OObservations of the failed eruption bservations of the failed eruption of the magnetic flux rope – of the magnetic flux rope –

a direct application of a direct application of the quadrupthe quadrupolarolar model for a solar flare model for a solar flare

Tomasz MrozekTomasz MrozekAstronomical InstituteAstronomical InstituteUniversity of WrocławUniversity of Wrocław

OObservations of the failed eruption bservations of the failed eruption of the magnetic flux rope – of the magnetic flux rope –

a direct application of a direct application of the quadrupthe quadrupolarolar model for a solar flare model for a solar flare

Tomasz MrozekTomasz MrozekAstronomical InstituteAstronomical InstituteUniversity of WrocławUniversity of Wrocław

50th anniversary

50th anniversary

Sweet, P. A. 1958

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

The quadrupolar model

Uchida et al. 1999Hirose et al. 2001

A quotation from Hirose et al. (2001):

In this simulation (…) the upward motion of the dark filament (…) may eventuallybe arrested by the overlying closed field.

The flare

M6.2 GOES classN14 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

The flare

M6.2 GOES classN14 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

The flare

The image obtained 2 hours after the maximum of the flare.

The flare

Two systems of ribbons wereobserved:

inner – related to the flaringarcade

outer – related to the „post-flaresystem of loops”

The eruption

Abrupt brightening connected with the flare is visible inthe TRACE image obtained on 5:17:30 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)

The eruption

Initial phase,the eruption moves with small, constantvelocity

1Fast evolutionfollowing the strongest HXR peak visible in 25-50 keVrange

2

Deceleration phase. Main front changes its shape. Side eruptions areobserved

3

25-50 keV

Brightenings observed during the deceleration of the main front.

The deceleration value (about 600 m/s2) and the shape of the eruption front show that „something”stopped it. It is possible that two systems of loops were involved in braking the eruption.

Interaction with low-lying loops

Brightenings in the region marked with the red box were observed exactly during the deceleration of the eruption.

Interaction with low-lying loops

inner ribbons

outer ribbons

The lack of observations made with the 1600 Å filter

Interaction with low-lying loops

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

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.

the end of the force driving the movement of the high-lying loops

Interaction with high-lying loops

Clear relationship between an evolutionof the eruption and a height of the high-lyingloops

Summary

The eruption started in a very compact region, not in the large system of loops.The small arcade was visible after.

Decelaration of the eruption The interaction between the eruptionand overlying system of loops

Brightenings outside the flaring structure during the interaction between the eruption and surrounding loops