Heliospheric modulation of cosmic rays: model and observation

Gerasimova, S. K.; Gololobov, P. Yu.; Григорьев, В. Г.; Grigoryev, Vladislav; Krivoshapkin, P. A.; Krymskii, G. F.; Krymsky, G. F.; Starodubtsev, S. A.

doi:10.12737/article_58f970f2455545.93154609

Cited by 2 publications

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“…On the other hand, the GCR modulation theory has predominantly been formulated which includes effects of GCR adiabatic deceleration and convection by the solar wind, their diffusion in irregular HMFs, as well as of particle drift in nonuniform HMF [Krymskiy, 1964;Parker, 1965;Jokipii et al, 1977]. The consideration of the 11-year cycle in sunspot activity as the main cause of the long-term GCR intensity variations in the heliosphere is still used and repeated from article to article (see, e.g., [Potgieter., 2013;Gerasimova et al, 2017]). In this case, the observed insignificant 22-year effects in GCRs are related to the variation with this period of preferred HMF polarity by magnetic drift (A is the sign of the radial HMF component in the northern hemisphere of the heliosphere) [Jokipii et al, 1977].…”

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confidence: 99%

Manifestations of Two Branches of Solar Activity in the Heliosphere and GCR Intensity

Крайнев

2019

Solar-Terrestrial Physics

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This paper provides insight into heliospheric processes and galactic cosmic ray (GCR) modulation occurring due to the presence of two branches of solar activity in this solar layer. According to the topology of solar magnetic fields, these branches are called toroidal (active regions, sunspots, flares, coronal mass ejections, etc.) and poloidal (high-latitude magnetic fields, polar coronal holes, zonal unipolar magnetic regions, etc.). The main cause of different manifestations of the two branches on the solar surface and in the heliosphere — the layer at the base of the heliosphere in which the main energetic factor is the magnetic field — is formulated. In this case, the magnetic fields of the poloidal branch, which have a larger scale but a lower intensity, gain an advantage in penetrating into the heliosphere. A connection is shown between the poloidal branch and the heliospheric characteristics (solar wind velocity field, size of the heliosphere, form of the heliospheric current sheet, regular heliospheric magnetic field and its fluctuations) that, according to modern notions, determine GCR propagation in the heliosphere.

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