Skip to content

Research at St Andrews

Coronal heating by MHD waves

Research output: Contribution to journalArticlepeer-review

Standard

Coronal heating by MHD waves. / Van Doorsselaere, Tom; Srivastava, Abhishek K.; Antolin, Patrick; Magyar, Norbert; Vasheghani Farahani, Soheil; Tian, Hui; Kolotkov, Dmitrii; Ofman, Leon; Guo, Mingzhe; Arregui, Iñigo; De Moortel, Ineke; Pascoe, David.

In: Space Science Reviews, Vol. 216, No. 8, 140 , 02.12.2020.

Research output: Contribution to journalArticlepeer-review

Harvard

Van Doorsselaere, T, Srivastava, AK, Antolin, P, Magyar, N, Vasheghani Farahani, S, Tian, H, Kolotkov, D, Ofman, L, Guo, M, Arregui, I, De Moortel, I & Pascoe, D 2020, 'Coronal heating by MHD waves', Space Science Reviews, vol. 216, no. 8, 140 . https://doi.org/10.1007/s11214-020-00770-y

APA

Van Doorsselaere, T., Srivastava, A. K., Antolin, P., Magyar, N., Vasheghani Farahani, S., Tian, H., Kolotkov, D., Ofman, L., Guo, M., Arregui, I., De Moortel, I., & Pascoe, D. (2020). Coronal heating by MHD waves. Space Science Reviews, 216(8), [140 ]. https://doi.org/10.1007/s11214-020-00770-y

Vancouver

Van Doorsselaere T, Srivastava AK, Antolin P, Magyar N, Vasheghani Farahani S, Tian H et al. Coronal heating by MHD waves. Space Science Reviews. 2020 Dec 2;216(8). 140 . https://doi.org/10.1007/s11214-020-00770-y

Author

Van Doorsselaere, Tom ; Srivastava, Abhishek K. ; Antolin, Patrick ; Magyar, Norbert ; Vasheghani Farahani, Soheil ; Tian, Hui ; Kolotkov, Dmitrii ; Ofman, Leon ; Guo, Mingzhe ; Arregui, Iñigo ; De Moortel, Ineke ; Pascoe, David. / Coronal heating by MHD waves. In: Space Science Reviews. 2020 ; Vol. 216, No. 8.

Bibtex - Download

@article{b4167872b3764708b24a7eb25a62444c,
title = "Coronal heating by MHD waves",
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 Alfv{\'e}n 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.",
keywords = "Sun: corona, Sun: waves",
author = "{Van Doorsselaere}, Tom and Srivastava, {Abhishek K.} and Patrick Antolin and Norbert Magyar and {Vasheghani Farahani}, Soheil and Hui Tian and Dmitrii Kolotkov and Leon Ofman and Mingzhe Guo and I{\~n}igo Arregui and {De Moortel}, Ineke and David Pascoe",
note = "This paper originated in discussions at ISSI-BJ. T.V.D. was supported by the European Research Council (ERC) under the European Union{\textquoteright}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{\textquoteright}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.",
year = "2020",
month = dec,
day = "2",
doi = "10.1007/s11214-020-00770-y",
language = "English",
volume = "216",
journal = "Space Science Reviews",
issn = "0038-6308",
publisher = "Springer",
number = "8",

}

RIS (suitable for import to EndNote) - Download

TY - JOUR

T1 - Coronal heating by MHD waves

AU - Van Doorsselaere, Tom

AU - Srivastava, Abhishek K.

AU - Antolin, Patrick

AU - Magyar, Norbert

AU - Vasheghani Farahani, Soheil

AU - Tian, Hui

AU - Kolotkov, Dmitrii

AU - Ofman, Leon

AU - Guo, Mingzhe

AU - Arregui, Iñigo

AU - De Moortel, Ineke

AU - Pascoe, David

N1 - 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.

PY - 2020/12/2

Y1 - 2020/12/2

N2 - 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.

AB - 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.

KW - Sun: corona

KW - Sun: waves

U2 - 10.1007/s11214-020-00770-y

DO - 10.1007/s11214-020-00770-y

M3 - Article

VL - 216

JO - Space Science Reviews

JF - Space Science Reviews

SN - 0038-6308

IS - 8

M1 - 140

ER -

Related by author

  1. The effects of driving time scales on heating in a coronal arcade

    Howson, T. A., De Moortel, I. & Fyfe, L., 17 Sep 2020, (Accepted/In press) In: Astronomy & Astrophysics. 14 p.

    Research output: Contribution to journalArticlepeer-review

  2. Forward modelling of MHD Waves in braided magnetic fields

    Fyfe, L., Howson, T. A. & De Moortel, I., 15 Sep 2020, (Accepted/In press) In: Astronomy & Astrophysics.

    Research output: Contribution to journalArticlepeer-review

  3. Effect of coronal loop structure on wave heating by phase mixing

    Pagano, P., De Moortel, I. & Morton, R., 9 Sep 2020, (Accepted/In press) In: Astronomy & Astrophysics.

    Research output: Contribution to journalArticlepeer-review

  4. Alfvén on heating by waves

    De Moortel, I., Falconer, I. & Stack, R., Apr 2020, In: Astronomy & Geophysics. 61, 2, p. 2.34–2.39

    Research output: Contribution to journalArticle

  5. Phase mixing and wave heating in a complex coronal plasma

    Howson, T. A., De Moortel, I. & Reid, J., Apr 2020, In: Astronomy & Astrophysics. 636, 13 p., A40.

    Research output: Contribution to journalArticlepeer-review

Related by journal

  1. Decoding the pre-eruptive magnetic field configurations of coronal mass ejections

    Patsourakos, S., Vourlidas, A., Török, T., Kliem, B., Antiochos, S. K., Archontis, V., Aulanier, G., Cheng, X., Chintzoglou, G., Georgoulis, M. K., Green, L. M., Leake, J. E., Moore, R., Nindos, A., Syntelis, P., Yardley, S. L., Yurchyshyn, V. & Zhang, J., 6 Nov 2020, In: Space Science Reviews. 216, 8, 131.

    Research output: Contribution to journalArticlepeer-review

  2. Mission to planet Earth: the first two billion years

    Stueeken, E. E., Som, S. M., Claire, M., Rugheimer, S., Scherf, M., Sproß, L., Tosi, N., Ueno, Y. & Lammer, H., 16 Mar 2020, In: Space Science Reviews. 216, 37 p., 31.

    Research output: Contribution to journalReview articlepeer-review

  3. The isotopic imprint of life on an evolving planet

    Lloyd, M., McClelland, H., Antler, G., Bradley, A., Halevy, I., Junium, C., Wankel, S. & Zerkle, A. L., 6 Oct 2020, In: Space Science Reviews. 216, 112.

    Research output: Contribution to journalReview articlepeer-review

  4. Global non-potential magnetic models of the solar corona during the March 2015 eclipse

    Yeates, A. R., Amari, T., Contopoulos, I., Feng, X., Mackay, D. H., Mikić, Z., Wiegelmann, T., Hutton, J., Lowder, C. A., Morgan, H., Petrie, G., Rachmeler, L. A., Upton, L. A., Canou, A., Chopin, P., Downs, C., Druckmüller, M., Linker, J. A., Seaton, D. B. & Török, T., Aug 2018, In: Space Science Reviews. 214, 5, 27 p., 99.

    Research output: Contribution to journalArticlepeer-review

ID: 271739054

Top