1. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System

2. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Exploring the Planets and Moons in our Solar System The interplanetary medium, the solar wind and its interaction with magnetized planets

3. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Exploring the Planets and Moons in our Solar System The interplanetary medium, the solar wind and its interaction with magnetized planets Space missions to the outer planets

4. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Exploring the Planets and Moons in our Solar System The interplanetary medium, the solar wind and its interaction with magnetized planets Space missions to the outer planets Specific aspects of magnetospheric physics – radio emission

5. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Exploring the Planets and Moons in our Solar System The interplanetary medium, the solar wind and its interaction with magnetized planets Space missions to the outer planets Specific aspects of magnetospheric physics – radio emission Volcanoes and icy worlds

6. Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Exploring the Planets and Moons in our Solar System The interplanetary medium, the solar wind and its interaction with magnetized planets Space missions to the outer planets Specific aspects of magnetospheric physics – radio emission Volcanoes and icy worlds Space Missions to the terrestrial planets

7. Space Research Institute Graz Austrian Academy of Sciences „ CERN, Geneve, June 2006 Helmut O. Rucker The interplanetary medium, the solar wind and its interaction with magnetized planets

8. The central star of our solar system – the Sun

9. Mass loss by the expanding solar atmosphere, i.e. the solar wind: ~ 10 E6 tons per second

10. Viewgraph: Helmet streamer

11. The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)

12. The interplanetary magnetic field is a solar magnetic field drawn out of the Sun by the highly conducting solar wind plasma. Due to the solar rotation a spiral structure is formed. The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)

13. Parker spiral:

14. Solar wind average properties at r ~ 1 AU: Different types of solar wind (sw): Fast sw: 400 < v < 800 km/s, Helium 3 – 4 % Slow sw of minimum type: 250 < v < 400 km/s, Helium < 2 % Slow sw of maximum type: 250 < v < 400 km/s, Helium ~ 4 % Coronal mass ejections (CMEs): 400 < v < 2000 km/s, Helium(++) ~ 30 %

15. Solar wind average properties at r ~ 1 AU:

16. Dipole structure

17. Interaction between the solar wind and planetary magnetic field Solar wind bulk flow = super-sonic flow = super-Alfvenic flow

18. Bow shock: Transition of solar wind plasma described by the Rankine Hugoniot equations bulk speed particle density Plasma pressure plasma temperature Interaction between the solar wind and planetary magnetic field

19. 3D schematics of the terrestrial magnetosphere magnetopause boundary conditions:

20. Magnetic reconnection

23. Courtesy Prange, 2006

25. 1 st reconnection = start of the cycle Courtesy Prange, 2006

28. transport over the poles Courtesy Prange, 2006

30. 2 nd reconnection Courtesy Prange, 2006

31. impulsive acceleration Release of energy ( the stretched configuration contains additional energy to accelerate plasma) Courtesy Prange, 2006

32. ejection of plasma into the magnetotail Courtesy Prange, 2006

33. returning of a « magnetic loop » back to the dayside Courtesy Prange, 2006

35. Cluster Double Star Themis MMS

36. Earth Dynamic Explorer ) UV - 130 nm (Courtesy. L. Frank) Saturn HST-STIS UV - 130 nm (R. Prangé & L Pallier) Jupiter HST-STIS UV - 150 nm (R. Prangé & L Pallier) PLANETARY AURORAE a fascinating phenomen at and around the magnetis poles of magnetized planets

37. Earth Dynamic Explorer ) UV - 130 nm (Courtesy. L. Frank) Saturn HST-STIS UV - 130 nm (R. Prangé & L Pallier) Jupiter HST-STIS UV - 150 nm (R. Prangé & L Pallier) PLANETARY AURORAE a fascinating phenomen at and around the magnetis poles of magnetized planets

39. Summary:

40. Prospect for tomorrow: Saturn, seen by Cassini