Solar wind-magnetosphere coupling in the form of recurrent substorms with one-hour periodicity

2020 ◽  
Author(s):  
Andreas Keiling ◽  
Masahito Nosé ◽  
Vassillis Angelopoulos
Keyword(s):  
Solar Wind ◽  
Repetitive Behavior ◽  
Response Mode ◽  
Magnetospheric Substorm ◽  
Periodic Behavior ◽  
Recurrence Period ◽  
Mhd Simulations ◽  
Reconnection Site ◽  
Kinetic Effects ◽  
Satisfactory Answer

<p>The magnetospheric substorm is a response mode of the magnetosphere to solar wind driving. It has been shown that substorms can show repetitive behavior (that is, three or more substorms following each other with a quasi-period). The most common period is approximately three hours. A conclusive and satisfactory answer to the cause of this periodicity has not yet been given. Very limited mentioning of a shorter recurrence period, namely around one hour, has sparsely been appeared in the literature. In this presentation, we report on this lesser studied periodicity, giving observational examples from the THEMIS fleet. We compare the observations with global magnetosphere MHD simulations (BATS-R-US) of solar wind-magnetosphere coupling that incorporate kinetic corrections at the reconnection site. The similarity is striking, suggesting that indeed kinetic effects in tail reconnection are responsible - at least in some cases - for this periodic behavior of the magnetosphere.</p>

Embedding particle-in-cell simulations in global magnetohydrodynamic simulations of the magnetosphere

2019 ◽  
Vol 85 (1) ◽  
Author(s):  
Raymond J. Walker ◽  
Giovanni Lapenta ◽  
Jean Berchem ◽  
Mostafa El-Alaoui ◽  
David Schriver
Keyword(s):  
Solar Wind ◽  
Mhd Simulation ◽  
Magnetospheric Substorm ◽  
Pic Simulation ◽  
Particle In Cell ◽  
Mhd Simulations ◽  
Dayside Magnetopause ◽  
Thin Current Sheet ◽  
Cell Simulation ◽  
Magnetohydrodynamic Simulations

We have combined global magnetohydrodynamic (MHD) simulations of the solar wind and magnetosphere interaction with an implicit particle-in-cell simulation (PIC) and used this approach to model magnetic reconnection at both the dayside magnetopause and in the magnetotail plasma sheet. In this approach, we first model the magnetospheric configuration driven by the solar wind using the MHD simulation. At a time of interest (usually when a thin current sheet has formed in the MHD simulation), we load a large particle-in-cell simulation with plasma and fields based on the MHD state. We use the MHD results to set the boundary conditions on the PIC simulation. The coupling between the two models is one way – the PIC results do not change the MHD results. In these calculations, we use the UCLA global MHD code and the iPic3D implicit particle-in-cell code. In this paper we describe this technique in detail. As an example of this approach, we present PIC results on reconnection in the magnetotail during a magnetospheric substorm.

scholarly journals Global MHD Simulations of the Earth's Bow Shock Shape and Motion Under Variable Solar Wind Conditions

2018 ◽  
Vol 123 (1) ◽  
pp. 259-271 ◽  
Author(s):  
L. Mejnertsen ◽  
J. P. Eastwood ◽  
H. Hietala ◽  
S. J. Schwartz ◽  
J. P. Chittenden
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Mhd Simulations ◽  
Earth’S Bow Shock

scholarly journals Common solar wind drivers behind magnetic storm–magnetospheric substorm dependency

2018 ◽  
Vol 8 (1) ◽  
Author(s):  
Jakob Runge ◽  
Georgios Balasis ◽  
Ioannis A. Daglis ◽  
Constantinos Papadimitriou ◽  
Reik V. Donner
Keyword(s):  
Solar Wind ◽  
Magnetic Storm ◽  
Magnetospheric Substorm

scholarly journals Plasma environment of magnetized asteroids: a 3-D hybrid simulation study

2006 ◽  
Vol 24 (1) ◽  
pp. 407-414 ◽  
Author(s):  
S. Simon ◽  
T. Bagdonat ◽  
U. Motschmann ◽  
K.-H. Glassmeier
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Hybrid Simulation ◽  
Interaction Region ◽  
Bow Shock ◽  
The Other ◽  
Simulation Code ◽  
Kinetic Effects ◽  
Intrinsic Magnetic Moment ◽  
The One

