Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 41325 10.12737/stp-64202006 Results of current research Results of current research Results of current research Increases in SCR energetic proton fluxes on Earth and their relation to solar sources Increases in SCR energetic proton fluxes on Earth and their relation to solar sources Лазутин Леонид Леонидович Lazutin Leonid Leonidovich lll@srd.sinp.msu.ru

доктор физико-математических наук;

doctor of physical and mathematical sciences;

 Научно-исследовательский нститут ядерной физики им. Д.В. Скобельцина МГУ Москва Россия Skobeltsyn Institute of Nuclear Physics MSU Moscow Russian Federation 6 4 40 43 https://naukaru.ru/en/nauka/article/41325/view

Logachev catalog data for solar cycle 23 has been used to study the dependence of measured increases in solar cosmic rays (SCRs) on solar perturbations. The efficiency of recording the SCR increases, driven by proton acceleration in the corona, on Earth and in its vicinity is shown to depend on power of a solar flare that created a shock wave and on position of the flare on the solar disk. As the particle flux moves along the heliolongitude away from the parent flare, the acceleration efficiency decreases, i.e. the maximum energy of the accelerated particles and their intensity at equal energy decrease. As a result, at a certain distance along a heliolongitude from the parent solar flare, the solar proton flux intensity decreases to the galactic background, and there is no SCR increase detected.

Logachev catalog data for solar cycle 23 has been used to study the dependence of measured increases in solar cosmic rays (SCRs) on solar perturbations. The efficiency of recording the SCR increases, driven by proton acceleration in the corona, on Earth and in its vicinity is shown to depend on power of a solar flare that created a shock wave and on position of the flare on the solar disk. As the particle flux moves along the heliolongitude away from the parent flare, the acceleration efficiency decreases, i.e. the maximum energy of the accelerated particles and their intensity at equal energy decrease. As a result, at a certain distance along a heliolongitude from the parent solar flare, the solar proton flux intensity decreases to the galactic background, and there is no SCR increase detected.

 solar cosmic rays solar flare intensity heliolongitude solar cosmic rays solar flare intensity heliolongitude

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