The Relation between Maximum Fluxes of Solar Protons and Electrons: Acceleration and/or Propagation?

This work is the first step in creating our own catalog of proton events from 1997 to the present based on SOHO/EPHIN data. A method has been developed for automatically identifying significant increases in the solar proton flux against the dynamically changing background of galactic cosmic rays (GCRs)—conglomerates of proton increases. The GCR background in the 25–53 MeV EPHIN channel has been calculated from 1996 to the present, and 486 conglomerates of proton enhancements have been found. Two methods for automatic search for individual proton enhancements within a conglomerate have been developed. A conglomerate formed in May–June 2024 is considered, in which 12 proton enhancements have been identified based on SOHO/EPHIN and ART-XC radiation environment monitor data. Only two of them did not have an obvious solar source (a “proton” flare or a CME with a velocity of >900 km/s). A scatter diagram of the electron and proton flux maxima in 486 conglomerates has been constructed, in which two areas of maxima location are highlighted: 1) there is no obvious proportionality between the maximum fluxes, and 2) such proportionality exists in a fairly wide range of values. The position of the 12 proton increases in May–June 2024 on the diagram shows that the observed e/p ratio is formed by both acceleration and propagation processes. The relative number of electrons increases with unfavorable locations of particle acceleration and entry into the IMF.