Abstract. The interaction of a magnetized asteroid with the solar wind is studied by using a three-dimensional hybrid simulation code (fluid electrons, kinetic ions). When the obstacle's intrinsic magnetic moment is sufficiently strong, the interaction region develops signs of magnetospheric structures. On the one hand, an area from which the solar wind is excluded forms downstream of the obstacle. On the other hand, the interaction region is surrounded by a boundary layer which indicates the presence of a bow shock. By analyzing the trajectories of individual ions, it is demonstrated that kinetic effects have global consequences for the structure of the interaction region.

scholarly journals Comparative Study on Planetary Magnetosphere in the Solar System

Sensors ◽  
2020 ◽  
Vol 20 (6) ◽  
pp. 1673
Author(s):  
Ching-Ming Lai ◽  
Jean-Fu Kiang
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar System ◽  
Comparative Study ◽  
Magnetic Reconnection ◽  
Tilt Angle ◽  
Planetary Magnetosphere ◽  
Field Distributions ◽  
Mhd Simulations ◽  
The Magnetic Field

The magnetospheric responses to solar wind of Mercury, Earth, Jupiter and Uranus are compared via magnetohydrodynamic (MHD) simulations. The tilt angle of each planetary field and the polarity of solar wind are also considered. Magnetic reconnection is illustrated and explicated with the interaction between the magnetic field distributions of the solar wind and the magnetosphere.

scholarly journals Proton Kinetic Effects and Turbulent Energy Cascade Rate in the Solar Wind

2013 ◽  
Vol 111 (20) ◽  
Author(s):  
K. T. Osman ◽  
W. H. Matthaeus ◽  
K. H. Kiyani ◽  
B. Hnat ◽  
S. C. Chapman
Keyword(s):  
Solar Wind ◽  
Turbulent Energy ◽  
Energy Cascade ◽  
Kinetic Effects

scholarly journals Direct evidence for kinetic effects associated with solar wind reconnection

2015 ◽  
Vol 5 (1) ◽  
Author(s):  
Xiaojun Xu ◽  
Yi Wang ◽  
Fengsi Wei ◽  
Xueshang Feng ◽  
Xiaohua Deng ◽  
...  
Keyword(s):  
Solar Wind ◽  
Direct Evidence ◽  
Kinetic Effects

scholarly journals Unusual Location of the Geotail Magnetopause Near Lunar Orbit: A Case Study

2021 ◽  
Author(s):  
Wensai Shang ◽  
Binbin Tang ◽  
Quanqi Shi ◽  
Et al
Keyword(s):  
Solar Wind ◽  
Velocity Vector ◽  
Solar Wind Velocity ◽  
Full Moon ◽  
Interplanetary Shock ◽  
Time Intervals ◽  
Mhd Simulation ◽  
Mhd Simulations ◽  
Solar Wind Flow

<p>The Earth's magnetopause is highly variable in location and shape and is modulated by solar wind conditions. On 8 March 2012, the ARTEMIS probes were located near the tail current sheet when an interplanetary shock arrived under northward interplanetary magnetic field conditions and recorded an abrupt tail compression at ∼(-60, 0, -5) Re in Geocentric Solar Ecliptic coordinate in the deep magnetotail. ~ 10 minutes later, the probes crossed the magnetopause many times within an hour after the oblique interplanetary shock passed by. The solar wind velocity vector downstream from the shock was not directed along the Sun-Earth line but had a significant Y component. We propose that the compressed tail was pushed aside by the appreciable solar wind flow in the Y direction. Using a virtual spacecraft in a global magnetohydrodynamic (MHD) simulation, we reproduce the sequence of magnetopause crossings in the X-Y plane observed by ARTEMIS under oblique shock conditions, demonstrating that the compressed magnetopause is sharply deflected at lunar distances in response to the shock and solar wind Vy effects. The results from two global MHD simulations show that the shocked magnetotail at lunar distances is mainly controlled by the solar wind direction with a timescale of about a quarter hour, which appears to be consistent with the windsock effect. The results also provide some references for investigating interactions between the solar wind/magnetosheath and lunar nearside surface during full moon time intervals, which should not happen in general.</p>

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