Heliospheric current sheet and effects of its interaction with solar cosmic rays
- Autores: Malova H.1,2, Popov V.2,3,4, Grigorenko E.2, Dunko A.2,5, Petrukovich A.2
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Afiliações:
- Skobeltsyn Institute of Nuclear Physics
- Space Research Institute
- Faculty of Physics
- Financial University under the Government of the Russian Federation
- Moscow Institute of Physics and Technology (State University)
- Edição: Volume 42, Nº 8 (2016)
- Páginas: 749-760
- Seção: Space Plasma
- URL: https://journals.rcsi.science/1063-780X/article/view/185900
- DOI: https://doi.org/10.1134/S1063780X16080079
- ID: 185900
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Resumo
The effects of interaction of solar cosmic rays (SCRs) with the heliospheric current sheet (HCS) in the solar wind are analyzed. A self-consistent kinetic model of the HCS is developed in which ions with quasiadiabatic dynamics can present. The HCS is considered an equilibrium embedded current structure in which two main plasma species with different temperatures (the low-energy background plasma of the solar wind and the higher energy SCR component) contribute to the current. The obtained results are verified by comparing with the results of numerical simulations based on solving equations of motion by the particle tracing method in the given HCS magnetic field with allowance for SCR particles. It is shown that the HCS is a relatively thin multiscale current configuration embedded in a thicker plasma layer. In this case, as a rule, the shear (tangential to the sheet current) component of the magnetic field is present in the HCS. Taking into account high-energy SCR particles in the HCS can lead to a change of its configuration and the formation of a multiscale embedded structure. Parametric family of solutions is considered in which the current balance in the HCS is provided at different SCR temperatures and different densities of the high-energy plasma. The SCR densities are determined at which an appreciable (detectable by satellites) HCS thickening can occur. Possible applications of this modeling to explain experimental observations are discussed.
Sobre autores
H. Malova
Skobeltsyn Institute of Nuclear Physics; Space Research Institute
Autor responsável pela correspondência
Email: hmalova@yandex.ru
Rússia, Moscow, 119991; Profsoyuznaya ul. 84/32, Moscow, 117997
V. Popov
Space Research Institute; Faculty of Physics; Financial University under the Government of the Russian Federation
Email: hmalova@yandex.ru
Rússia, Profsoyuznaya ul. 84/32, Moscow, 117997; Moscow, 119991; Leningradskii pr. 49, Moscow, 125993
E. Grigorenko
Space Research Institute
Email: hmalova@yandex.ru
Rússia, Profsoyuznaya ul. 84/32, Moscow, 117997
A. Dunko
Space Research Institute; Moscow Institute of Physics and Technology (State University)
Email: hmalova@yandex.ru
Rússia, Profsoyuznaya ul. 84/32, Moscow, 117997; Institutskii per. 9, Dolgoprudnyi, Moscow oblast, 141700
A. Petrukovich
Space Research Institute
Email: hmalova@yandex.ru
Rússia, Profsoyuznaya ul. 84/32, Moscow, 117997