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Phase mixing and wave heating in a complex coronal plasma

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Phase mixing and wave heating in a complex coronal plasma. / Howson, Thomas Alexander; De Moortel, Ineke; Reid, Jack.

In: Astronomy & Astrophysics, Vol. 636, A40, 04.2020.

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Harvard

Howson, TA, De Moortel, I & Reid, J 2020, 'Phase mixing and wave heating in a complex coronal plasma', Astronomy & Astrophysics, vol. 636, A40. https://doi.org/10.1051/0004-6361/201937332

APA

Howson, T. A., De Moortel, I., & Reid, J. (2020). Phase mixing and wave heating in a complex coronal plasma. Astronomy & Astrophysics, 636, [A40]. https://doi.org/10.1051/0004-6361/201937332

Vancouver

Howson TA, De Moortel I, Reid J. Phase mixing and wave heating in a complex coronal plasma. Astronomy & Astrophysics. 2020 Apr;636. A40. https://doi.org/10.1051/0004-6361/201937332

Author

Howson, Thomas Alexander ; De Moortel, Ineke ; Reid, Jack. / Phase mixing and wave heating in a complex coronal plasma. In: Astronomy & Astrophysics. 2020 ; Vol. 636.

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@article{1d0c1084cd80410fb8cc7c1f271a22d3,
title = "Phase mixing and wave heating in a complex coronal plasma",
abstract = "Aims. We investigate the formation of small scales and the related dissipation of magnetohydronamic (MHD) wave energy through non-linear interactions of counter-propagating, phase-mixed Alfv{\'e}nic waves in a complex magnetic field. Methods. We conducted fully three-dimensional, non-ideal MHD simulations of transverse waves in complex magnetic field configurations. Continuous wave drivers were imposed on the foot points of magnetic field lines and the system was evolved for several Alfv{\'e}n travel times. Phase-mixed waves were allowed to reflect off the upper boundary and the interactions between the resultant counter-streaming wave packets were analysed. Results. The complex nature of the background magnetic field encourages the development of phase mixing throughout the numerical domain, leading to a growth in alternating currents and vorticities. Counter-propagating phase-mixed MHD wave modes induce a cascade of energy to small scales and result in more efficient wave energy dissipation. This effect is enhanced in simulations with more complex background fields. High-frequency drivers excite localised field line resonances and produce efficient wave heating. However, this relies on the formation of large amplitude oscillations on resonant field lines. Drivers with smaller frequencies than the fundamental frequencies of field lines are not able to excite resonances and thus do not inject sufficient Poynting flux to power coronal heating. Even in the case of high-frequency oscillations, the rate of dissipation is likely too slow to balance coronal energy losses, even within the quiet Sun. Conclusions. For the case of the generalised phase-mixing presented here, complex background field structures enhance the rate of wave energy dissipation. However, it remains difficult for realistic wave drivers to inject sufficient Poynting flux to heat the corona. Indeed, significant heating only occurs in cases which exhibit oscillation amplitudes that are much larger than those currently observed in the solar atmosphere.",
keywords = "Sun: corona, Sun: magnetic fields, Sun: oscillations, Magnetohydrodyanmics (MHD)",
author = "Howson, {Thomas Alexander} and {De Moortel}, Ineke and Jack Reid",
note = "Funding: UK Science and Technology Facilities Council (consolidated grants ST/N000609/1 and ST/S000402/1); European Union Horizon 2020 research and innovation programme (grant agreement No. 647214); Research Council of Norway through its Centres of Excellence scheme, project number 262622 (IDM); Carnegie Trust for the Universities of Scotland (JR).",
year = "2020",
month = apr,
doi = "10.1051/0004-6361/201937332",
language = "English",
volume = "636",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "EDP SCIENCES S A",

}

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TY - JOUR

T1 - Phase mixing and wave heating in a complex coronal plasma

AU - Howson, Thomas Alexander

AU - De Moortel, Ineke

AU - Reid, Jack

N1 - Funding: UK Science and Technology Facilities Council (consolidated grants ST/N000609/1 and ST/S000402/1); European Union Horizon 2020 research and innovation programme (grant agreement No. 647214); Research Council of Norway through its Centres of Excellence scheme, project number 262622 (IDM); Carnegie Trust for the Universities of Scotland (JR).

