Low Atmosphere Reconnections Associated with an Eruptive Solar Flare

Details Low Atmosphere Reconnections Associated with an Eruptive Solar Flare Low Atmosphere Reconnections Associated with an Eruptive Solar Flare

Mar 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jkas...37...41m&link_type=abstract

Journal of the Korean Astronomical Society, Vol. 37, no. 1, pp. 41-53

Astronomy and Astrophysics

Astronomy

15

Sun: Magnetic Fields, Sun: Flare, Sun: Coronal Mass Ejection, Sun: Filament

Scientific paper

It has been a big mystery what drives filament eruptions and flares. We have studied in detail an X1.8 flare and its associated filament eruption that occurred in NOAA Active Region 9236 on November 24, 2000. For this work we have analyzed high temporal (about 1 minute) and spatial (about 1 arcsec) resolution images taken by Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory, Hα centerline and blue wing (-0.6Å) images from Big Bear Solar Observatory, and 1600 Å UV images by the Transition Region and Corona Explorer (TRACE). We have found that there were several transient brightenings seen in Hα and, more noticeably in TRACE 1600 Å images around the preflare phase. A closer look at the UV brightenings in 1600 Å images reveals that they took place near one end of the erupting filament, and are a kind of jets supplying mass into the transient loops seen in 1600 Å. These brightenings were also associated with canceling magnetic features (CMFs) as seen in the MDI magnetograms. The flux variations of these CMFs suggest that the flux cancellation may have been driven by the emergence of the new flux. For this event, we have estimated the ejection speeds of the filament ranging from 10 to 160 km s-1 for the first twenty minutes. It is noted that the initiation of the filament eruption (as defined by the rise speed less than 20 km s-1) coincided with the preflare activity characterized by UV brightenings and CMFs. The speed of the associated LASCO CME can be well extrapolated from the observed filament speed and its direction is consistent with those of the disturbed UV loops associated with the preflare activity. Supposing the Hα/UV transient brightenings and the canceling magnetic features are due to magnetic reconnection in the low atmosphere, our results may be strong observational evidence supporting that the initiation of the filament eruption and the preflare phase of the associated flare may be physically related to low-atmosphere magnetic reconnection.

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