Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 28040 10.12737/stp-51201904 Results of current research Results of current research Results of current research Recurrent and sporadic Forbush decreases during solar cycles 23–24 Recurrent and sporadic Forbush decreases during solar cycles 23–24 Мелкумян Анаид Ашотовна Melkumyan Anaid Ashotovna amelkumyan6@gamail.com Белов Анатолий Владимирович Belov Anatoliy Vladimirovich abelov@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Абунина Мария Александровна Abunina Mariya Aleksandrovna abunina@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Абунин Артем Анатольевич Abunin Artem Anatol'evich abunin@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Ерошенко Евгения Александровна Eroshenko Evgeniya Aleksandrovna erosh@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Оленева Виктория Александровна Oleneva Viktoria Aleksandrovna olene@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Янке Виктор Гугович Yanke Viktor Gugovich yanke@izmiran.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Российский государственный университет нефти и газа (национальный исследовательский университет) имени И.М. Губкина Москва Россия Gubkin Russian State University of Oil and Gas (National Research University) Moscow Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк, Москва Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation, RAS Troitsk, Moscow Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS Troitsk Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS Troitsk Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк, Москва Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation, RAS Troitsk, Moscow Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк, Москва Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation, RAS Troitsk, Moscow Russian Federation Институт земного магнетизма, ионосферы и распространения радиоволн им. Н.В. Пушкова РАН Троицк, Москва Россия Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation, RAS Troitsk, Moscow Russian Federation 5 1 28 34 https://zh-szf.ru/en/nauka/article/28040/view

A comparison has been made between recurrent (associated with high-speed streams from coronal holes) and sporadic (caused by interplanetary coronal mass ejections (ICMEs)) Forbush decreases (FDs) in solar cycles 23 and 24 (as well as in the maxima of these cycles and the minimum between them). Forbush Effects and Interplanetary Disturbances database created and maintained in IZMIRAN provided a large number of events (about 1700 isolated FDs, among them 350 recurrent FDs, and 207 sporadic FDs selected with high reliability), which allowed us to apply statistical methods. The results revealed that sporadic FDs prevailed in the maxima of the cycles; recurrent FDs, in the minimum between the cycles. FD parameters (magnitude, decrease rate, anisotropy) are larger for sporadic events than for recurrent ones, especially in the maxima of the cycles. FD magnitude is greater in the maxima than in the minimum for sporadic events, and it changes weakly for recurrent ones. The solar wind velocity is on average greater for recurrent events than for sporadic ones; it is larger for recurrent FDs in the minimum and for sporadic FDs in the maxima. The magnetic field is stronger for sporadic FDs than for recurrent ones in the maxima and it is approximately equal for both types of events in the minimum. The magnetic field of ICMEs is weaker in the current solar cycle than in the previous one. The duration of the FD main phase is less in the maxima for both types of events; sporadic FDs developed significantly faster than recurrent ones in the maximum of cycle 23.

A comparison has been made between recurrent (associated with high-speed streams from coronal holes) and sporadic (caused by interplanetary coronal mass ejections (ICMEs)) Forbush decreases (FDs) in solar cycles 23 and 24 (as well as in the maxima of these cycles and the minimum between them). Forbush Effects and Interplanetary Disturbances database created and maintained in IZMIRAN provided a large number of events (about 1700 isolated FDs, among them 350 recurrent FDs, and 207 sporadic FDs selected with high reliability), which allowed us to apply statistical methods. The results revealed that sporadic FDs prevailed in the maxima of the cycles; recurrent FDs, in the minimum between the cycles. FD parameters (magnitude, decrease rate, anisotropy) are larger for sporadic events than for recurrent ones, especially in the maxima of the cycles. FD magnitude is greater in the maxima than in the minimum for sporadic events, and it changes weakly for recurrent ones. The solar wind velocity is on average greater for recurrent events than for sporadic ones; it is larger for recurrent FDs in the minimum and for sporadic FDs in the maxima. The magnetic field is stronger for sporadic FDs than for recurrent ones in the maxima and it is approximately equal for both types of events in the minimum. The magnetic field of ICMEs is weaker in the current solar cycle than in the previous one. The duration of the FD main phase is less in the maxima for both types of events; sporadic FDs developed significantly faster than recurrent ones in the maximum of cycle 23.

 Forbush decrease solar wind interplanetary magnetic field coronal mass ejections coronal holes solar cycle statistical analysis Forbush decrease solar wind interplanetary magnetic field coronal mass ejections coronal holes solar cycle statistical analysis

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