heliosphere - lectures 5-7
DESCRIPTION
Lecture 5 (Sep. 27, 2005) Solar wind formation and acceleration (how the Sun generates it’s solar wind. Why Does the Sun has a wind?) - Interplanetary magnetic field (How the Magnetic Field from the Sun is carried into space? How does it look?) Corotating interaction regions - PowerPoint PPT PresentationTRANSCRIPT
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Heliosphere - Lectures 5-7
@P.Frisch
Lecture 5 (Sep. 27, 2005) -Solar wind formation and acceleration(how the Sun generates it’s solar wind. Why Does the Sun has a wind?)
- Interplanetary magnetic field(How the Magnetic Field from the Sun is carried into space? How does it look?)
-Corotating interaction regions(what are they? How do they form?)
-Heliosphere during the solar cycle(the Sun changes every 11 years-so how the HeliosphereReacts to that?)
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@P.Frisch
Lecture 6 (Oct. 4, 2005)-CMEs in the interplanetary space (magnetic clouds),(How CMEs propagate in the heliosphere)
-interplanetary shocks(CMEs pile up material forming shocks-how those shocks propagate in space)
-shock physics(what happens at a shock?)
-energetic particles in the heliosphere (galactic, anomalous cosmic rays and solar energetic particles) (who are they? Where do they come from?Which ones are the most hazardous to Earth?)
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@P.Frisch
Lecture 7 (Oct. 18, 2005)-Solar wind interaction with the nearby interstellar medium.(the solar system interacts with the interstellar medium-how this interacts happens? How itaffects the Heliosphere, Earth and Space Weather?
I will also talk about the State-of-the Art of What is done today to tackle these problem:Which numerical techniques are being used!
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A global view of the Heliosphere
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Solar Wind: Bi-Modal Structure
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Property (1 AU) Slow Wind Fast WindFlow Speed 400 km/s 750 km/s Density 7 cm-3 3 cm-3 Variance "large", >50% Variance "small", <50%Temperature T(proton, 1AU) ~ 200,000 K T(proton, 1 AU) ~ 50,000 K
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Magnetic Structure of the Sun
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Helmet Streamers
Open and closed Field Lines
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Heliospheric Current Sheet
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Propagating Shocks
• Analogy with sonic booms
• Efficient particle accelerators
• Radiation Environment and Space Weather
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Computational Modeling Effort
Why its so hard?Need of a 3 Dimensional ModelPlasma: Fluid or KineticEnergetic particles (acceleration)Different domains and regimes: need of an Adaptive grid
Example of a grid:
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Using the Space Weather Modeling Framework (SWMF) developed by Univ. of Michigan
Realistic photospheric fields Current Sheet
CR2008 (AR1046) Resolution: 1/64 RS; 4 million cells
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Movie of the Interaction of the Solar System with the Interstellar
Medium
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LASCO CME