1 / 17

O bservations of the failed eruption of the magnetic flux rope – a direct application of

O bservations of the failed eruption of the magnetic flux rope – a direct application of the quadrup olar model for a solar flare Tomasz Mrozek Astronomical Institute University of Wrocław. 50 th anniversary. 50 th anniversary. 50 years ago Sweet suggested that flares

flynn-sweeney
Download Presentation

O bservations of the failed eruption of the magnetic flux rope – a direct application of

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Observations of the failed eruption of the magnetic flux rope – a direct application of the quadrupolar model for a solar flare Tomasz Mrozek AstronomicalInstitute University of Wrocław

  2. 50th anniversary

  3. 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

  4. 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

  5. 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

  6. 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

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

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

  9. 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)

  10. The eruption Initial phase, the eruption moves with small, constant velocity 3 H[km] 2 1 Fast evolution following the strongest HXR peak visible in 25-50 keV range 25-50 keV Deceleration phase. Main front changes its shape. Side eruptions are observed

  11. Interaction with low-lying loops 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. Brightenings observed during the deceleration of the main front.

  12. Interaction with low-lying loops Brightenings in the region marked with the red box were observed exactly during the deceleration of the eruption.

  13. Interaction with low-lying loops inner ribbons outer ribbons The lack of observations made with the 1600 Å filter

  14. 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

  15. 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.

  16. Interaction with high-lying loops the end of the force driving the movement of the high-lying loops Clear relationship between an evolution of the eruption and a height of the high-lying loops

  17. 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.

More Related