PY - 2020/4

Y1 - 2020/4

N2 - Aims. We investigate the formation of small scales and the related dissipation of magnetohydronamic (MHD) wave energy through non-linear interactions of counter-propagating, phase-mixed Alfvénic waves in a complex magnetic field. Methods. We conducted fully three-dimensional, non-ideal MHD simulations of transverse waves in complex magnetic field configurations. Continuous wave drivers were imposed on the foot points of magnetic field lines and the system was evolved for several Alfvén travel times. Phase-mixed waves were allowed to reflect off the upper boundary and the interactions between the resultant counter-streaming wave packets were analysed. Results. The complex nature of the background magnetic field encourages the development of phase mixing throughout the numerical domain, leading to a growth in alternating currents and vorticities. Counter-propagating phase-mixed MHD wave modes induce a cascade of energy to small scales and result in more efficient wave energy dissipation. This effect is enhanced in simulations with more complex background fields. High-frequency drivers excite localised field line resonances and produce efficient wave heating. However, this relies on the formation of large amplitude oscillations on resonant field lines. Drivers with smaller frequencies than the fundamental frequencies of field lines are not able to excite resonances and thus do not inject sufficient Poynting flux to power coronal heating. Even in the case of high-frequency oscillations, the rate of dissipation is likely too slow to balance coronal energy losses, even within the quiet Sun. Conclusions. For the case of the generalised phase-mixing presented here, complex background field structures enhance the rate of wave energy dissipation. However, it remains difficult for realistic wave drivers to inject sufficient Poynting flux to heat the corona. Indeed, significant heating only occurs in cases which exhibit oscillation amplitudes that are much larger than those currently observed in the solar atmosphere.

AB - Aims. We investigate the formation of small scales and the related dissipation of magnetohydronamic (MHD) wave energy through non-linear interactions of counter-propagating, phase-mixed Alfvénic waves in a complex magnetic field. Methods. We conducted fully three-dimensional, non-ideal MHD simulations of transverse waves in complex magnetic field configurations. Continuous wave drivers were imposed on the foot points of magnetic field lines and the system was evolved for several Alfvén travel times. Phase-mixed waves were allowed to reflect off the upper boundary and the interactions between the resultant counter-streaming wave packets were analysed. Results. The complex nature of the background magnetic field encourages the development of phase mixing throughout the numerical domain, leading to a growth in alternating currents and vorticities. Counter-propagating phase-mixed MHD wave modes induce a cascade of energy to small scales and result in more efficient wave energy dissipation. This effect is enhanced in simulations with more complex background fields. High-frequency drivers excite localised field line resonances and produce efficient wave heating. However, this relies on the formation of large amplitude oscillations on resonant field lines. Drivers with smaller frequencies than the fundamental frequencies of field lines are not able to excite resonances and thus do not inject sufficient Poynting flux to power coronal heating. Even in the case of high-frequency oscillations, the rate of dissipation is likely too slow to balance coronal energy losses, even within the quiet Sun. Conclusions. For the case of the generalised phase-mixing presented here, complex background field structures enhance the rate of wave energy dissipation. However, it remains difficult for realistic wave drivers to inject sufficient Poynting flux to heat the corona. Indeed, significant heating only occurs in cases which exhibit oscillation amplitudes that are much larger than those currently observed in the solar atmosphere.

KW - Sun: corona

KW - Sun: magnetic fields

KW - Sun: oscillations

KW - Magnetohydrodyanmics (MHD)

U2 - 10.1051/0004-6361/201937332

DO - 10.1051/0004-6361/201937332

M3 - Article

VL - 636

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A40

ER -

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