Heliosphere Intro Opher

Heliosphere - Lectures 5-7: 

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 Heliosphere Reacts to that?)

Slide2: 

@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?)

Slide3: 

@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 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!

The Heliosphere: 

The Heliosphere A global view of the Heliosphere

Slide5: 

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

Slide6: 

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

Heliospheric Current Sheet: 

Heliospheric Current Sheet

Propagating Shocks: 

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

Computational Modeling Effort: 

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:

Halloween Storms: 

Halloween Storms 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

Movie of the Interaction of the Solar System with the Interstellar Medium: 

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

LASCO CME: 

LASCO CME