We present the results of a comparative analysis of the properties of a series of successive solar flares, which occurred in active region (AR) 10069 in August 2002, and the associated solar energetic particle (SEP) events (see Figure 1). The active region was extremely flare-productive during its evolution. The solar flare characteristics are based on X-ray and radio emission data: maximum detected photon energies and spectral index, delays between microwave, metric-radio and hard X-ray emissions. The coronal mass ejections (CMEs) are characterized by their projected speed. The SEP properties are described by the relative electron to proton abundance as well as by the abundance of lower relative to higher energy particles. See parameters of SEP events and related flares in Table 1 in Kashapova et al (2019).
Figure 1 Evolution of electron (upper plot) and proton fluxes (lower plot) in the period 17 to 25 August 2005 . Vertical lines show the onset times of the solar flares under consideration.
Figure 2 Scatter plots of the electron RE (marked by asterisks) and proton RP (marked by diamonds) flux ratio vs. CME projected speed (the left plot), vs. GOES flare class (central plot) and vs. X-ray photon spectral index (right plot), respectively.
Figure 3 Scatter plots of the logarithm of the electron-to-proton flux ratio vs. CME projected speed (left), vs. GOES flare class (central plot), and vs. X-ray photon spectral index
(right plot), respectively.
Summarizing the results of analysis we conclude that:
Publications
Larisa Kashapova, Rositsa Miteva, Irina Myagkova, Andrey Bogomolov. Characteristics of SEP Events and Their Solar Origin During the Evolution of Active Region NOAA 10069, (2019) Solar Physics, vol. 294: 9 [DOI:10.1007/s11207-019-1400-3]
