• General data

       *GOES soft X-rays       *some images      GOES protons

*SOHO/LASCO/C2 (running difference)

SOHO/LASCO/C3 (running difference)
 

Multicomponent, 3-harmonic type II  radio burst

 
*Semi-compressed dynamic spectrum (09:50 - 12:30 UT)

Fixed-frequency plots (169, 204, and 3000 MHz)

*Type II bands (10:16 - 10:34 UT)

*Three harmonics
 

*IZMIRAN spectrum and NRH

Origin of a coronal type II shock wave(s)

*Lifting of soft X-ray loops (~10:14 UT)

*Yohkoh/SXT swing mode (between 10:12:50 and 10:14:50 UT)

 
Above the top of rapidly expanding and disrupting soft X-ray structures
           (see Klassen, Aurass, Klein et al., 1999; Klein, Khan, Vilmer et al. 1999)

 
• Pulsating radio continuum and type III-like bursts

 
*Semi-compressed dynamic spectrum (09:50 - 12:30 UT)

 *Pulsation phase

* Drifting type III-like features
 

Pulsations with a time scale of tens of seconds consisting of second-scale type III-like features.

Quasi-periodic electron ejections modulated by MHD oscilations of  large-scale post-CME magnetic tubes (see, e.g., Zaitsev, Stepanov, 1975; Aschwanden, 1987, Aurass, Mann, 1987).

 

 
• Large-scale CME-associated activity:

              re-formation of the coronal magnetic structures

SOHO/EIT,  195 A (original)
 
*SOHO/EIT 195 A (modified)
 
SOHO/EIT 195 A (difference to 10:00 UT)
 
     SOHO/EIT 195 A: difference images to 10:00 UT
 
*SOHO/EIT 195 A (running difference)
 
         * SOHO/EIT 195 A: running difference images
 
        * EUV dimming and CME

Extended EUV dimming area on the disk and over the limb maps out the apparent location and configuration of the white-light CME (see Thompson et al., 2000).
 

*Yohkoh soft X-ray arcade before and after the event (H. Hudson)