Research output: Contribution to journal › Article › peer-review
Magnetospheric "penetration" of IMF By viewed through the lens of an empirical RBF modeling. / Tsyganenko, N. A. ; Andreeva, V. A.
In: Journal of Geophysical Research: Space Physics, Vol. 125, No. 1, e2019JA027439, 01.01.2020.Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - Magnetospheric "penetration" of IMF By viewed through the lens of an empirical RBF modeling
AU - Tsyganenko, N. A.
AU - Andreeva, V. A.
N1 - Publisher Copyright: ©2019. American Geophysical Union. All Rights Reserved. Copyright: Copyright 2020 Elsevier B.V., All rights reserved.
PY - 2020/1/1
Y1 - 2020/1/1
N2 - The spiral structure of the interplanetary magnetic field (IMF) is known to induce intramagnetospheric azimuthal magnetic field urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0002, which strongly correlates with the IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0003. We reconstruct this effect for the first time in 3‐D, using a large set of data taken in the near/inner magnetosphere and a flexible magnetic field model based on expansions in radial basis functions (RBF). The RBF model serves here as a magnifying glass with tunable resolution, focused on the specific region of interest. In this study, we used it to explore the IMF‐induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0004 both on a global scale (i.e., for the entire range of local times) and in the night sector only, to better visualize details in the region with the strongest “penetration” magnitude. The induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0005 was found to maximize on the nightside at distances urn:x-wiley:jgra:media:jgra55432:jgra55432-math-000610–12 urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0007, where it concentrates around the solar‐magnetic equator and bifurcates into a pair of peaks located in predawn and postdusk sectors. The urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0008 “penetration” is associated with the IMF‐induced asymmetry of field‐aligned currents at the plasma sheet boundary. Even on a statistical level, the peak values of the induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0009 can substantially exceed the external IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0010. The effect is significantly stronger under southward IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0011 conditions and grows with increasing geodipole tilt angle.
AB - The spiral structure of the interplanetary magnetic field (IMF) is known to induce intramagnetospheric azimuthal magnetic field urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0002, which strongly correlates with the IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0003. We reconstruct this effect for the first time in 3‐D, using a large set of data taken in the near/inner magnetosphere and a flexible magnetic field model based on expansions in radial basis functions (RBF). The RBF model serves here as a magnifying glass with tunable resolution, focused on the specific region of interest. In this study, we used it to explore the IMF‐induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0004 both on a global scale (i.e., for the entire range of local times) and in the night sector only, to better visualize details in the region with the strongest “penetration” magnitude. The induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0005 was found to maximize on the nightside at distances urn:x-wiley:jgra:media:jgra55432:jgra55432-math-000610–12 urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0007, where it concentrates around the solar‐magnetic equator and bifurcates into a pair of peaks located in predawn and postdusk sectors. The urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0008 “penetration” is associated with the IMF‐induced asymmetry of field‐aligned currents at the plasma sheet boundary. Even on a statistical level, the peak values of the induced urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0009 can substantially exceed the external IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0010. The effect is significantly stronger under southward IMF urn:x-wiley:jgra:media:jgra55432:jgra55432-math-0011 conditions and grows with increasing geodipole tilt angle.
KW - магнитосфера
KW - солнечный ветер
KW - геомагнитное поле
KW - моделирование
KW - магнитосфера
KW - солнечный ветер
KW - геомагнитное поле
KW - моделирование
KW - magnetosphere
KW - modeling
KW - interplanetary magnetic field
KW - spacecraft data
KW - solar wind
KW - CONVECTION
KW - CURRENTS
KW - SHEET
KW - DEPENDENCE
KW - ASYMMETRIES
KW - COMPONENT
UR - http://www.scopus.com/inward/record.url?scp=85081413201&partnerID=8YFLogxK
UR - https://www.mendeley.com/catalogue/2e11380d-e85b-389b-bba2-120cf6d76286/
U2 - 10.1029/2019JA027439
DO - 10.1029/2019JA027439
M3 - Article
VL - 125
JO - Journal of Geophysical Research: Biogeosciences
JF - Journal of Geophysical Research: Biogeosciences
SN - 0148-0227
IS - 1
M1 - e2019JA027439
ER -
ID: 52005862