Slow Magnetoacoustic Waves in Two-Ribbon Flares: Difference between revisions
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on this problem. | on this problem. | ||
According to the more or less standard picture of large 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. | According to the more or less standard picture of large 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 [http://en.wikipedia.org/wiki/Current_sheet/ 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 | 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 ortogonal to the loop planes - along the flaring arcade axis and the magnetic neutral line. But often large, eruptive, two-ribbon flares develop predominantly just in this direction - in a number of observations energy release is seen to propagate mainly along the flaring arcade axis. In particular, RHESSI made a great contribution in this issue observing an impressive motions of non-thermal hard X-ray sources along the flare arcade axis and the neutral line (e.g. see [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=4/ Nugget 4] and [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=6/ Nugget 6]). | ||
== Bright Peculiarities of the Energy Release Source Motions Along the Flare Arcade Axis == | |||
Such type of energy release source motions in two-ribbon solar flares has two bright and exciting features: | |||
# the still unknown triggering disturbances observed to propagate along the flare arcade axis at the speed of a few tens km/s, well below the Alfven and sound speeds; | |||
# it is often accompanied by wavetrains of quasi-periodic pulsations of non-thermal hard X-ray and microwave emissions with typical periods from a few seconds up to several tens of seconds. | |||
Revision as of 11:06, 5 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 large 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 ortogonal to the loop planes - along the flaring arcade axis and the magnetic neutral line. But often large, eruptive, two-ribbon flares develop predominantly just in this direction - in a number of observations energy release is seen to propagate mainly along the flaring arcade axis. In particular, RHESSI made a great contribution in this issue observing an impressive motions of non-thermal hard X-ray sources along the flare arcade axis and the neutral line (e.g. see Nugget 4 and Nugget 6).
Bright Peculiarities of the Energy Release Source Motions Along the Flare Arcade Axis
Such type of energy release source motions in two-ribbon solar flares has two bright and exciting features:
- the still unknown triggering disturbances observed to propagate along the flare arcade axis at the speed of a few tens km/s, well below the Alfven and sound speeds;
- it is often accompanied by wavetrains of quasi-periodic pulsations of non-thermal hard X-ray and microwave emissions with typical periods from a few seconds up to several tens of seconds.