Slow-Rise and Fast-Rise Phases of an Erupting Solar Filament, and Flare Emission Onset

Details Slow-Rise and Fast-Rise Phases of an Erupting Solar Filament, and Flare Emission Onset Slow-Rise and Fast-Rise Phases of an Erupting Solar Filament, and Flare Emission Onset

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...630.1148s&link_type=abstract

The Astrophysical Journal, Volume 630, Issue 2, pp. 1148-1159.

Astronomy and Astrophysics

Astronomy

47

Sun: Coronal Mass Ejections (Cmes), Sun: Filaments, Sun: Flares, Sun: Uv Radiation, Sun: X-Rays, Gamma Rays

Scientific paper

We observe the eruption of an active-region solar filament on 1998 July 11 using high time cadence and high spatial resolution EUV observations from the TRACE satellite, along with soft X-ray images from the soft X-ray telescope (SXT) on the Yohkoh satellite, hard X-ray fluxes from the BATSE instrument on the CGRO satellite and from the hard X-ray telescope (HXT) on Yohkoh, and ground-based magnetograms. We concentrate on the initiation of the eruption in an effort to understand the eruption mechanism. Prior to eruption the filament undergoes a slow upward movement in a slow-rise phase with an approximately constant velocity of ~15 km s-1 that lasts about 10 minutes. It then erupts in a fast-rise phase, accelerating to a velocity of ~200 km s-1 in about 5 minutes and then decelerating to ~150 km s-1 over the next 5 minutes. EUV brightenings begin about concurrently with the start of the filament's slow rise and remain immediately beneath the rising filament during the slow rise; initial soft X-ray brightenings occur at about the same time and location. Strong hard X-ray emission begins after the onset of the fast rise and does not peak until the filament has traveled to a substantial altitude (to a height about equal to the initial length of the erupting filament) beyond its initial location. Our observations are consistent with the slow-rise phase of the eruption resulting from the onset of ``tether cutting'' reconnection between magnetic fields beneath the filament, and the fast rise resulting from an explosive increase in the reconnection rate or by catastrophic destabilization of the overlying filament-carrying fields. About 2 days prior to the event, new flux emerged near the location of the initial brightenings, and this recently emerged flux could have been a catalyst for initiating the tether-cutting reconnection. With the exception of the sudden transition from the slow-rise phase to the fast-rise phase in our event, our filament's height-time profile is qualitatively similar to the plot of the erupting flux rope height as a function of time recently computed by Chen and Shibata for a model in which the eruption is triggered by reconnection between an emerging field and another field under the flux rope.

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