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?)

@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?)

@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!

A global view of the Heliosphere

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

Heliospheric Current Sheet

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Propagating Shocks

• Analogy with sonic booms

• Efficient particle accelerators

• Radiation Environment and Space Weather

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:

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