Multi-wavelength study of coronal waves associated with the CME-flare event of 3 November 2003

Abstract

The large flare/CME event that occurred close to the west solar limb on 3 November 2003 launched a large-amplitude large-scale coronal wave that was observed in Hα and Fe xii 195 Å spectral lines, as well as in the soft X-ray and radio wavelength ranges. The wave also excited a complex decimeter-to-hectometer type II radio burst, revealing the formation of coronal shock(s). The back-extrapolation of the motion of coronal wave signatures and the type II burst sources distinctly marks the impulsive phase of the flare (the hard X-ray peak, drifting microwave burst, and the highest type III burst activity), favoring a flare-ignited wave scenario. On the other hand, comparison of the kinematics of the CME expansion with the propagation of the optical wave signatures and type II burst sources shows a severe discrepancy in the CME-driven scenario. However, the CME is quite likely associated with the formation of an upper-coronal shock revealed by the decameter-hectometer type II burst. Finally, some six minutes after the launch of the first coronal wave, another coronal disturbance was launched, exciting an independent (weak) decimeter-meter range type II burst. The back-extrapolation of this radio emission marks the revival of the hard X-ray burst, and since there was no CME counterpart, it was clearly ignited by the new energy release in the flare. Moreton waves and type II bursts are very closely related phenomena (e.g., Harvey et al. 1974;Klassen et al. 2000;Khan & Aurass 2002;Warmuth et al. 2004b), indicating the common nature of the underlying disturbance. The physical background of the relationship was explained by Uchida (1974): the coronal fast-mode MHD shock that propagates along "valleys of low Alfven velocity" excites type II bursts in the corona, whereas the Moreton wave is a "surface track" of the shock front propagation (cf., Uchida 1974, and references therein).Generally, the coronal large-amplitude MHD disturbance could be generated by flares as well as by CMEs, and quite likely, both types of processes happen . The excellent timing association of Moreton waves and type II bursts with the impulsive phase of associated flares (e.g., Harvey 1965;Švestka & Fritzova-Švestkova 1974;Vršnak et al. 1995;Vršnak 2001;Klassen et al. 1999Klassen et al. , 2003) strongly suggests that the waves are ignited by flares. This is also supported by a number of relatively well-defined correlations between various wave characteristics and the flare energy release characteristics (e.g.,Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx

Large-scale Globally Propagating Coronal Waves

“…This correlation could not be established for EIT wave speeds (Klassen et al, 2000), most likely due to the severe undersampling of the waves' kinematics. A kinematical consistency (in terms of distances/heights and speeds) between type II bursts and coronal waves was also found in a large number of case studies (e.g., Vršnak et al, 2006;Pohjolainen et al, 2008;Grechnev et al, 2011b,a;Kozarev et al, 2011;Ma et al, 2011;Kumar and Manoharan, 2013). An example is shown in the right panel of Figure 15.…”

“…Figure 14b illustrates the spatial association of the type II burst source with the Moreton wave in the event reported by Khan and Aurass (2002). In the limb event studied by Vršnak et al (2005Vršnak et al ( , 2006, a complex type II burst was found to propagate obliquely through the corona, but a broad-band radio source was connecting it with the Hα, EIT, and SXR wavefronts in the low corona (cf. Section 3.3.1).…”

“…Metric signatures of a coronal wave were successfully detected by Vršnak et al (2005) for the first time (see Figure 12). They observed a broadband radio source (visible at 151, 164, 237, and 327 MHz) that was moving colaterally with a coronal wave seen in Hα, EUV, and SXRs (see also Vršnak et al, 2006). The source was brighter at lower frequencies, and overall it was significantly weaker than the type II and type IV burst sources also present in the event.…”

“…Most studies have used density models that reflect some average coronal conditions, which may or may not be a good representation of the actual characteristics of an event. More accurate velocities can be derived when the density model is normalized by either direct density measurements and/or radio imaging observations of the type II burst sources (see e.g., Vršnak et al, 2006;Cho et al, 2007;Mancuso, 2007;Magdalenić et al, 2008).…”

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

“…There have been many studies of the possible association of SRBT II with either flares or CMEs [153][154][155][156][157][158][159][160][161][162]. SRBT II has extensively studied to understand their sources and in connection with CMEs and Solar Energetic Particles (SEP) events [50,163] based on signatures of the shock-associated plasma oscillate signatures of type II bursts occurred near off after the maximum of chromosphere flare.…”