Токовые слои электронных масштабов, наблюдаемые миссией MMS в русле высокоскоростных потоков в плазменном слое геомагнитного хвоста

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Resumo

Наблюдения миссии MMS с высоким временным и пространственным разрешением позволили исследовать характеристики интенсивных сверхтонких токовых слоев (СТС) с плотностью тока J > 30 нА/м2, формируемых в русле быстрых плазменных потоков (БПП), распространяющихся в плазменном слое (ПС) геомагнитного хвоста из области магнитного пересоединения. Статистический анализ более 1000 наблюдений СТС в ПС показал, что, в большинстве случаев, ток в СТС является продольным, и основной вклад в его генерацию вносят пучки ускоренных электронов, движущиеся вдоль магнитного поля. Характерная толщина СТС равна нескольким гирорадиусам электронов. В таких слоях электрический ток может переносить популяция размагниченных электронов. На краях и внутри СТС часто наблюдаются всплески сильных неидеальных электрических полей E’ > 10 мВ/м. Генерация таких полей обусловливает плотность мощности энергии, выделяемой в СТС и составляющей несколько сотен пВт/м3, а в некоторых случаях — до нескольких нВт/м3, что сравнимо с мощностью энергии, выделяемой в X-линии. Наиболее сильное энерговыделение наблюдается в СТС, сформированных в русле наиболее высокоскоростных БПП и при сильных вариациях магнитного поля в долях хвоста.

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Sobre autores

Е. Григоренко

Институт космических исследований РАН

Autor responsável pela correspondência
Email: elenagrigorenko2003@yandex.ru
Rússia, Москва

М. Леоненко

Институт космических исследований РАН; Московский физико-технический институт (национальный исследовательский университет)

Email: elenagrigorenko2003@yandex.ru
Rússia, Москва; Долгопрудный

А. Малыхин

Институт космических исследований РАН

Email: elenagrigorenko2003@yandex.ru
Rússia, Москва

Л. Зелёный

Институт космических исследований РАН

Email: elenagrigorenko2003@yandex.ru
Rússia, Москва

Х. Фу

Университет Бейханг; Главная Лаборатория по мониторингу космической среды и обработке информации

Email: elenagrigorenko2003@yandex.ru

Факультет исследований космоса и окружающей среды

República Popular da China, Пекин; Пекин

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2. Fig. 1. Overview of the BPP interval observed by the MMS-1 satellite on 9.VII.2017 at 10:45–10:51 UT. From top to bottom: time profiles of three magnetic field components (a); field modulus in tail lobes (b); X-component of ion flow velocity (c): X-component of ion and electron flow velocity (d); electron temperature (e); current density. Gray circles mark the SCS (f); modulus of the observed electric field, |-Ve × B|, |-Vi × B| (g); parameter J E’ (h). The vertical black line marks the SCS shown in Fig. 2.

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3. Fig. 2. Overview of the STS interval marked in Fig. 1 by the vertical black line. From top to bottom: time profiles of |J| and |Je|, shown in black and gray, respectively (a); VJ of electrons measured on different MMS satellites (shown in corresponding colors) and VJ of ions observed on MMS-1 (shown in gray) (b); LMN — components of the magnetic field in the MMS barycenter (c) and the current density (d); Ne measured on different MMS satellites (shown in corresponding colors) (e); LMN — components of the E’ field measured in the MMS barycenter (f); parameter (g) and (J|| E||) (h) measured on different MMS satellites (shown in corresponding colors); 2D slices of the electron velocity distribution functions (u, k); The spatial profile of the current density JM(lN) and its approximation by the Harris profile are shown in black and gray colors, respectively (l).

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4. Fig. 3. Schematic representation of the dipolarization front with the STS created by the longitudinal beam of accelerated electrons (shown in shades of pink). The gradient fill schematically depicts the change of sign (in the lighter zone . The direction of the current J in the STS is shown by the red arrow. The MMS satellites are shown by dark blue circles with the corresponding numbers. The trajectory of the intersection of the STS by the MMS quartet is shown by the dark blue dotted line. The direction of movement of the accelerated plasma flows from the region of possible secondary reconnection to the STS is shown by light blue arrows. The direction of the fast flow carrying the dipolarization front to the Earth is shown by the black arrow.

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5. Fig. 4. Statistical distributions (option 1) of the characteristics of the STS observed during the intervals of the BBP moving towards the Earth (left column) and away from the Earth (right column).

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6. Fig. 5. Statistical distributions (option 2) of the characteristics of the STS observed in the intervals of the BBP moving towards the Earth (left column) and away from the Earth (right column).

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7. Fig. 6. Statistical distributions (option 3) of the characteristics of the STS observed in the intervals of the BBP moving towards the Earth (left column) and away from the Earth (right column).

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