Модель потоков высокоэнергичных электронов на орбитах ГЛОНАСС

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Abstract

Моделирование динамики потоков энергичных электронов во внутренней магнитосфере Земли представляет собой актуальную задачу изучения “космической погоды”, учитывая роль, которую энергичные электроны играют в сбоях аппаратуры космических аппаратов. В настоящей работе исследуется возможность построения эмпирической модели потоков электронов на средневысотной круговой орбите спутников ГЛОНАСС. В качестве основной базы данных потоков использованы измерения спутниковой миссии Radiation Belt Storm Probes за 2012–2019 гг. Околоэкваториальные измерения Radiation Belt Storm Probes спроецированы на высоты орбит спутников ГЛОНАСС с использованием эмпирической модели магнитного поля. Главной особенностью представляемой модели потоков энергичных электронов является тот факт, что вместо среднего потока модель восстанавливает функцию распределения вероятностей амплитуд потоков в зависимости от энергии электронов и геомагнитных условий.

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About the authors

П. И. Шустов

Институт космических исследований РАН

Author for correspondence.
Email: p.shustov@gmail.com
Russian Federation, Москва

А. А. Петрукович

Институт космических исследований РАН

Email: p.shustov@gmail.com
Russian Federation, Москва

А. В. Артемьев

Институт космических исследований РАН

Email: p.shustov@gmail.com
Russian Federation, Москва

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Supplementary files

Supplementary Files
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2. Fig. 1. Projections of magnetic field lines of force (red) passing through one revolution of the RBSP satellite orbit trajectory (blue) on three planes. The red dots indicate the intersection of the force lines with the height HG

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3. Fig. 2. Distribution of the fluxes of energetic electrons with energies 33-4096 keV measured at RBSP and the fluxes at the studied altitude of the GLONASS orbit, the colour shows the number of measurements falling within the range of parameters

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4. Fig. 3. Histogram of the number of observations from RBSP data from the value of the geomagnetic index SymH at the corresponding moment of time. The horizontal line corresponds to 1000 observations for which the cut-off is performed

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5. Fig. 4. Examples of histograms of observations of different flux values (left) and the corresponding electron flux probability density for three different energies (right)

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6. Fig. 5. Example of approximation of distribution functions for different values of energy and geomagnetic index. Blue colour - probability density obtained from the flux measurements on the RBSP satellites, red - approximation of the presented probability density function

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7. Fig. 6. Dependences of approximation parameters on energy and geomagnetic index. Parameter R - correlation coefficient of the model (surface) and parameter values at data approximation (blue points)

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8. Fig. 7. SymH geomagnetic index (top) and fluence (bottom) for four time intervals in the energy range 0.5...3.0 MeV. Blue solid lines show the fluence based on RBSP data projected onto GLONASS altitudes; blue dashed lines show the fluence based on the model constructed in this work; red solid lines show the fluence based on open data from the GPS satellite

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