Hinode Observations of the Onset Stage of a Solar Filament Eruption

Details Hinode Observations of the Onset Stage of a Solar Filament Eruption Hinode Observations of the Onset Stage of a Solar Filament Eruption

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007pasj...59s.823s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.59, No.SP3, pp.S823--S829

Astronomy and Astrophysics

Astronomy

7

Sun: Filaments, Sun: Flares, Sun: Uv Radiation, Sun: X-Rays, Gamma Rays

Scientific paper

We used Hinode X-Ray Telescope (XRT) and Solar Optical Telescope (SOT) filtergraph (FG) Stokes-V magnetogram observations, to study the early onset of a solar eruption that includes an erupting filament that we observe in TRACE EUV images. The filament undergoes a slow rise for at least 20min prior to its fast eruption and strong soft X-ray (SXR) flaring; such slow rises have been previously reported, and the new Hinode data elucidate the physical processes occurring during this period. XRT images show that during the slow-rise phase, an SXR sigmoid forms from apparent reconnection low in the sheared core field traced by the filament, and there is a low-level intensity peak in both EUV and SXRs during the slow rise. MDI and SOT FG Stokes-V magnetograms show that the pre-eruption filament is along a neutral line between opposing-polarity enhanced network cells, and the SOT magnetograms show that these opposing fields are flowing together and canceling for at least six hours prior to eruption. From the MDI data we measured the canceling network fields to be ˜ 40G, and we estimated that ˜ 1019 Mx of flux canceled during the five hours prior to eruption; this is only ˜ 5% of the total flux spanned by the eruption and flare, but apparently its tether-cutting cancellation was enough to destabilize the sigmoid field holding the filament and resulted in that field's eruption.

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