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 Wrocław 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 Wrocław

50 th anniversary

Sweet, P. A 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 Hirose et al 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.

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

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

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

The flare Two systems of ribbons were observed: inner – related to the flaring arcade outer – related to the „post-flare system of loops”

The eruption Abrupt brightening connected with the flare is visible in the 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, constant velocity 1 Fast evolution following the strongest HXR peak visible in keV range 2 Deceleration phase. Main front changes its shape. Side eruptions are observed keV H[km]

Brightenings observed during the deceleration of the main front. The deceleration value (about 600 m/s 2 ) 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

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 evolution of the eruption and a height of the high-lying loops

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