Solnechno-Zemnaya Fizika Solnechno-Zemnaya Fizika Солнечно-земная физика 2712-9640 50739 10.12737/szf-83202201 Обзоры Reviews Обзоры Numerical analysis of the spatial structure of Alfvén waves in a finite pressure plasma in a dipole magnetosphere Численный анализ пространственной структуры альфвеновских волн в плазме конечного давления в дипольной магнитосфере Петращук Александр Владимирович Petrashchuk Aleksandr Vladimirovich av.petrashchuk@mail.ru https://orcid.org/0000-0002-5450-3397 Магер Павел Николаевич Mager Pavel Nikolaevich p.mager@iszf.irk.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 https://orcid.org/0000-0002-3278-6250 Климушкин Дмитрий Юрьевич Klimushkin Dmitri Yur'evich klimush@iszf.irk.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Институт солнечно-земной физики СО РАН Иркутск Россия Institute of Solar-Terrestrial Physics SB RAS Irkutsk Russian Federation Институт солнечно-земной физики СО РАН Иркутск Россия Institute of Solar Terrestrial Physics SB RAS Irkutsk Russian Federation Институт солнечно-земной физики СО РАН Иркутск Россия Institute of Solar-Terrestrial Physics SB RAS Irkutsk Russian Federation 30 09 2022 30 09 2022 8 3 4 13 28 05 2022 17 08 2022 https://naukaru.ru/en/nauka/article/50739/view

Проведен численный анализ пространственной структуры альфвеновских волн в неоднородной плазме конечного давления в дипольной модели магнитосферы. Были рассмотрены три модели магнитосферы, различающиеся максимальным плазменным давлением и градиентом давления. Была рассмотрена задача на собственные значения частоты волны. Установлено, что частота полоидальной моды может быть либо больше частоты тороидальной моды, либо меньше ее в зависимости от давления плазмы и его градиента. Рассмотрена задача на собственные значения радиальной компоненты волнового вектора. Найдены точки отражения альфвеновской волны в различных моделях магнитосферы. Показано, что область распространения волны в модели с холодной плазмой существенно уже, чем в моделях с конечным давлением плазмы. Исследована структура главной гармоники альфвеновской волны при смене ее поляризации в трех моделях магнитосферы. Проведено численное исследование влияния давления плазмы на структуру поведения всех компонент электрического и магнитного поля альфвеновских волн. Установлено, что при определенных параметрах модели магнитосферы магнитное поле может иметь три узла в то время как в модели с холодной плазмой только один. Кроме того, продольная компонента магнитного поля дважды меняет знак вдоль силовой линии магнитного поля.

We have carried out a numerical analysis of the spatial structure of Alfvén waves in a finite pressure inhomogeneous plasma in a dipole model of the magnetosphere. We have considered three magnetosphere models differing in maximum plasma pressure and pressure gradient. The problem of wave eigenfrequencies was addressed. We have established that the poloidal frequency can be either greater or less than the toroidal frequency, depending on plasma pressure and its gradient. The problem of radial wave vector component eigenvalues was considered. We have found points of Alfvén wave reflection in various magnetosphere models. The wave propagation region in the cold plasma model is shown to be significantly narrower than that in models with finite plasma pressure. We have investigated the structure of the main Alfvén wave harmonic when its polarization changes in three magnetosphere models. A numerical study into the effect of plasma pressure on the structure of behavior of all Alfvén wave electric and magnetic field components has been carried out. We have established that for certain parameters of the magnetosphere model the magnetic field can have three nodes, whereas in the cold plasma model there is only one. Moreover, the longitudinal magnetic field component changes sign twice along the magnetic field line.

 МГД-волны дипольная модель магнитосферы МГД-резонансы MHD waves dipole model of the magnetosphere MHD resonances Работа выполнена при финансовой поддержке Минобрнауки России The work was financially supported by the Ministry of Science and Higher Education of the Russian Federation

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