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Heliosphere - Lectures 5-7

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

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Heliosphere - Lectures 5-7

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  1. 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 Heliosphere • Reacts to that?) Heliosphere - Lectures 5-7 @P.Frisch

  2. 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

  3. 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 it affects 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! @P.Frisch

  4. A global view of the Heliosphere The Heliosphere

  5. Solar Wind: Bi-Modal Structure Property (1 AU) Slow Wind Fast Wind Flow 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

  6. Magnetic Structure of the Sun Helmet Streamers Open and closed Field Lines

  7. Heliospheric Current Sheet

  8. Propagating Shocks • Analogy with sonic booms • Efficient particle accelerators • Radiation Environment and Space Weather

  9. Computational Modeling Effort Why its so hard? Need of a 3 Dimensional Model Plasma: Fluid or Kinetic Energetic particles (acceleration) Different domains and regimes: need of an Adaptive grid Example of a grid:

  10. Using the Space Weather Modeling Framework (SWMF) developed by Univ. of Michigan Halloween Storms Realistic photospheric fields Current Sheet CR2008 (AR1046) Resolution: 1/64 RS; 4 million cells

  11. Movie of the Interaction of the Solar System with the Interstellar Medium

  12. LASCO CME

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