Abstract. We present observations of a spectacular eruption of a huge quiescent prominence, which was clearly associated with a coronal mass ejection (CME). The CME consisted of a typical three-part structure: a bright loop-like leading edge, a dark cavity and a bright core. The prominence exhibited a very symmetrical loop-like eruption in low corona and matched well with the bright CME core trailing the CME leading edge. By combining the Hα, 17GHz and EUV observations with white-light coronagraphs observations, the bright CME core was conclusively identified as the erupting cool, dense prominence material.

Abstract. We report the eruption of a small Hα filament and associated partial halo coronal mass ejection (CME) occurring in NOAA AR 9616. Accompanied by a M1.5 flare, the filament quickly erupted, a remote coronal dimming region far away from the eruption site was formed above quiet-sun area, and then a long H α surge developed from the flare site. During the eruption, remote Hα and EUV brightenings appeared near the dimming, along the dimming boundary in EUV and in its interior in Hα, leaving behind EUV loops connecting the eruption source region and the remote EUV brightenings. Finnally, as a definite indication of the CME, a huge dark loop appeared to span the eruption region. These observations indicate that a much larger-scale rearrangement of the corona magnetic fields, eventually represented by the CME, was involved in the eruption of the small filament. Keywords. Sun: activity, coronal mass ejections (CMEs), filaments, flaresOn 2001 September 17, a partial Halo CME was observed by SOHO/LASCO. Using H α data from Yunnan Astronomical Observatory (YNAO), EUV and white-light coronagraph data from SOHO/EIT and SOHO/LASCO, we will show that a filament eruption occurring in NOAA AR 9616 (S14E04) was closely associated with the CME.In H α observations (Figure 1(a1-a4 )), a small filament around the preceding end of AR 9616, 'F', started to erupt violently at about 08:11 UT, followed by an X-ray class M1.5 flare with start, peak and end times at 08:18, 08:25 and 08:34 UT, respectively. Then a long surge appeared near the eruption F after the flare maximum. The flare consisted of three ribbons, 'R', 'Rb' and 'Rc'. The Rb showed spreading motion towards the south, and the Rc was a remote brightening containing a few less bright points. The Rb and Rc were located over quiet-sun regions with opposite magnetic polarities (Figure 1(b)). In EIT 195Å observations (Figure 1(c1-c4 )), a dimming , 'D', and a brightening, 'EB', appeared around the Rc site (see their 195Å light curves in Figure 2(a)). The Rc was inside the D, while the EB, along its northern boundary. Then EUV loops were formed to connect the EB and Rb. Similar to the situation in a halo event reported by Wang, et al. (2002), it seems that the R consisted of two unresolved flare ribbons resulted from the F eruption, while the Rb, EB and EUV loops were the product of the reconnection between the erupting F and outlying coronal loops. The dimming may be due to chromosphere evaporation involved near the footpoint of the remote flare ribbon.A partial halo CME with a width of 166 o was first seen in LASCO C2 images at 08:54 UT. The 195Å difference images reveal that an expanding semicircular dark loop trailed the CME front. Figure 1(d ) shows that its angular extent (see the white arrow) is approximately comparable with that of the CME front. Therefore, we believe that it is the definite indication of the CME start as a result of the F eruption. The CME front heights measured by Seiji Yashiro is shown in Figure 2(b), and the average velocity and acceleration from...