Relaxation and Heating Triggered by Nonlinear Kink Instability: Application to Solar Flares and Coronal Heating

2012 ◽  
pp. 69-75
Author(s):  
Philippa K. Browning ◽  
Michael R. Bareford ◽  
Mykola Gordovskyy
Keyword(s):  
Solar Flares ◽  
Coronal Heating ◽  
Kink Instability

scholarly journals The Role of Magnetic Helicity in Solar Flares

2005 ◽  
Vol 13 ◽  
pp. 128-131
Author(s):  
Mark G. Linton
Keyword(s):  
Solar Flares ◽  
Magnetic Energy ◽  
Active Regions ◽  
Excess Energy ◽  
Flux Tubes ◽  
Surplus Energy ◽  
Coronal Magnetic Fields ◽  
Kink Instability ◽  
Magnetic Energy Release

AbstractHelicity in coronal magnetic fields, often occurring in the form of twisted or sheared fields, can provide surplus energy which is available for release in solar flares. In this paper, several models of how this extra, non-potential, energy can be released will be reviewed. For example, twisted flux tubes can release excess energy via the kink instability. Or energy can be released via a transfer of helicity between different magnetic tubes. For untwisted field, the mutual helicity between flux tubes provides a measure of the shear in the fields, and therefore how much energy is available for release in a flare. For twisted flux tubes, the twist helicity of each tube in combination with the mutual helicity between the tubes dictate what type of reconnection the tubes can undergo and how much energy is available for release. Measuring the helicity of coronal active regions, and studying how this helicity affects magnetic energy release is therefore vital for our understanding of and our ability to predict solar flares.

LATTICE MODELS FOR SOLAR FLARES AND CORONAL HEATING

2006 ◽  
Vol 2 (S233) ◽  
pp. 481
Author(s):  
O. Podladchikova ◽  
B. Lefebvre
Keyword(s):  
Solar Flares ◽  
Lattice Models ◽  
Coronal Heating

Geometric Effects in Avalanche Models of Solar Flares: Implications for Coronal Heating

2001 ◽  
Vol 563 (2) ◽  
pp. L165-L168 ◽  
Author(s):  
S. W. McIntosh ◽  
P. Charbonneau
Keyword(s):  
Solar Flares ◽  
Coronal Heating ◽  
Geometric Effects ◽  
Avalanche Models

scholarly journals Magnetic Instabilities in Stellar Atmospheres

1983 ◽  
Vol 71 ◽  
pp. 545-558
Author(s):  
E.R. Priest
Keyword(s):  
Magnetic Field ◽  
Solar Flares ◽  
Impulsive Phase ◽  
Coronal Magnetic Field ◽  
Stellar Atmospheres ◽  
Stored Energy ◽  
Global Instability ◽  
Magnetohydrodynamic Instability ◽  
Kink Instability ◽  
The Magnetic Field

ABSTRACT.The extensive theory for magnetohydrodynamic instability of a flux tube is briefly reviewed, together with its application to tokamaks and solar flares. In a star a single coronal loop whose footprints are anchored in the dense photosphere may become unstable to the kink instability when it is twisted too much. Magnetic arcades may also be subject to an eruptive instability when they are sheared too much. After the eruption the magnetic field closes back down by reconnection and continues to heat the plasma long after the impulsive phase. Global instability of a large part of the coronal magnetic field is also possible when the stored energy is too great.

scholarly journals Coronal Heating by Nanoflares and the Variability of the Occurrence Frequency in Solar Flares

1996 ◽  
Vol 469 (2) ◽  
pp. L135-L138 ◽  
Author(s):  
Manolis K. Georgoulis ◽  
Loukas Vlahos
Keyword(s):  
Solar Flares ◽  
Coronal Heating ◽  
Occurrence Frequency

Solar flares, microflares, nanoflares, and coronal heating

Solar Physics ◽  
1991 ◽  
Vol 133 (2) ◽  
pp. 357-369 ◽  
Author(s):  
H. S. Hudson
Keyword(s):  
Solar Flares ◽  
Coronal Heating

Kink instability of solar coronal loops as the cause of solar flares

Solar Physics ◽  
1979 ◽  
Vol 64 (2) ◽  
pp. 303-321 ◽  
Author(s):  
A. W. Hood ◽  
E. R. Priest
Keyword(s):  
Solar Flares ◽  
Coronal Loops ◽  
Kink Instability ◽  
Solar Coronal

Trigger mechanisms of the major solar flares

2019 ◽  
Vol 15 (S354) ◽  
pp. 392-406
Author(s):  
Shuhong Yang
Keyword(s):  
Active Region ◽  
Solar Flares ◽  
Magnetic Energy ◽  
Active Regions ◽  
Polarity Inversion ◽  
Strong Gradient ◽  
Cycle 24 ◽  
Kink Instability ◽  
Shearing Motion ◽  
Trigger Mechanisms

AbstractSolar flares, suddenly releasing a large amount of magnetic energy, are one of the most energetic phenomena on the Sun. For the major flares (M- and X-class flares), there exist strong-gradient polarity-inversion lines in the pre-flare photospheric magnetograms. Some parameters (e.g., electric current, shear angle, free energy) are used to measure the magnetic non-potentiality of active regions, and the kernels of major flares coincide with the highly non-potential regions. Magnetic flux emergence and cancellation, shearing motion, and sunspot rotation observed in the photosphere are deemed to play an important role in the energy buildup and flare trigger. Solar active region 12673 produced many major flares, among which the X9.3 flare is the largest one in solar cycle 24. According to the newly proposed block-induced eruption model, the block-induced complex structures built the flare-productive active region and the X9.3 flare was triggered by an erupting filament due to the kink instability.

Studies of the structure and dynamics of theDregion of the polar ionosphere during solar flares in April 2004

2006 ◽  
Vol 6 (2) ◽  
Author(s):  
V. D. Tereshchenko ◽  
E. B. Vasil'ev ◽  
O. F. Ogloblina ◽  
V. A. Tereshchenko ◽  
S. M. Chernyakov
Keyword(s):  
Solar Flares ◽  
Polar Ionosphere ◽  
Structure And Dynamics
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