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Solar coronal heating by magnetosonic waves
Monthly Notices of the Royal Astronomical Society, 2001Solar coronal heating by magnetohydrodynamic (MHD) waves is investigated. ultraviolet (UV) and X-ray emission lines of the corona show non-thermal broadenings. The wave rms velocities inferred from these observations are of the order of 25–60 km s−1. Assuming that these values are not negligible, we solved MHD equations in a quasi-linear approximation,
Pekunlu, ER, Cakirli, O, Ozetken, E
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Nonlinear wave heating of solar coronal loops.
Astronomy and Astrophysics, 1997The heating of magnetically closed structures (loops) in the solar corona by the resonant absorption of incident waves is studied by means of numerical simulations in the framework of nonlinear resistive magnetohydrodynamics (MHD). It is shown that the dynamics in the resonant layer is indeed very nonlinear for typical coronal parameters. The effect of
Poedts, S., Goedbloed, J.P.
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Observational Research on Solar Coronal Waves.
1976Abstract : An observational search has been made for intensity fluctuations associated with the wave motions that are thought to heat the corona. Brightness changes in the coronal green line (Fe XIV lambda 5303) and the coronal continuum were measured with the University of Hawaii's polarimeter at Mt. Haleakala.
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Solar coronal heating by high-frequency dispersive Alfvén waves
Solar Physics, 1999It is shown that high-frequency dispersive kinetic Alfven waves can cause significant electron heating in the solar corona. The heating is produced by collisionless electron Landau dissipation of the parallel electron current associated with high-frequency dispersive kinetic Alfven waves, which have a parallel electric field.
Shukla, P. +3 more
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Solar Coronal Heating via Alfvén Wave Turbulence
AIP Conference Proceedings, 2010A short review is given about the self‐consistent MHD model of solar coronal heating recently proposed by Bigot et al. (2008) in which the dynamical effect of the background magnetic field along a coronal structure is taken into account through exact results from Alfven wave turbulence.
B. Bigot +7 more
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Impulsively Generated Wave Trains in a Solar Coronal Loop
IEEE Transactions on Plasma Science, 2010Impulsively generated fast magnetoacoustic wave trains in a solar coronal loop are numerically studied. The problem is considered as 2-D in space, and for the description, the full set of magnetohydrodynamic (MHD) equations is used. The numerical solution of the MHD equations is performed by means of the Lax-Wendroff algorithm on a uniformly structured
Petr Jelinek, Marian Karlicky
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Reflection of Alfvén Waves and Heating in Solar Coronal Holes
1991Using a simple model coronal hole, we estimate the short-period period limit for the reflection of Alfven waves in solar coronal holes. Waves with periods longer than this limit are strongly reflected and blocked from escaping into the solar wind; waves with periods appreciably shorter than this limit suffer little reflection and freely escape into the
Ronald L. Moore +3 more
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Solar global coronal wave front velocity estimation
PHYSICS OF SPACE : Proceedings of the 53-st All-Russian with international participation student scientific conferenceGlobal coronal waves are one of the manifestations of solar activity. They are generated as a result of impulsive energy releases such as solar flares, coronal mass ejections, and jets. The nature of global waves is not completely clear. Estimations of the wave parameters are needed.
D. D. Kuziy, E. G. Kupriyanova
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Magnetohydrodynamic Waves in Open Coronal Structures
Space Science Reviews, 2021Tom Van Doorsselaere +2 more
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