Определение оптимальных параметров токовых систем магнитосферы меркурия по данным КА MESSENGER

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Аннотация

Мы используем параболоидную модель магнитосферы Меркурия и данные магнитометра KA MESSENGER, полученные в апреле 2011 г. для определения оптимальных параметров токовых систем магнитосферы Меркурия, в том смысле, что они дают наименьшую невязку (меньше 10 нТл) между предсказаниями модели и измерениями. Полученные модельные данные сравниваются с экспериментальными данными и моделью магнитосферного магнитного поля Меркурия KT17.

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Авторлар туралы

А. Лаврухин

Научно-исследовательский институт ядерной физики им. Д.В. Скобельцына, Московский государственный университет им. М.В. Ломоносова

Хат алмасуға жауапты Автор.
Email: lavrukhin@physics.msu.ru
Ресей, Москва

И. Алексеев

Научно-исследовательский институт ядерной физики им. Д.В. Скобельцына, Московский государственный университет им. М.В. Ломоносова

Email: lavrukhin@physics.msu.ru
Ресей, Москва

Д. Невский

Научно-исследовательский институт ядерной физики им. Д.В. Скобельцына, Московский государственный университет им. М.В. Ломоносова; Московский государственный университет им. М.В. Ломоносова, Физический факультет

Email: lavrukhin@physics.msu.ru
Ресей, Москва; Москва

Әдебиет тізімі

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Жүктеу
2. Fig. 1. Diagram illustrating the main parameters of the paraboloid model of Mercury's magnetosphere in the solar-magnetospheric coordinate system MSM. The paraboloid of revolution with the parabolic coordinate describes the surface of the bow shock, the paraboloid of revolution with the parabolic coordinate describes the surface of the magnetopause with the distance to the subsolar point .

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3. Fig. 2. Distribution for the first five orbits under consideration.

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4. Fig. 3. Calculated parameters of the paraboloid model of Mercury's magnetosphere from the 28th to the 44th orbits of the MESSENGER spacecraft. The abscissa axis shows the orbit number, and the ordinate axis shows the distance to the subsolar point, the distance to the magnetopause tail, the displacement of the tail current sheet relative to the magnetic equatorial plane, the magnitude of the magnetic field modulus at the leading edge of the tail current sheet, the polar cap boundary, and the residual.

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5. Fig. 4. Comparison of the experimentally measured (black), calculated using the paraboloid model (red) and the KT17 model (blue) magnetic field for the 43rd orbit of the MESSENGER spacecraft. Top row – x-component of the magnetic field (left), y-component (right); bottom row – z-component (left), magnetic field modulus (right).

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6. Fig. 5. Comparison of the experimentally measured (black), calculated using the paraboloid model (red) and the KT17 model (blue) magnetic field for the 37th orbit of the MESSENGER spacecraft. Top row – x-component of the magnetic field (left), y-component (right); bottom row – z-component (left), magnetic field modulus (right).

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7. Fig. 6. Comparison of the experimentally measured (black), calculated using the paraboloid model (red) and the KT17 model (blue) magnetic field for the 30th orbit of the MESSENGER spacecraft. Top row – x-component of the magnetic field (left), y-component (right); bottom row – z-component (left), magnetic field modulus (right).

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