I.M. Chertok (1), A.V. Belov (1), V.V. Grechnev (2)

(1) Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Troitsk, Moscow, Russia
(2)  Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia

Abstract. 

Figure 1. The STEREO/EUVI 195 °A B-streaks typical of C-, M-, and X-class flares.

 

Table 1: A list of flares registered both with GOES and STEREO/EUVI 

 

Figure 2. Scatter plot of the relative lengths of the STEREO/EUVI B-streaks versus the
GOES 1–8 °A fluxes. 

 

Figure 3. Impulsive GOES M-class flares and their thin, single, long B-streaks.

 

Figure 4. Long-duration GOES X-class flares and their thick, two or multi-element,
relatively short B-streaks. 

Figure 5. The distribution of the time difference between the observations of the longest
STEREO/EUVI B-streak and the peak of the SXR flux measured by GOES. 

Figure 6. Full-Sun STEREO/EUVI 195 °A images of six strongest far-side flares detected
from B-streaks (see Table 2). 

Table 2. A list of major far-side flares detected from B-streaks in STEREO/EUVI 195 °A images. 

Figure 7. Probable time history of the 1–8 °A flux of two famous far-side flares estimated
from STEREO/EUVI B-streaks. 

 PDF file  of the paper

Solar Phys. Volume 290, Issue 7, pp. 1947-1961, 2015. DOI:  10.1007/s11207-015-0738-4.