Three-dimensional MHD simulations of the Earth's magnetosphere on Feb 9-10 1995 for northward interplanetary magnetic field and comparison of the lobe field with Geotail observations

The interaction between the solar wind and the Earth’s magnetosphere–ionosphere system is very complex, being essentially the result of the interplay between an external driver, the solar wind, and internal processes to the magnetosphere–ionosphere system. In this framework, modelling the Earth’s magnetosphere–ionosphere response to the changes of the solar wind conditions requires a correct identification of the causality relations between the different parameters/quantities used to monitor this coupling. Nowadays, in the framework of complex dynamical systems, both linear statistical tools and Granger causality models drastically fail to detect causal relationships between time series. Conversely, information theory-based concepts can provide powerful model-free statistical quantities capable of disentangling the complex nature of the causal relationships. In this work, we discuss how to deal with the problem of measuring causal information in the solar wind–magnetosphere–ionosphere system. We show that a time delay of about 30–60 min is found between solar wind and magnetospheric and ionospheric overall dynamics as monitored by geomagnetic indices, with a great information transfer observed between the z component of the interplanetary magnetic field and geomagnetic indices, while a lower transfer is found when other solar wind parameters are considered. This suggests that the best candidate for modelling the geomagnetic response to solar wind changes is the interplanetary magnetic field component B z . A discussion of the relevance of our results in the framework of Space Weather is also provided.

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Turbulence in a global magnetohydrodynamic simulation of the Earth's magnetosphere during northward and southward interplanetary magnetic field

Nonlinear Processes in Geophysics ◽

10.5194/npg-19-165-2012 ◽

2012 ◽

Vol 19 (2) ◽

pp. 165-175 ◽

Cited By ~ 12

Author(s):

M. El-Alaoui ◽

R. L. Richard ◽

M. Ashour-Abdalla ◽

R. J. Walker ◽

M. L. Goldstein

Keyword(s):

Magnetic Field ◽

Interplanetary Magnetic Field ◽

Solar Wind Plasma ◽

Inertial Range ◽

Earth’S Magnetosphere ◽

Power Spectral ◽

Power Spectral Densities ◽

Theoretical Predictions ◽

Earth's Magnetosphere

Abstract. We report the results of MHD simulations of Earth's magnetosphere for idealized steady solar wind plasma and interplanetary magnetic field (IMF) conditions. The simulations feature purely northward and southward magnetic fields and were designed to study turbulence in the magnetotail plasma sheet. We found that the power spectral densities (PSDs) for both northward and southward IMF had the characteristics of turbulent flow. In both cases, the PSDs showed the three scale ranges expected from theory: the energy-containing scale, the inertial range, and the dissipative range. The results were generally consistent with in-situ observations and theoretical predictions. While the two cases studied, northward and southward IMF, had some similar characteristics, there were significant differences as well. For southward IMF, localized reconnection was the main energy source for the turbulence. For northward IMF, remnant reconnection contributed to driving the turbulence. Boundary waves may also have contributed. In both cases, the PSD slopes had spatial distributions in the dissipative range that reflected the pattern of resistive dissipation. For southward IMF there was a trend toward steeper slopes in the dissipative range with distance down the tail. For northward IMF there was a marked dusk-dawn asymmetry with steeper slopes on the dusk side of the tail. The inertial scale PSDs had a dusk-dawn symmetry during the northward IMF interval with steeper slopes on the dawn side. This asymmetry was not found in the distribution of inertial range slopes for southward IMF. The inertial range PSD slopes were clustered around values close to the theoretical expectation for both northward and southward IMF. In the dissipative range, however, the slopes were broadly distributed and the median values were significantly different, consistent with a different distribution of resistivity.

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Magnetospheric access for solar protons during the January 2005 SEP event

Journal of Space Weather and Space Climate ◽

10.1051/swsc/2018040 ◽

2018 ◽

Vol 8 ◽

pp. A55 ◽

Cited By ~ 1

Author(s):

Vladimir V. Kalegaev ◽

Natalia A. Vlasova ◽

Ilya S. Nazarkov ◽

Sophia A. Melkova

Keyword(s):

Magnetic Field ◽

Interplanetary Magnetic Field ◽

High Latitude ◽

Early Phase ◽

Energetic Particle ◽

Field Model ◽

Solar Energetic Particle ◽

Earth’S Magnetosphere ◽

Earth's Magnetosphere ◽

Magnetic Field Model

The early phase of the extraordinary solar energetic particle 20 January, 2005 event having the highest peak flux of any SEP in the past 50 years of protons with energies > 100 MeV is studied. Solar energetic particles (>16 MeV) entry to the Earth’s magnetosphere on January 20, 2005 under northward interplanetary magnetic field conditions is considered based on multi-satellite data analysis and magnetic field simulation. Solar wind parameters and interplanetary magnetic field data, as well as calculations in terms of the A2000 magnetospheric magnetic field model were used to specify conditions in the Earth’s environment corresponding to solar proton event. It was shown that during the early phase of the event energetic particle penetration into the magnetosphere took place in the regions on the magnetopause where the magnetospheric and interplanetary magnetic field vectors are parallel. Complex analysis of the experimental data on particle fluxes in the interplanetary medium (data from ACE spacecraft) and on low-altitude (POES) and geosynchronous (GOES) orbits inside the Earth’s magnetosphere show two regions on the magnetopause responsible for particle access to the magnetosphere: the near equatorial day-side region and open field lines window at the high-latitude magnetospheric boundary. Calculations in terms of A2000 magnetospheric magnetic field model and comparison with SuperDARN images support the link between high-latitude solar energetic particle precipitations and the region at the magnetopause where the magnetospheric field is coupled with northward IMF, allowing solar particles entrance into the magnetosphere and access to the northern polar cap.

