Time‐Dependent Hybrid Plasma Simulations of Lunar Electromagnetic Induction in the Solar Wind

2019 ◽  
Vol 46 (8) ◽  
pp. 4151-4160 ◽  
Author(s):  
H. Fuqua Haviland ◽  
A. R. Poppe ◽  
S. Fatemi ◽  
G. T. Delory ◽  
I. Pater
Keyword(s):  
Solar Wind ◽  
Electromagnetic Induction ◽  
Time Dependent ◽  
Hybrid Plasma ◽  
Plasma Simulations

scholarly journals Ion Charge States in a Time-Dependent Wave-Turbulence-Driven Model of the Solar Wind

Solar Physics ◽  
2019 ◽  
Vol 294 (1) ◽  
Author(s):  
Roberto Lionello ◽  
Cooper Downs ◽  
Jon A. Linker ◽  
Zoran Mikić ◽  
John Raymond ◽  
...  
Keyword(s):  
Solar Wind ◽  
Time Dependent ◽  
Wave Turbulence ◽  
Charge States

scholarly journals Compacting the description of a time-dependent multivariable system and its multivariable driver by reducing the state vectors to aggregate scalars: the Earth's solar-wind-driven magnetosphere

2019 ◽  
Vol 26 (4) ◽  
pp. 429-443 ◽  
Author(s):  
Joseph E. Borovsky ◽  
Adnane Osmane
Keyword(s):  
Solar Wind ◽  
State Vector ◽  
Complexity Analysis ◽  
Low Noise ◽  
Time Dependent ◽  
Permutation Entropy ◽  
System Response ◽  
System A ◽  
Driven System ◽  
Time Dependent System

Abstract. Using the solar-wind-driven magnetosphere–ionosphere–thermosphere system, a methodology is developed to reduce a state-vector description of a time-dependent driven system to a composite scalar picture of the activity in the system. The technique uses canonical correlation analysis to reduce the time-dependent system and driver state vectors to time-dependent system and driver scalars, with the scalars describing the response in the system that is most-closely related to the driver. This reduced description has advantages: low noise, high prediction efficiency, linearity in the described system response to the driver, and compactness. The methodology identifies independent modes of reaction of a system to its driver. The analysis of the magnetospheric system is demonstrated. Using autocorrelation analysis, Jensen–Shannon complexity analysis, and permutation-entropy analysis the properties of the derived aggregate scalars are assessed and a new mode of reaction of the magnetosphere to the solar wind is found. This state-vector-reduction technique may be useful for other multivariable systems driven by multiple inputs.

scholarly journals Generation and evolution of interplanetary slow shocks

1996 ◽  
Vol 14 (4) ◽  
pp. 375-382 ◽  
Author(s):  
C.-C. Wu ◽  
S. T. Wu ◽  
M. Dryer
Keyword(s):  
Solar Wind ◽  
Mach Number ◽  
Solar Radius ◽  
Time Dependent ◽  
The Sun ◽  
Wave Perturbation ◽  
One Dimensional ◽  
Slow Shock ◽  
Square Wave ◽  
Pass Through

Abstract. It is well known that most MHD shocks observed within 1 AU are MHD fast shocks. Only a very limited number of MHD slow shocks are observed within 1 AU. In order to understand why there are only a few MHD slow shocks observed within 1 AU, we use a one-dimensional, time-dependent MHD code with an adaptive grid to study the generation and evolution of interplanetary slow shocks (ISS) in the solar wind. Results show that a negative, nearly square-wave perturbation will generate a pair of slow shocks (a forward and a reverse slow shock). In addition, the forward and the reverse slow shocks can pass through each other without destroying their characteristics, but the propagating speeds for both shocks are decreased. A positive, square-wave perturbation will generate both slow and fast shocks. When a forward slow shock (FSS) propagates behind a forward fast shock (FFS), the former experiences a decreasing Mach number. In addition, the FSS always disappears within a distance of 150R⊙ (where R⊙ is one solar radius) from the Sun when there is a forward fast shock (with Mach number ≥1.7) propagating in front of the FSS. In all tests that we have performed, we have not discovered that the FSS (or reverse slow shock) evolves into a FFS (or reverse fast shock). Thus, we do not confirm the FSS-FFS evolution as suggested by Whang (1987).

scholarly journals Self-consistent and Time-dependent Solar Wind Models

1997 ◽  
Vol 474 (2) ◽  
pp. L143-L145 ◽  
Author(s):  
K. K. Ong ◽  
Z. E. Musielak ◽  
R. Rosner ◽  
S. T. Suess ◽  
M. E. Sulkanen
Keyword(s):  
Solar Wind ◽  
Time Dependent ◽  
Self Consistent

Solar Wind Variation with the Cycle

2000 ◽  
Vol 179 ◽  
pp. 423-429
Author(s):  
I. S. Veselovsky ◽  
A. V. Dmitriev ◽  
A. V. Suvorova ◽  
M. V. Tarsina
Keyword(s):  
Solar Wind ◽  
Coronal Holes ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Time Dependent ◽  
Solar Cycles ◽  
Solar Wind Density ◽  
Plasma Parameters ◽  
Decadal Variations ◽  
Wind Measurements

AbstractThe cyclic evolution of the heliospheric plasma parameters is related to the time-dependent boundary conditions in the solar corona. “Minimal” coronal configurations correspond to the regular appearance of the tenuous, but hot and fast plasma streams from the large polar coronal holes. The denser, but cooler and slower solar wind is adjacent to coronal streamers. Irregular dynamic manifestations are present in the corona and the solar wind everywhere and always. They follow the solar activity cycle rather well. Because of this, the direct and indirect solar wind measurements demonstrate clear variations in space and time according to the minimal, intermediate and maximal conditions of the cycles. The average solar wind density, velocity and temperature measured at the Earth’s orbit show specific decadal variations and trends, which are of the order of the first tens per cent during the last three solar cycles. Statistical, spectral and correlation characteristics of the solar wind are reviewed with the emphasis on the cycles.

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