1. 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
(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?)
@P.Frisch

2. -CMEs in the interplanetary space (magnetic clouds),
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

5. Solar Wind: Bi-Modal Structure
Property (1 AU) Slow Wind Fast Wind
Flow Speed 400 km/s km/s
Density cm 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. 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

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

12. LASCO CME