An MHD simulation of energy flow in the solar wind, magnetosphere, and ionosphere system: Steady convection events

1996 ◽  
Vol 18 (8) ◽  
pp. 247-251 ◽  
Author(s):  
T Ogino ◽  
R.J Walker ◽  
M Ashour-Abdalla
Keyword(s):  
Solar Wind ◽  
Energy Flow ◽  
Mhd Simulation ◽  
Steady Convection

Magnetic Energy Flow in the Solar Wind

1972 ◽  
Vol 174 ◽  
pp. 151 ◽  
Author(s):  
Jerry L. Modisette
Keyword(s):  
Solar Wind ◽  
Energy Flow ◽  
Magnetic Energy

scholarly journals Different magnetospheric modes: solar wind driving and coupling efficiency

2009 ◽  
Vol 27 (11) ◽  
pp. 4281-4291 ◽  
Author(s):  
N. Partamies ◽  
T. I. Pulkkinen ◽  
R. L. McPherron ◽  
K. McWilliams ◽  
C. R. Bryant ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Speed ◽  
Coupling Efficiency ◽  
Slow Solar Wind ◽  
Cycle Phase ◽  
Particle Injection ◽  
Superposed Epoch Analysis ◽  
Magnetospheric Convection ◽  
Epoch Analysis ◽  
Steady Convection

Abstract. This study describes a systematic statistical comparison of isolated non-storm substorms, steady magnetospheric convection (SMC) intervals and sawtooth events. The number of events is approximately the same in each group and the data are taken from about the same years to avoid biasing by different solar cycle phase. The very same superposed epoch analysis is performed for each event group to show the characteristics of ground-based indices (AL, PCN, PC potential), particle injection at the geostationary orbit and the solar wind and IMF parameters. We show that the monthly occurrence of sawtooth events and isolated non-stormtime substorms closely follows maxima of the geomagnetic activity at (or close to) the equinoxes. The most strongly solar wind driven event type, sawtooth events, is the least efficient in coupling the solar wind energy to the auroral ionosphere, while SMC periods are associated with the highest coupling ratio (AL/EY). Furthermore, solar wind speed seems to play a key role in determining the type of activity in the magnetosphere. Slow solar wind is capable of maintaining steady convection. During fast solar wind streams the magnetosphere responds with loading–unloading cycles, represented by substorms during moderately active conditions and sawtooth events (or other storm-time activations) during geomagnetically active conditions.

Ionospheric Power Consumption in Global MHD Simulation Predicted From Solar Wind Measurements

2004 ◽  
Vol 32 (4) ◽  
pp. 1511-1518 ◽  
Author(s):  
M. Palmroth ◽  
H.E.J. Koskinen ◽  
T.I. Pulkkinen ◽  
P. Janhunen
Keyword(s):  
Solar Wind ◽  
Power Consumption ◽  
Mhd Simulation ◽  
Wind Measurements ◽  
Global Mhd Simulation

An MHD simulation of the interaction of the solar wind with the outflowing plasma from a comet

1986 ◽  
Vol 13 (9) ◽  
pp. 929-932 ◽  
Author(s):  
Tatsuki Ogino ◽  
Raymond J. Walker ◽  
Maha Ashour-Abdalla
Keyword(s):  
Solar Wind ◽  
Mhd Simulation

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>

scholarly journals Full compressible 3D MHD simulation of solar wind

2020 ◽  
Vol 500 (4) ◽  
pp. 4779-4787
Author(s):  
Takuma Matsumoto
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Solar Physics ◽  
Mass Loss Rate ◽  
Three Dimensional ◽  
Lower Atmosphere ◽  
Fast Solar Wind ◽  
Solar Mass ◽  
Mhd Simulation ◽  
Driving Mechanisms

ABSTRACT Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance s of 27 solar radii (R⊙). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass-loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region (s > 1.3 R⊙), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region (s < 1.03 R⊙) as well.

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