Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 109222 10.12737/stp-114202511 20TH ANNUAL CONFERENCE “PLASMA PHYSICS IN THE SOLAR SYSTEM”. FEBRUARY 10–14, 2025, SPACE RESEARCH INSTITUTE RAS, MOSCOW, RUSSIA 20TH ANNUAL CONFERENCE “PLASMA PHYSICS IN THE SOLAR SYSTEM”. FEBRUARY 10–14, 2025, SPACE RESEARCH INSTITUTE RAS, MOSCOW, RUSSIA 20TH ANNUAL CONFERENCE “PLASMA PHYSICS IN THE SOLAR SYSTEM”. FEBRUARY 10–14, 2025, SPACE RESEARCH INSTITUTE RAS, MOSCOW, RUSSIA MHD-simulation of corotating interaction regions in the heliosphere using different boundary conditions and codes MHD-simulation of corotating interaction regions in the heliosphere using different boundary conditions and codes Павлов Дмитрий Алексеевич Pavlov Dmitry Alexeevich dapavlov@etu.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Крайнев Михаил Борисович Krainev Mikhail Borisovich mkrainev46@mail.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Калинин Михаил Сергеевич Kalinin Mikhail Sergeevich kalininms@lebedev.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Кодуков Александр Владимирович Kodukov Alexander Vladimirovich akodukovich@mail.ru Си Ло Xi Luo xi.luo@iat.cn Фан Шэнь Fang Shen fshen@spaceweather.ac.cn Юйцзи Чжу Yuji Zhu yjzhu@spaceweather.ac.cn Санкт-Петербургский государственный электротехнический университет «ЛЭТИ» Санкт-Петербург Россия St. Petersburg State Electrotechnical University “LETI” St. Petersburg Russian Federation Санкт-Петербургский государственный университет, Санкт-Петербург Россия St. Petersburg State University St. Petersburg Russian Federation 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 Физический институт им. П.Н. Лебедева РАН Москва Россия Lebedev Physical Institute RAS Moscow Russian Federation Санкт-Петербургский государственный электротехнический университет «ЛЭТИ» Санкт-Петербург Россия St. Petersburg State Electrotechnical University “LETI” St. Petersburg Russian Federation Шаньдунский институт передовых технологий Китайская Народная Республика Shandong Institute of Advanced Technology China Государственная ключевая лаборатория космической погоды Национального центра космических наук КАН Пекин Россия State Key Laboratory of Space Weather, National Space Science Center CAS Beijing Russian Federation Шаньдунский институт передовых технологий Цзинань Россия Shandong Institute of Advanced Technology Jinan Russian Federation 10 12 2025 10 12 2025 11 4 104 115 08 06 2025 06 08 2025 https://zh-szf.ru/en/nauka/article/109222/view

The paper presents the results of MHD modeling of corotating interaction regions (CIRs) at distances of 0.1 AU from the Sun (inner boundary) to much larger distances (20–30 AU) in two variants in which the magnetic field on the photosphere (1) is determined from a detailed synoptic map and (2) is represented only by the dipole component. The calculations are made for Carrington rotation 2066 (January–February 2008), using two independent software packages of Russian and Chinese groups. The time period under study is characterized by the presence of long-lived coronal holes on the Sun and a stable recurrent variation in heliosphere characteristics, as well as in the intensity of galactic cosmic rays. We discuss the advantages and disadvantages of modeling CIRs by detailed and dipole models of the photospheric magnetic field, as well as with the two mentioned software packages. The mechanisms of formation and evolution of CIRs with distance in the two models are compared and correlated to the conclusions of our previous works.

The paper presents the results of MHD modeling of corotating interaction regions (CIRs) at distances of 0.1 AU from the Sun (inner boundary) to much larger distances (20–30 AU) in two variants in which the magnetic field on the photosphere (1) is determined from a detailed synoptic map and (2) is represented only by the dipole component. The calculations are made for Carrington rotation 2066 (January–February 2008), using two independent software packages of Russian and Chinese groups. The time period under study is characterized by the presence of long-lived coronal holes on the Sun and a stable recurrent variation in heliosphere characteristics, as well as in the intensity of galactic cosmic rays. We discuss the advantages and disadvantages of modeling CIRs by detailed and dipole models of the photospheric magnetic field, as well as with the two mentioned software packages. The mechanisms of formation and evolution of CIRs with distance in the two models are compared and correlated to the conclusions of our previous works.

 heliosphere corotating interaction regions (CIRs) MHD simulation of CIRs detailed and dipole CIR models heliosphere corotating interaction regions (CIRs) MHD simulation of CIRs detailed and dipole CIR models The work of D.A. Pavlov was carried out at Leonhard Euler International Mathematical Institute in Saint Petersburg with financial support from the Ministry of Science and Higher Education of the Russian Federation (Agreement No. 075-15-2025-343 dated April 29, 2025) The work of D.A. Pavlov was carried out at Leonhard Euler International Mathematical Institute in Saint Petersburg with financial support from the Ministry of Science and Higher Education of the Russian Federation (Agreement No. 075-15-2025-343 dated April 29, 2025)

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