Смена состава плазмы на повороте магнитопаузы Марса

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Abstract

Высокое временное разрешение измерений магнитного поля и плазмы Марса обеспечиваются наблюдениями на спутнике Mars Atmosphere and Volatile Evolution (MAVEN; Jakosky и др., 2015), позволяют анализировать тонкие слои плазменной оболочки Марса. В этой статье описана магнитная структура, связанная с дневной марсианской магнитопаузой. Было показано, что прошедший через ударную волну солнечный ветер на дневной стороне Марса напрямую не взаимодействует с ионосферой Марса. Слой плазмы и магнитного поля толщиной 200–300 км образует дневную магнитосферу, которая является областью между магнитослоем и ионосферой (Вайсберг, Шувалов, 2020). Дневная магнитосфера бывает двух типов: 1) магнитосфера более распространенного типа состоит из нагретых и ускоренных ионов O+ и O2+, находящихся между ионосферой и обтекающим горячим потоком Марса; 2) другой тип дневной магнитосферы состоит из ускоренных ионов O+ и O2+ в магнитослое, где они образуют продолжающийся ускоренный пучок, формирующий плюм. Между магнитослоем и магнитосферой находится магнитная структура, которая вращается, почти не меняя своей величины. Эта структура расположена во второй части перехода np/(np + nh) от величины ~1 до ~10–2. Переход между магнитослоем и магнитосферой происходит плавно, как по плотности энергии, так и по составу ионов при уменьшении потока протонов и увеличении потока тяжелых ионов.

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About the authors

О. Л. Вайсберг

Институт космических исследований РАН

Author for correspondence.
Email: olegv@iki.rssu.ru
Russian Federation, Москва

А. Ю. Шестаков

Институт космических исследований РАН

Email: olegv@iki.rssu.ru
Russian Federation, Москва

Р. Н. Журавлев

Институт космических исследований РАН

Email: olegv@iki.rssu.ru
Russian Federation, Москва

Д. Н. Морозова

Институт космических исследований РАН

Email: dashia110999@mail.ru
Russian Federation, Москва

А. Рамазан

Московский физико-технический институт

Email: olegv@iki.rssu.ru
Russian Federation, Москва

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Supplementary files

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2. Fig. 1. The MAVEN instruments used to study Mars in this paper include the ion and electron spectrometers and the magnetometer. MAVEN data include the magnetosheath, magnetopause, magnetosphere, and ionosphere on August 17, 2019, at ~23:32–23:45 EDT. Panels, from top to bottom: 1 – All ion flux; 2 – Proton flux H+; 3 – Oxygen flux O+; 4 – Oxygen flux O2+; 5 – Electron flux; 6 – Colored lines of ion density (key in right box) and relative ion and proton density (green lines); 7 – Velocities of the three ions (key in right box); 8 – Magnetic field components in the Mars-oriented Solar Orbit (MSO) coordinate system (keys on the right) and magnetic field magnitude (black line).

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3. Fig. 2. Result of the minimum analysis of the magnetic field: (a) – the region of rotation of the magnetic field, vertical lines highlight the interval of the rotating magnetic field. (b) – components of the eigenvalues ​​of the minimum analysis L and N, where L and N are different projections in the coordinate system of the magnetic field (B1, B2, B3).

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4. Fig. 3. The Mercator chart shows three intervals: slow movement in the region of point “a”, rapid rotation between points “a” and “b”, and slow movement at point “b”. The total angle is slightly more than 60°.

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5. Fig. 4. The upper section shows a decrease in the differential flux of H+, i.e. solar wind protons, and the differential flux of O+ ion energy shows an increase in the ion energy flux in the same sector. The interval ranges from ~23:36:0 UT to 23:36:44 UT.

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6. Fig. 5. August 4, 2019, 05:20:47 – 05:24:22 EDT. MAVEN data include the magnetosheath, magnetopause, magnetosphere, and ionosphere. Panels from top to bottom: 1 – sum of all ions differential energy-time; 2 – proton differential energy-time H+; 3 – oxygen differential energy-time O+; 4 – oxygen energy-time O2+; 5 – electron differential energy-time; 6 – colored lines for ion density (in the box on the right) and the relative density of ions and protons (green lines); 7 – velocities of the three ions (key in the box on the right); 8 – magnetic floor components in the Mars Solar Orbit (MSO) coordinate system (color legend on the right), and magnetic field magnitude (black line). The red color stripe at the bottom shows that the satellite is in the northern hemisphere. The vertical black stripes show approximately the magnetopause region. The sector between the two vertical lines indicates the location where the magnetic field rotates.

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7. Fig. 6. Result of the minimum analysis of the magnetic field: (a) – diagrams of the components of the magnetic field and the type of rotation of the components of the magnetic field; (b) – components of the eigenvalues ​​of the minimum analysis L and N with minimum dispersion.

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8. Fig. 7. Part of the Mercator map shows time intervals from approximately August 17, 2019, from 05:22:40 UT to 05:23:20 UT. Green dots show the trajectory of the rapid magnetic turn.

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9. Fig. 8. Distribution of n+ and O+ densities in the time interval from 05:22:24 – 05:22:04 UT within the magnetopause sector.

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10. Fig. 9. July 30, 2019, 01:10:26 – 01:20:30 EDT. MAVEN data include the magnetosheath, magnetopause, magnetosphere, and ionosphere. Panels from top to bottom: 1 – sum of all ions differential energy-time; 2 – proton differential energy-time H+; 3 – oxygen differential energy-time O+; 4 – oxygen energy-time O2+; 5 – electron differential energy-time; 6 – colored lines of ion density (keys in right box) and relative ion and proton density (green lines); 7 – velocities of the three ions (keys in right box); 8 – magnetic floor components in Mars Solar Orbit (MSO) coordinate system (color key is given on the right) and magnetic field magnitude (black line). The red color stripe at the bottom shows that the satellite is in the northern hemisphere. The two vertical black stripes show approximately the magnetopause region. The sector between the two vertical lines indicates the location where the magnetic field rotates.

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11. Fig. 10. Result of the minimum magnetic field analysis: (a) – diagram of the magnetic field of minimum dispersion; (b) – two-dimensional view of the rotation of the magnetic field, where L is a fairly long and almost straight section of the diagram, and N is the most curved section of the diagram.

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12. Fig. 11. Part of the Mercator map shows time intervals from about July 30, 2019 at ~01h23m UT. Green dots show the trajectory of the rapid magnetic turn.

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13. Fig. 12. O+ separating the surrounding flow from the magnetosphere 01:22:24–01:23:24 UT.

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