Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters

Standard

Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters. / Stepanov, N. A.; Sergeev, V. A.; Sormakov, D. A.; Andreeva, V. A.; Dubyagin, S. V.; Ganushkina, N.; Angelopoulos, V.; Runov, A. V.

в: Journal of Geophysical Research: Space Physics, Том 126, № 4, e2020JA028580, 26.03.2021.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Author

Stepanov, N. A. ; Sergeev, V. A. ; Sormakov, D. A. ; Andreeva, V. A. ; Dubyagin, S. V. ; Ganushkina, N. ; Angelopoulos, V. ; Runov, A. V. / Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters. в: Journal of Geophysical Research: Space Physics. 2021 ; Том 126, № 4.

BibTeX

@article{7ba972b114484bd7acf5cb2f7de1edc1,

title = "Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters",

abstract = "To study further the factors and mechanisms controlling 10–150 keV particle fluxes in the inner magnetosphere, we investigate empirically their behavior in the nightside transition region (6–14 Re) depending on solar wind parameters taken at different time lags. We aim to establish the hierarchy of predictors (V, N, Pd, Ekl = VByz sin2(θ/2), etc.) and the optimal range of their time delays, both depending on the distance and local time. We use THEMIS 5-min averaged observations of energetic proton and electron fluxes in 2007–2018 near the plasma sheet midplane and build regression models exploring the combination of predictors, taken at time delays up to 24 h. The model obtained shows that protons and electrons are controlled differently by solar wind parameters: electrons are influenced equally by Vsw and Ekl, whereas protons are controlled mostly by Vsw and Pd and less by Ekl. We found that a wide range of time delays is involved depending on distance and particle energy. Specifically, the Ekl affects the energetic fluxes with time delays up to 24 h (or more), exhibiting the long delays in the innermost regions. As regards the mechanism of Vsw influence, the Vsw-related flux changes are large and, to a large extent, established on the route of the energy flow from solar wind to the plasma sheet and, eventually, the inner magnetosphere. We also identified a new parameter, NBL = VByz cos2(θ/2), which helps to reveal the loss processes in the plasma sheet transition region.",

keywords = "energetic particles, magnetotail, plasma sheet, solar wind dependence, MODEL, DRIVEN, ACCELERATION, ENERGETIC OXYGEN, HYDROGEN, TEMPERATURE, GEOSTATIONARY ORBIT, SEED, SUBSTORMS",

author = "Stepanov, {N. A.} and Sergeev, {V. A.} and Sormakov, {D. A.} and Andreeva, {V. A.} and Dubyagin, {S. V.} and N. Ganushkina and V. Angelopoulos and Runov, {A. V.}",

year = "2021",

month = mar,

day = "26",

doi = "10.1029/2020ja028580",

language = "English",

volume = "126",

journal = "Journal of Geophysical Research: Biogeosciences",

issn = "0148-0227",

publisher = "American Geophysical Union",

number = "4",

}

RIS

TY - JOUR

T1 - Superthermal Proton and Electron Fluxes in the Plasma Sheet Transition Region and Their Dependence on Solar Wind Parameters

AU - Stepanov, N. A.

AU - Sergeev, V. A.

AU - Sormakov, D. A.

AU - Andreeva, V. A.

AU - Dubyagin, S. V.

AU - Ganushkina, N.

AU - Angelopoulos, V.

AU - Runov, A. V.

PY - 2021/3/26

Y1 - 2021/3/26

N2 - To study further the factors and mechanisms controlling 10–150 keV particle fluxes in the inner magnetosphere, we investigate empirically their behavior in the nightside transition region (6–14 Re) depending on solar wind parameters taken at different time lags. We aim to establish the hierarchy of predictors (V, N, Pd, Ekl = VByz sin2(θ/2), etc.) and the optimal range of their time delays, both depending on the distance and local time. We use THEMIS 5-min averaged observations of energetic proton and electron fluxes in 2007–2018 near the plasma sheet midplane and build regression models exploring the combination of predictors, taken at time delays up to 24 h. The model obtained shows that protons and electrons are controlled differently by solar wind parameters: electrons are influenced equally by Vsw and Ekl, whereas protons are controlled mostly by Vsw and Pd and less by Ekl. We found that a wide range of time delays is involved depending on distance and particle energy. Specifically, the Ekl affects the energetic fluxes with time delays up to 24 h (or more), exhibiting the long delays in the innermost regions. As regards the mechanism of Vsw influence, the Vsw-related flux changes are large and, to a large extent, established on the route of the energy flow from solar wind to the plasma sheet and, eventually, the inner magnetosphere. We also identified a new parameter, NBL = VByz cos2(θ/2), which helps to reveal the loss processes in the plasma sheet transition region.

AB - To study further the factors and mechanisms controlling 10–150 keV particle fluxes in the inner magnetosphere, we investigate empirically their behavior in the nightside transition region (6–14 Re) depending on solar wind parameters taken at different time lags. We aim to establish the hierarchy of predictors (V, N, Pd, Ekl = VByz sin2(θ/2), etc.) and the optimal range of their time delays, both depending on the distance and local time. We use THEMIS 5-min averaged observations of energetic proton and electron fluxes in 2007–2018 near the plasma sheet midplane and build regression models exploring the combination of predictors, taken at time delays up to 24 h. The model obtained shows that protons and electrons are controlled differently by solar wind parameters: electrons are influenced equally by Vsw and Ekl, whereas protons are controlled mostly by Vsw and Pd and less by Ekl. We found that a wide range of time delays is involved depending on distance and particle energy. Specifically, the Ekl affects the energetic fluxes with time delays up to 24 h (or more), exhibiting the long delays in the innermost regions. As regards the mechanism of Vsw influence, the Vsw-related flux changes are large and, to a large extent, established on the route of the energy flow from solar wind to the plasma sheet and, eventually, the inner magnetosphere. We also identified a new parameter, NBL = VByz cos2(θ/2), which helps to reveal the loss processes in the plasma sheet transition region.

KW - energetic particles

KW - magnetotail

KW - plasma sheet

KW - solar wind dependence

KW - MODEL

KW - DRIVEN

KW - ACCELERATION

KW - ENERGETIC OXYGEN

KW - HYDROGEN

KW - TEMPERATURE

KW - GEOSTATIONARY ORBIT

KW - SEED

KW - SUBSTORMS

UR - http://www.scopus.com/inward/record.url?scp=85104942069&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/0be941bd-512b-3a87-a533-420c0d483121/

U2 - 10.1029/2020ja028580

DO - 10.1029/2020ja028580

M3 - Article

AN - SCOPUS:85104942069

VL - 126

JO - Journal of Geophysical Research: Biogeosciences

JF - Journal of Geophysical Research: Biogeosciences

SN - 0148-0227

IS - 4

M1 - e2020JA028580

ER -

ID: 76829849