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 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 models with Alfvén wave heating in an unstructured corona can explain the observed coronal temperatures compatible with the quiet Sun, while 3D MHD wave heating models including cross-field density structuring are not yet able to account for the heating of coronal loops in active regions to their observed temperature.
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Notes
Small amplitude decayless oscillations were also observed in a prominence with Hinode/SOT (Ning et al. 2009), and of significant and increasing amplitude in a coronal loop with rain (Antolin and Verwichte 2011). Due to the presence of chromospheric material and the associated processes specific to the formation of prominences and coronal rain, the processes responsible for such oscillations may likely be different than those observed in coronal lines.
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Acknowledgements
This paper originated in discussions at ISSI-BJ. T.V.D. was supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 724326) and the C1 grant TRACEspace of Internal Funds KU Leuven (number C14/19/089). H.T. is supported by NSFC Grants No. 11825301 and No. 11790304(11790300). P.A. acknowledges funding from his STFC Ernest Rutherford Fellowship (No. ST/R004285/2). Numerical computations were carried out on Cray XC50 at the Center for Computational Astrophysics, NAOJ. D.J.P. was supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 724326). L.O. acknowledges support by NASA grants NNX16AF78G, 80NSSC18K1131 and NASA Cooperative Agreement NNG11PL10A to CUA. I.A. was supported by project PGC2018-102108-B-I00 from Ministerio de Ciencia, Innovacion y Universidades and FEDER funds. I.D.M. acknowledges support from the 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. D.Y.K. acknowledges support from the STFC consolidated grant ST/T000252/1 and the budgetary funding of Basic Research program No. II.16.
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Oscillatory Processes in Solar and Stellar Coronae
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Van Doorsselaere, T., Srivastava, A.K., Antolin, P. et al. Coronal Heating by MHD Waves. Space Sci Rev 216, 140 (2020). https://doi.org/10.1007/s11214-020-00770-y
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DOI: https://doi.org/10.1007/s11214-020-00770-y