Slajd 1

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Observations of the failed eruption of the
magnetic flux rope a direct application of
the quadrupolar model for a solar
flare Tomasz Mrozek Astronomical
Institute University of Wroclaw
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50th anniversary
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50th anniversary
50 years ago Sweet suggested that flares may
occur in the quadrupolar magnetic filed
configuration. The quadrupolar model describes
observed features of solar flares in a more
natural way. For some reason much of the
theoretical work has ignored this kind of
complexity and try to develop the theory of
simple, bipolar configuration the standard
model
Sweet, P. A. 1958
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The quadrupolar model
A quotation from Hirose et al. (2001) In this
simulation () the upward motion of the dark
filament () may eventually be arrested by the
overlying closed field.
Uchida et al. 1999 Hirose et al. 2001
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The flare
M6.2 GOES class N14 W61 RHESSI entire
event TRACE 171 Å (several seconds cadence,
entire event) 1600 Å (several second
cadence, decay phase) GOES SXI several,
saturated images SOHO LASCO no CME reported
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The flare
M6.2 GOES class N14 W61 RHESSI entire
event TRACE 171 Å (several seconds cadence,
entire event) 1600 Å (several second
cadence, decay phase) GOES SXI several,
saturated images SOHO LASCO no CME reported
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The flare
The image obtained 2 hours after the maximum of
the flare.
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The flare
Two systems of ribbons were observed inner
related to the flaring arcade outer related to
the post-flare system of loops
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The eruption
Abrupt brightening connected with the flare is
visible in the TRACE image obtained on 51730
UT The eruption of the magnetic flux tube is
observed several seconds after The eruption
started in a very compact region (about 3000 km
in diameter)
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The eruption
Hkm
25-50 keV
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Interaction with low-lying loops
The deceleration value (about 600 m/s2) and the
shape of the eruption front show that
somethingstopped it. It is possible that two
systems of loops were involved in braking the
eruption.
Brightenings observed during the deceleration of
the main front.
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Interaction with low-lying loops
Brightenings in the region marked with the red
box were observed exactly during the
deceleration of the eruption.
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Interaction with low-lying loops
inner ribbons
outer ribbons
The lack of observations made with the 1600 Å
filter
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Interaction with low-lying loops
Spatial relationship between decelerated front
and tops of loops visible later Brightenings
observed during the braking of the eruption HXR
source (6-12 keV) spatially correlated with the
decelerated front
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Interaction with high-lying loops
Above the erupting structure we observed the
system of high-lying loops. These loops changed
their height as the eruption evolved.
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Interaction with high-lying loops
Clear relationship between an evolution of the
eruption and a height of the high-lying loops
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Summary
The interaction between the eruption and
overlying system of loops
Decelaration of the eruption
Brightenings outside the flaring structure during
the interaction between the eruption and
surrounding loops
The eruption started in a very compact region,
not in the large system of loops. The small
arcade was visible after.