the solar wind - cpaess · the variable solar wind at 1 au n is proton density, v ... the...
TRANSCRIPT
![Page 1: The Solar Wind - CPAESS · The Variable Solar Wind at 1 AU n is proton density, V ... The Heliospheric Current Sheet and the Solar Dipole. Solar Latitude and Solar Cycle Effects:](https://reader031.vdocument.in/reader031/viewer/2022022603/5b5ae6157f8b9ab8578ce6d5/html5/thumbnails/1.jpg)
Structure and Evolution of the Three Dimensional Solar Wind
J. T. GoslingLASP, University of Colorado
Boulder, CO
Heliophysics Summer School, 30 July, 2011
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The Solar Origin of the Solar Wind
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Parker’s Isothermal Solar Wind Model
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Parker’s Model of the Heliospheric Magnetic Field
Axes are heliocentric distance in units of AU.
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The Variable Solar Wind at 1 AU
n is proton density, Vsw is solar wind speed, B is magnetic field strength, A(He) is He++/H+ ratio, Tp is proton temperature, Te is electron temperature, Tα is alpha particle temperature, Cs is sound speed, CA is Alfven speed.
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Commonly Observed Ionization States in the Solar Wind
He2+
C5+, C6+
O6+ to O8+
Si7+ to Si10+
Fe8+ to Fe14+
Unusual ionization states in portions of ICMEs:
He+ and Fe16+
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Coronal and Solar Wind Stream Structure
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The Heliospheric Current Sheet and the Solar Dipole
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Solar Latitude and Solar Cycle Effects: Ulysses
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Characteristics of Solar Wind Stream Structure
1-hr averaged data
Np (cm-3)
Tp (K)
P (dyne cm-2
V (km s-1)
Phi (Deg)
Br (nT)
|B| (nT)
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Evolution of Stream Structure with Heliocentric Distance
FR 1-D Compressible
Fluid Simulation
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Damped High-Speed Streams in the Outer Heliosphere
Voyager 2 data obtained at ~18 AU
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Stream Evolution in Two Dimensions
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Flow Deflections in CIRs Observed by Ulysses in the Opposite Solar Hemispheres
Flow Angles Relative to Radial
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Forward and Reverse Shocks Observed by Ulysses During its First Solar Orbit
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Corotating Interaction Regions in 3D
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A Meridional Cut Through Stream Structure at a Fixed Longitude
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Solar Wind Electrons
Integrated ver all look directions
Suprathermal Pitch Angle Distribution
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Coronal Mass Ejections and Transient Solar Wind Disturbances
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A Simple 1D Fluid Simulation of a Solar Wind Disturbance Driven by a Fast CME
FR
Shown at time when leading edge of disturbance reaches 1 AU.
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3D Simulation of CME-Driven Disturbances in a Simply Structured, Tilted Dipole Solar Wind
Colors indicate the CME material injected into the simulations
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CMEs in the Solar Wind
(ratio of gas pressure to magnetic field pressure)
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The Magnetic Field Topology of CMEs and the Problem of Magnetic Flux Balance
3D magnetic reconnection within the magnetic legs of a CME
Possible mixture of resulting field topologies
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Sketch Illustrating Effect of Suddenly Decreasing the Speed of the Solar Outflow on a Particular Field Line
This sketch ignores dynamic effects associated with the rarefaction produced by a sudden drop in speed.
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Field Lines Resulting From a Combination of Differential Rotation and a Rigidly Rotating Dipole
HMF lines originating from 70˚ S in Fisk’s model (a) and Parker’s
model (b).
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Variation of Solar Rotation-Averaged Magnetic Field Strength Over 4 Solar Activity Cycles
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Comparison of Solar Wind Between Cycles 22 (red) and 23 (blue)
as Function of Heliolatitude
Ulysses Data
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Lower Particle Density and Dynamic Pressure Near Most Recent Solar Minimum
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THE END