Irkutsk, Russian Federation
Irkutsk, Russian Federation
Irkutsk, Russian Federation
This article presents the review of experimental and theoretical studies on ultra-low-frequency MHD oscillations of the geomagnetic tail. We consider the Kelvin–Helmholtz instability at the magnetopause, oscillations with a discrete spectrum in the “magic frequencies” range, the ballooning instability of coupled Alfvén and slow magnetosonic waves, and “flapping” oscillations of the current sheet of the geomagnetic tail. Over the last decade, observations from THEMIS, CLUSTER and Double Star satellites have been of great importance for experimental studies. The use of several spacecraft allows us to study the structure of MHD oscillations with high spatial resolution. Due to this, we can make a detailed comparison between theoretical results and those obtained from multi-spacecraft studies. To make such comparisons in theoretical studies, in turn, we have to use the numerical models closest to the real magnetosphere.
ULF oscillations, geomagnetic tail, MHD instability, eigenmodes
ВВЕДЕНИЕ
В последние годы с появлением многоспутниковых систем появилась возможность подробного исследования МГД-колебаний, генерируемых и распространяющихся в магнитосфере Земли [Foullon et al., 2008; Agapitov, Cheremnykh, 2013]. Это, в свою очередь, требует более глубокого теоретического изучения таких колебаний. В неоднородной магнитосферной плазме различные ветви МГД-колебаний взаимодействуют между собой, порождая сложную картину волновых полей.
УНЧ-колебания в геомагнитном хвосте имеют свои особенности. Наличие здесь токового и плазменного слоев накладывает свой отпечаток на структуру и спектры альфвеновских волн [Pilipenko, 1990; Rankin et al., 2000; Keiling, 2009]. Во время геомагнитных суббурь происходит разрыв токового слоя, что порождает импульс быстрых магнитозвуковых (БМЗ) волн, который на резонансных магнитных оболочках трансформируется в альфвеновские волны [Allan, Wright, 1998]. Генерируемая в таком процессе альфвеновская волна выглядит как импульс продольных токов и по своим проявлениям не отличается от процесса магнитного пересоединения [Lee, Lysak, 1999; Lysak et al., 2009].
Медленные магнитозвуковые (ММЗ) волны, как и альфвеновские, распространяются почти вдоль силовых линий геомагнитного поля. На тех магнит-ных оболочках, которые пересекают токовый слой геомагнитного хвоста, эти волны могут взаимодействовать между собой [Ohtani et al., 1989]. При наличии кривизны магнитных силовых линий и направленного наружу градиента давления фоновой плазмы такие сцепленные колебания могут становиться неустойчивыми [Liu, 1997; Cheremnykh, Parnowski, 2006; Mazur et al., 2013]. Предполагают, что такая неустойчивость (баллонная) может приводить к пересоединению магнитных силовых линий на начальной стадии геомагнитных суббурь [Cheng, 2004; Saito et al., 2008].
Геомагнитный хвост может служить волноводом для быстрых магнитозвуковых волн [Mann et al., 1999, Мазур и др., 2010]. Собственные моды в таком волноводе могут возбуждаться неустойчивостью сдвигового течения плазмы на магнитопаузе [McKenzie, 1970]. Условия развития неустойчивости Кельвина-Гельмгольца за счет сдвига скорости плазмы в области плазменной мантии достигаются редко. Однако здесь могут возникать неустойчивые колебания, связанные с резонансной неустойчивостью потока плазмы (resonant flow instability, RFI) [Hasegawa et al., 2006]. Эти колебания развиваются в пограничном плазменном слое при достаточно сильных вариациях в нем альфвеновской скорости и скорости звука [Erdelyi, Taroyan, 2003].
БМЗ-волны, проникающие из солнечного ветра в магнитосферу, возбуждают в пограничном слое магнитопаузы резонансные альфвеновские и ММЗ-волны. Из-за высокой диссипативности ММЗ-волн происходит эффективная передача энергии и импульса ионам фоновой плазмы на резонансных оболочках. В результате этого в областях магнитосферы, прилегающих к магнитопаузе, могут сформироваться ячейки с обратной конвекцией плазмы [Leonovich, Kozlov, 2013a]. Отметим также недавно обнаруженные изгибные колебания токового слоя геомагнитного хвоста [Zhang et al., 2002]. Они не похожи на известные типы МГД-колебаний и требуют специального изучения.
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