Slow Magnetoacoustic Waves in Two-Ribbon Flares
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== Introduction == | == Introduction == | ||
| - | The understanding of three-dimensional morphology and dynamics of large, eruptive, two-ribbon flares can shed light | + | The physical processes operating in solar energy releases are still unclear and under very active scrutiny. The understanding of three-dimensional morphology and dynamics of large, eruptive, two-ribbon flares can shed light |
| - | on | + | on this problem. |
| - | According to the more or less standard picture of eruptive flares oppositely directed magnetic field lines being in the form of arcade of magnetic loops are stretched by some non-stationary agent (e.g. by an erupting twisted magnetic flux rope or filament) to form a quasi-vertical current sheet in the corona. Here, in the current sheet, magnetic field lines can reconnect converting free magnetic energy to thermal and kinetic energy of plasma and charged particles causing a multitude of secondary flaring effects. Unfortunately, the "standard" picture is essentially two-dimensional. Being capable to represent a lot of observational effects in the planes of magnetic loops, it does not represent flare development in the third direction perpendicular to the loop planes - along the flaring arcade axis | + | According to the more or less standard picture of eruptive flares oppositely directed magnetic field lines being in the form of arcade of magnetic loops are stretched by some non-stationary agent (e.g. by an erupting twisted magnetic flux rope or filament) to form a quasi-vertical current sheet in the corona. Here, in the current sheet, magnetic field lines can reconnect converting free magnetic energy to thermal and kinetic energy of plasma and charged particles causing a multitude of secondary flaring effects. Unfortunately, the "standard" picture is essentially two-dimensional. Being capable to represent a lot of observational effects in the planes of magnetic loops, it does not represent flare development in the third direction perpendicular to the loop planes - along the flaring arcade axis and the neutral line. |
| - | Nevertheless, in a number of observations energy release is seen to propagate just in this direction. | + | Nevertheless, in a number of observations energy release is seen to propagate just in this direction - along the flaring arcade axis. What is exciting here is that someone triggering disturbances observed to propagate at the speed of a few tens km/s, well below the Alfven and sound speeds. |
Revision as of 19:48, 4 March 2011
Introduction
The physical processes operating in solar energy releases are still unclear and under very active scrutiny. The understanding of three-dimensional morphology and dynamics of large, eruptive, two-ribbon flares can shed light on this problem.
According to the more or less standard picture of eruptive flares oppositely directed magnetic field lines being in the form of arcade of magnetic loops are stretched by some non-stationary agent (e.g. by an erupting twisted magnetic flux rope or filament) to form a quasi-vertical current sheet in the corona. Here, in the current sheet, magnetic field lines can reconnect converting free magnetic energy to thermal and kinetic energy of plasma and charged particles causing a multitude of secondary flaring effects. Unfortunately, the "standard" picture is essentially two-dimensional. Being capable to represent a lot of observational effects in the planes of magnetic loops, it does not represent flare development in the third direction perpendicular to the loop planes - along the flaring arcade axis and the neutral line.
Nevertheless, in a number of observations energy release is seen to propagate just in this direction - along the flaring arcade axis. What is exciting here is that someone triggering disturbances observed to propagate at the speed of a few tens km/s, well below the Alfven and sound speeds.
