Observations of the failed eruption of a filament

摘要: We have observed the fine temporal and spatial structure of a filament eruption on 2002 May 27 following an M2-class flare. Our observations at Big Bear Solar Observatory were made wavelength Halpha 1.3 Angstrom, with cadence 40 ms. The event was also by Reuven Ramaty High Energy Spectroscopic Imager (RHESSI) X-ray energies from 3 to 50 keV Transition Region Coronal Explorer (TRACE) in poFe XII 195 Angstrom. appears be "failed eruption," as material, seen absorption TRACE, first accelerated then decelerated it approached its peak height similar to8 x 10(4) km while threads drained back Sun. fact that did not lead coronal mass ejection indicates magnetic field near open during height-time curve obtained TRACE Angstrom images deceleration phase shows exceeded gravitational more than factor 10, which suggests material pulled tension. Also importance are three sequential but cospatial features-brightenings EUV, loop-top hard emission, "rupturing" filament-that point release energy (and probably reconnection) above initial filament's location well below terminal height. Reconnection does appear most models, notable exception quadrupolar "breakout" models. These provide evidence least two conditions required for successful eruption: reconnection very low corona (possibly filament) or opening fields point.