Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 33959 10.12737/stp-54201902 Results of current research Results of current research Results of current research Manifestations of two branches of solar activity in the heliosphere and GCR intensity Manifestations of two branches of solar activity in the heliosphere and GCR intensity Крайнев Михаил Борисович Krainev Mikhail Borisovich mkrainev46@mail.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Физический институт им. П.Н. Лебедева РАН Москва Россия Lebedev Physical Institute RAS Moscow Russian Federation Шаньдунский институт перспективных технологий Цзинань, Шаньдун Китайская Народная Республика Shandong Institute of Advanced Technology Jinan, Shandong China 5 4 10 20 https://zh-szf.ru/en/nauka/article/33959/view

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.

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.

 galactic cosmic rays heliosphere GCR modulation toroidal and poloidal branches of solar activity galactic cosmic rays heliosphere GCR modulation toroidal and poloidal branches of solar activity

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