Relevant heating of the quiet solar corona by Alfvén waves: a result of adiabaticity breakdown

Escande, Dominique; V, Gondret,; Sattin, F.

doi:10.1038/s41598-019-50820-x

Cited by 6 publications

(3 citation statements)

References 31 publications

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“…In principle, AEs could also provide the basis for a plasma heating scheme as supplementary heating of fusion plasmas [10][11][12]. Indeed, heating by Alfvén wave excitation is one of the common mechanisms envisaged for solar corona heating [13][14][15]. Alfvén waves are also thought to play a possible role during tokamak disruptions, as recently investigated both theoretically [16] and experimentally [17].…”

Section: Introductionmentioning

confidence: 99%

Alfvén waves in reversed-field pinch and tokamak ohmic plasmas: nonlinear 3D MHD modeling and comparison with RFX-mod

Kryzhanovskyy¹,

Bonfiglio²,

Cappello³

et al. 2022

Nucl. Fusion

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The properties and possible triggering mechanisms of Alfvén waves in the reversed-field pinch (RFP) and circular tokamak configurations are discussed in the framework of nonlinear 3D MHD modelling. Numerical simulations are performed with the SpeCyl code (S. Cappello and D. Biskamp 1996 Nuclear Fusion) that solves the equations of the viscoresistive MHD model in cylindrical geometry. Configurations with increasing level of complexity are analyzed. First, single-wave numerical solutions have been compared with analytical ones in the simplest case of a uniform axial magnetic field: an excellent agreement is obtained for both the shear Alfvén wave (SAW) and the compressional Alfvén eigenmodes (CAEs). Then, tokamak and RFP configurations have been studied. Phenomena such as phase mixing of SAW, resonant absorption of CAEs and the appearance of the global Alfvén eigenmode (GAE) are described. Finally, the fully 3D RFP case with the typical sawtoothing activity has been investigated, showing for the first time in nonlinear RFP simulations the excitation of Alfvén waves by magnetic reconnection events. Modeling results appear to be consistent with the experimental characterization of Alfvénic activity observed in RFX-mod.

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Section: Introductionmentioning

confidence: 99%

Alfvén waves in reversed-field pinch and tokamak ohmic plasmas: nonlinear 3D MHD modeling and comparison with RFX-mod

Kryzhanovskyy¹,

Bonfiglio²,

Cappello³

et al. 2022

Nucl. Fusion

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“…The maximum energy injected into the corona by spicules may largely balance the total coronal energy losses in quiet regions and possibly also in coronal holes, but not in active regions (Goodman 2014). Another possibility to transport energy between atmospheric layers is by Alfvén waves (Escande et al 2019). Also, loop footpoint reconnection that is both inside and outside active regions (Reale et al 2019;Wang et al 2019) and a forced magnetic reconnection triggered by external perturbation, for example by non-linear magnetohydrodynamic (MHD) waves (Hahm & Kulsrud 1985), can contribute to the process of coronal heating.…”

Section: Introductionmentioning

confidence: 99%

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

Mészárosová

Gömöry

2020

A&A

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Aims. We study the physical properties and behaviour of the solar atmosphere during the GOES X1.6 solar flare on 2014 September 10. Methods. The steady plasma flows and the fast sausage MHD waves were analysed with the wavelet separation method. The magnetically coupled atmosphere and the forced magnetic field reconnection were studied with the help of the Vertical-Current Approximation Non-linear Force-Free Field code. Results. We studied a mechanism of MHD wave transfer from the photosphere without dissipation or reflection before reaching the corona and a mechanism of the wave energy distribution over the solar corona. We report a common behaviour of (extreme)ultraviolet steady plasma flows (speed of 15.3 → 10.9 km s−1) and fast sausage MHD waves (Alfvén speed of 13.7 → 10.3 km s−1 and characteristic periods of 1587 → 1607 s), propagating in cylindrical plasma waveguides of the individual atmospheric layers (photosphere → corona) observed by SDO/AIA/HMI and IRIS space instruments. A magnetically coupled solar atmosphere by a magnetic field flux tube above a sunspot umbra and a magnetic field reconnection forced by the waves were analysed. The solar seismology with trapped, leakage, and tunnelled modes of the waves, dissipating especially in the solar corona, is discussed with respect to its possible contribution to the outer atmosphere heating. Conclusions. We demonstrate that a dispersive nature of fast sausage MHD waves, which can easily generate the leaky and other modes propagating outside of their waveguide, and magnetic field flux tubes connecting the individual atmospheric layers can distribute the magnetic field energy across the active region. This mechanism can contribute to the coronal energy balance and to our knowledge on how the coronal heating is maintained.

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Section: Introductionmentioning

confidence: 99%

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

Meszarosova,

Gomory

2020

Preprint

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Aims. We study the physical properties and behaviour of the solar atmosphere during the GOES X1.6 solar flare on 2014 September 10.Methods. The steady plasma flows and the fast sausage MHD waves were analysed with the wavelet separation method. The magnetically coupled atmosphere and the forced magnetic field reconnection were studied with the help of the Vertical-Current Approximation Non-linear Force-Free Field code.Results. We studied a mechanism of MHD wave transfer from the photosphere without dissipation or reflection before reaching the corona and a mechanism of the wave energy distribution over the solar corona. We report a common behaviour of (extreme)ultraviolet steady plasma flows (speed of 15.3→10.9 km s −1 ) and fast sausage MHD waves (Alfvén speed of 13.7→10.3 km s −1 and characteristic periods of 1 587→1 607 s), propagating in cylindrical plasma waveguides of the individual atmospheric layers (photosphere→corona) observed by SDO/AIA/HMI and IRIS space instruments. A magnetically coupled solar atmosphere by a magnetic field flux tube above a sunspot umbra and a magnetic field reconnection forced by the waves were analysed. The solar seismology with trapped, leakage, and tunnelled modes of the waves, dissipating especially in the solar corona, is discussed with respect to its possible contribution to the outer atmosphere heating.Conclusions. We demonstrate that a dispersive nature of fast sausage MHD waves, which can easily generate the leaky and other modes propagating outside of their waveguide, and magnetic field flux tubes connecting the individual atmospheric layers can distribute the magnetic field energy across the active region. This mechanism can contribute to the coronal energy balance and to our knowledge on how the coronal heating is maintained.

show abstract

Relevant heating of the quiet solar corona by Alfvén waves: a result of adiabaticity breakdown

Cited by 6 publications

References 31 publications

Alfvén waves in reversed-field pinch and tokamak ohmic plasmas: nonlinear 3D MHD modeling and comparison with RFX-mod

Alfvén waves in reversed-field pinch and tokamak ohmic plasmas: nonlinear 3D MHD modeling and comparison with RFX-mod

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

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