Динамика электронного радиационного пояса во время магнитных возмущений и в спокойное время

Динамика электронного радиационного пояса во время магнитных возмущений и в спокойное время

Автор: Лазутин Л.Л., Дмитриев А.В., Суворова А.В.

Журнал: Солнечно-земная физика @solnechno-zemnaya-fizika

Статья в выпуске: 1 т.4, 2018 года.

Бесплатный доступ

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...

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Магнитосфера, электроны, радиационный пояс, пополнения и потери

Короткий адрес: https://sciup.org/142220276

IDR: 142220276   |   DOI: 10.12737/szf-41201805

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