Space Flight Center, Greenbelt, MD, USA
11
Institute of Space Sciences, Shandong University, Weihai 264209, People’s Republic of China
12
Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
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of coronal heating relies on two main mechanism: reconnection and MHD waves that may have various degrees of importance in different coronal regions. In this review we focus on recent advances in our understanding of MHD wave heating mechanisms. First, we focus on giving an overview of observational results, where we show that different wave modes have been discovered in the corona in the last decade, many of which are associated with a significant energy flux, either generated in situ or pumped from the lower solar atmosphere. Afterwards, we summarise the recent findings of numerical modelling of waves, motivated by the observational results. Despite the advances, only 3D MHD mod
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