Magnetospheric "penetration" of IMF By viewed through the lens of an empirical RBF modeling

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Magnetospheric "penetration" of IMF By viewed through the lens of an empirical RBF modeling. / Tsyganenko, N. A. ; Andreeva, V. A.

в: Journal of Geophysical Research: Space Physics, Том 125, № 1, e2019JA027439, 01.01.2020.

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

BibTeX

@article{8f92b46420f941a88b81489fc10a92e1,

title = "Magnetospheric {"}penetration{"} of IMF By viewed through the lens of an empirical RBF modeling",

abstract = "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.",

keywords = "магнитосфера, солнечный ветер, геомагнитное поле, моделирование, магнитосфера, солнечный ветер, геомагнитное поле, моделирование, magnetosphere, modeling, interplanetary magnetic field, spacecraft data, solar wind, CONVECTION, CURRENTS, SHEET, DEPENDENCE, ASYMMETRIES, COMPONENT",

author = "Tsyganenko, {N. A.} and Andreeva, {V. A.}",

year = "2020",

month = jan,

day = "1",

doi = "10.1029/2019JA027439",

language = "English",

volume = "125",

journal = "Journal of Geophysical Research: Biogeosciences",

issn = "0148-0227",

publisher = "American Geophysical Union",

number = "1",

}

RIS

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.

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