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An MHD simulation of the effects of the interplanetary magnetic fieldBycomponent on the interaction of the solar wind with the Earth's magnetosphere during southward interplanetary magnetic field

Journal of Geophysical Research Atmospheres ◽

10.1029/ja091ia09p10029 ◽

1986 ◽

Vol 91 (A9) ◽

pp. 10029 ◽

Cited By ~ 64

Author(s):

T. Ogino ◽

R. J. Walker ◽

M. Ashour-Abdalla ◽

J. M. Dawson

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Interplanetary Magnetic Field ◽

Mhd Simulation ◽

Earth’S Magnetosphere ◽

Earth's Magnetosphere

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Three-dimensional MHD simulations of the steady state magnetosphere with northward interplanetary magnetic field

Journal of Geophysical Research Atmospheres ◽

10.1029/2000ja000066 ◽

2001 ◽

Vol 106 (A1) ◽

pp. 275-287 ◽

Cited By ~ 14

Author(s):

P. N. Guzdar ◽

X. Shao ◽

C. C. Goodrich ◽

K. Papadopoulos ◽

M. J. Wiltberger ◽

...

Keyword(s):

Magnetic Field ◽

Steady State ◽

Interplanetary Magnetic Field ◽

Three Dimensional ◽

Mhd Simulations

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Absence of a long-lived lunar paleomagnetosphere

Science Advances ◽

10.1126/sciadv.abi7647 ◽

2021 ◽

Vol 7 (32) ◽

pp. eabi7647

Author(s):

John A. Tarduno ◽

Rory D. Cottrell ◽

Kristin Lawrence ◽

Richard K. Bono ◽

Wentao Huang ◽

...

Keyword(s):

Magnetic Field ◽

Lunar Regolith ◽

The Moon ◽

Earth’S Magnetosphere ◽

Solar Winds ◽

Planetary Bodies ◽

Earth's Magnetosphere ◽

Impact Glass ◽

Magnetic Inclusions

Determining the presence or absence of a past long-lived lunar magnetic field is crucial for understanding how the Moon’s interior and surface evolved. Here, we show that Apollo impact glass associated with a young 2 million–year–old crater records a strong Earth-like magnetization, providing evidence that impacts can impart intense signals to samples recovered from the Moon and other planetary bodies. Moreover, we show that silicate crystals bearing magnetic inclusions from Apollo samples formed at ∼3.9, 3.6, 3.3, and 3.2 billion years ago are capable of recording strong core dynamo–like fields but do not. Together, these data indicate that the Moon did not have a long-lived core dynamo. As a result, the Moon was not sheltered by a sustained paleomagnetosphere, and the lunar regolith should hold buried 3He, water, and other volatile resources acquired from solar winds and Earth’s magnetosphere over some 4 billion years.

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Three-dimensional Multispecies Simulation of the Solar Wind Interaction with Mars Under Different Interplanetary Magnetic Field Orientations

The Astrophysical Journal ◽

10.3847/1538-4357/ac1ce5 ◽

2021 ◽

Vol 921 (2) ◽

pp. 139

Author(s):

Yun Li ◽

Haoyu Lu ◽

Jinbin Cao ◽

Shibang Li ◽

Christian Mazelle ◽

...

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Interplanetary Magnetic Field ◽

Three Dimensional ◽

Polarity Reversal ◽

Solar Wind Interaction ◽

Magnetic Structures ◽

Parker Spiral ◽

Global Configuration ◽

Spiral Angle

Abstract Without the intrinsic magnetic field, the solar wind interaction with Mars can be significantly different from the interaction with Earth and other magnetized planets. In this paper, we investigate how a global configuration of the magnetic structures, consisting of the bow shock, the induced magnetosphere, and the magnetotail, is modulated by the interplanetary magnetic field (IMF) orientation. A 3D multispecies numerical model is established to simulate the interaction of solar wind with Mars under different IMF directions. The results show that the shock size including the subsolar distance and the terminator radius increases with Parker spiral angle, as is the same case with the magnetotail radius. The location and shape of the polarity reversal layer and inverse polarity reversal layer in the induced magnetotail are displaced to the y < 0 sector for a nonzero flow-aligned IMF component, consistent with previous analytical solutions and observations. The responses of the Martian global magnetic configuration to the different IMF directions suggest that the external magnetic field plays an important role in the solar wind interaction with unmagnetized planets.

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