Solnechno-Zemnaya Fizika Solnechno-Zemnaya Fizika Солнечно-земная физика 2712-9640 28709 10.12737/szf-54201902 Результаты исследований Results of current research Результаты исследований Manifestations of two branches of solar activity in the heliosphere and GCR intensity Проявления в гелиосфере и в интенсивности ГКЛ двух ветвей солнечной активности 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 12 25 https://naukaru.ru/en/nauka/article/28709/view

Дается представление о процессах в гелиосфере и модуляции галактических космических лучей (ГКЛ) в ней как результатах действия в этом слое Солнца двух ветвей солнечной активности, называемых по топологии солнечных магнитных полей внутри Солнца тороидальной ветвью (активные области, пятна, вспышки, корональные выбросы массы и т. д.) и полоидальной ветвью (высокоширотные магнитные поля, полярные корональные дыры, зональные униполярные магнитные области и т. д.). Формулируется основная причина различного проявления обеих ветвей на поверхности Солнца и в гелиосфере — наличие в основании гелиосферы слоя, в котором основным энергетическим фактором является магнитное поле. При этом преимущество при проникновении в гелиосферу получают более крупномасштабные, хотя и менее интенсивные солнечные магнитные поля полоидальной ветви. Показана связь с полоидальной ветвью солнечной активности гелиосферных характеристик (поле скорости солнечного ветра, размер гелиосферы, форма гелиосферного токового слоя, регулярное гелиосферное магнитное поле и его флуктуации), которые, согласно современным представлениям, определяют распространение в гелиосфере ГКЛ.

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.

 галактические космические лучи гелиосфера модуляция ГКЛ тороидальная и полоидальная ветви солнечной активности galactic cosmic rays heliosphere GCR modulation toroidal and poloidal branches of solar activity

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