Solnechno-Zemnaya Fizika Solnechno-Zemnaya Fizika Солнечно-земная физика 2712-9640 18108 10.12737/szf-41201805 Обзоры Reviews Обзоры Electron radiation belt dynamics during magnetic storms and in quiet time Динамика электронного радиационного пояса во время магнитных возмущений и в спокойное время Лазутин Леонид Леонидович Lazutin Leonid Leonidovich lll@srd.sinp.msu.ru

доктор физико-математических наук;

doctor of physical and mathematical sciences;

 Дмитриев Алексей Владимирович Dmitriev Alexei Vladimirovich dalex@jupiter.ss.ncu.edu.tw Суворова Алла Васильевна Suvorova Alla Vasil'evna all@yahoo.com

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Научно-исследовательский нститут ядерной физики им. Д.В. Скобельцина МГУ Москва Россия Skobeltsyn Institute of Nuclear Physics MSU Moscow Russian Federation Научно-исследовательский институт ядерной физики им. Д.В. Скобельцина МГУ, Москва , Россия Москва Россия Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow , Russian Federation Moscow Russian Federation Факультет космических наук и инженерии, Национальный Центральный Университет, Тайвань Тайвань Китайская Республика Department of Space Science and Engineering, National Central University, Taiwan Taiwan Taiwan Научно-исследовательский нститут ядерной физики им. Д.В. Скобельцина МГУ Москва Россия Skobeltsyn Institute of Nuclear Physics, Moscow State University Moscow Russian Federation 4 1 59 71 https://naukaru.ru/en/nauka/article/18108/view

В работе рассмотрена динамика внешнего электронного радиационного пояса, адиабатические и неадиабатические механизмы пополнения и потерь энергичных электронов. В свободное от магнитных возмущений время внешний электронный пояс постепенно опустошается: на внутренних оболочках вследствие сброса электронов в атмосферу, а в зоне квазизахвата, поскольку дрейфовые оболочки электронов там не замкнуты, вследствие потерь на магнитопаузе. Последний процесс маскируется пополнением свежеускоренными частицами и мало заметен в обычные годы, но в годы экстремально низкой солнечной активности приводит к существенному понижению численности электронной популяции радиационного пояса. На главной фазе магнитной бури основной причиной понижения интенсивности потока электронов является адиабатическое охлаждение, связанное с сохранением адиабатических инвариантов, дополненное сбросом электронов в атмосферу и гибелью их на магнитопаузе. Возрастания потока электронов обусловливаются суммарным действием четырех процессов: Е×В-заб-роса электронов глубоко к Земле импульсным индукционным электрическим полем суббуревой активизации, а также крупномасштабным электрическим полем солнечного ветра, в обоих случаях перенос частиц в область более сильного магнитного поля при сохранении магнитного момента приводит к росту их энергии. Тот же механизм ускорения работает при переносе электронов из-за радиальной диффузии, которая сопровождает питч-угловую диффузию. Четвертый процесс связан с адиабатическим подогревом частиц на фазе восстановления. Степень восстановления потока электронов после бури определяется соотношением неадиабатических возрастаний и потерь, в результате значения потока составляют непрерывный ряд от низкого до сильно повышенного. Сочетание этих процессов определяет индивидуальный характер развития радиационного пояса во время каждой магнитной бури и поведение пояса в спокойные периоды.

The paper discusses the dynamics of the outer electron belt, adiabatic and nonadiabatic mechanisms of replenishment and losses of energetic electrons. Under undisturbed conditions, the outer electron belt gradually empties: in the inner magnetosphere due to electron precipitation in the atmosphere and in the quasi-trapping region due to losses at the magnetopause because drift shells of electrons are not closed there. The latter process does not occur in normal years due to the masking replenishment by freshly accelerated particles, but in years of extremely low activity it leads to a significant decrease in the electron population of the belt. During the magnetic storm main phase, the first reason for the decrease in the electron flux intensity is the adiabatic cooling associated with conservation of adiabatic invariants and complemented by precipitation of electrons into the atmosphere and their dropout at the magnetopause. Electron flux increases involve EB electron injection by the induction electric field of substorm activation and by the large-scale solar wind electric field, with pitch energy diffusion along with adiabatic heating in the recovery phase. The rate of electron flux recovery after a storm is determined by the ratio of nonadiabatic increases and losses; hence the electron flux represents a continuous series from low to very high values. The combination of these processes determines the individual character of radiation belt development during each magnetic storm and the behavior of the belt in the quiet time.

 магнитосфера электроны радиационный пояс пополнения и потери magnetosphere electrons radiation belt replenishment and losses.

ВВЕДЕНИЕВ существующих обзорах по радиационным поясам (РП) [Parks, Winkler 1968; Vernov et al., 1969; Friedel et al., 2002; Millan, Thorne, 2007; Shprits et al., 2008а] достаточно подробно описывается как структура РП, так и его формирование. Согласно принятой теории [Тверской, 1964, 1965], формирование РП объясняется сочетанием медленной радиальной диффузии электронов под действием небольших по величине импульсов магнитного поля с потерями в атмосфере из-за питч-угловой диффузии. В принципе, это объясняет наблюдаемую пространственную структуру захваченных электронов с провалом между внутренним и внешним РП.Во время магнитных бурь этот стройный порядок нарушается, происходят динамические вариации, понижения и повышения потоков энергичных электронов. Потоки энергичных электронов-«киллеров» привлекают повышенное внимание исследователей, появляются работы, посвященные предсказанию их средних или пиковых значений [Li et al., 2001; Simms et al., 2016] (см. также обзор [Потапов, 2017]).Большое число работ посвящено анализу динамики РП во время магнитных бурь [Baker et al., 1997; Li et al., 1997; Reeves et al., 1998; Yu et al., 2015; Hwang et al., 2015; Turner et al., 2017], среди них существенную часть составляют работы, выполненные в НИИЯФ МГУ [Вернов и др., 1965; Кузнецов и др., 1966; Бахарева, 2003; Иванова и др., 2000; Калегаев и др., 2015; Antonova, 2005; Lazutin, 2012; Kalegaev, Vlasova, 2014; Dmitriev et al., 2010, 2014; Slivka et al., 2006; Tverskaya et al., 2005; Vernov et al., 1969]. В связи с этим нам представляется целесообразным сделать обзор современных представлений о динамике РП. Заметим, что обзор создавался в значительной мере на основе работ, выполненных в НИИЯФ МГУ.В обзоре мы сначала опишем динамику РП во время магнитных бурь, затем остановимся на механизмах пополнения и потерь энергичных электронов и в завершение рассмотрим поведение РП в спокойное время. Мы ориентируемся на читателя, знакомого с базовыми понятиями: с характером движения частиц и адиабатическими инвариантами, динамикой полей и токов во время магнитных бурь и т. п.

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