1. Thomas Zurbuchen University of Michigan thomasz@umich.edu The Structure and Sources of the Solar Wind during the Solar Cycle

2. Contents Space weather and heliospheric structure Solar cycle –What happens in the corona? –What happens to the heliospheric current sheet? Heliospheric polarity change –What happens to the solar wind? Identification of solar wind sources Conclusions

3. Satellite upsets: GOES

4. Transformer damage

5. Solar Cycle: Sunspot Numbers

6. Solar Magnetic Cycle

8. Propagation and Heliospheric Interaction

9. Geospace Interactions

10. Heliospheric Structure? Major effects of solar storms are caused by swept-up heliospheric plasma. Energetic particles release from the Sun follow the magnetic field in the heliosphere.

11. The Corona

12. Solar Minimum Corona Solar corona falls into two areas with fundamentally different magnetic topologies. High latitudes: coronal holes Low latitudes: large loops -> streamers

13. Solar Minimum Corona

14. Solar Maximum Corona Open magnetic field regions appear at all latitudes. In principle, still two fundamentally different magnetic topologies. Highly transient evolution on many time- scales. Current status of research: Use time- stationary MHD solution with parameterized heating.

15. Photospheric magnetic field

16. Solar Maximum Corona

17. Solar Minimum Corona Overall structure well approximated by stationary potential field model. Assume outside surface is conductor.

18. Magnetic field in 1998. Liewer et al., 2002. 1) Larger  range of sources 2) Long magnetic connections in 

19. Magnetic field in 2001 Linker et al., 2001.

20. Magnetic loops are heated

21. The Heliosphere

22. Major questions What is the large-scale structure of the heliosphere during the solar cycle? How does it relate to the magnetic structure of the corona? How does the heliospheric field change?

23. The Current Sheet (CS) Separates magnetic polarities

24. Solar Minimum CS

25. Solar Maximum CS

27. Heliospheric Polarity Change Heliospheric field is calculated under following approximation (Riley et al, for details) 1.Measure Earth-pointing magnetic field each Carrington rotation. 2.Assume stationary condition for this time and calculate coronal magnetic field using certain approximation on heating. 3.Use fluid code to project this field into heliosphere.

29. Heliospheric Polarity Change Fundamental processes: –Magnetic flux emergence at small geometrical scale. –Differential rotation and meridional motion that pushes and tears magnetic field and forces interactions of photospheric magnetic flux. –Reconnection between magnetic field lines, open and closed. Neither of these processes are well understood and currently modeled!

30. Surface Motions Images from Stanford Observatory

31. Reconnection effects Loop -loop Loop –open field line

32. A physical model: Fisk and Schwadron, 2001; Zurbuchen et al., 2004 Realize that there are open and closed field lines that have their constraints. Solar wind comes from closed structures, released by reconnection. Open heliospheric magnetic field lines: “diffusive” motions due to reconnections convective motions - differential rotation - meridional flow

33. Solar minimum, high latitudes

34. Solar wind sources Common assumption by modelers: –All solar wind comes from coronal holes. –Coronal heating differences produce fast and slow solar wind. Composition data: –There are two fundamentally different sources of solar wind that result in fast and slow flows. –These sources directly relate to the reconnection processes just described!

35. Composition Solar wind elemental composition from Ulysses. Both, solar maximum and solar minimum solar wind consist of coronal hole associated and streamer associated wind. Zurbuchen et al., 2002.

36. Slow solar wind Sources Compositional patterns in coronal loops of 100 Mm are observed to be like slow solar wind. These loops are likely source of slow solar wind. Plasma must be released through reconnection.

37. Important questions Fundamental processes: –Magnetic flux emergence at small geometrical scale. –Differential rotation and meridional motion that pushes and tears magnetic field and forces interactions of photospheric magnetic flux. –Reconnection between magnetic field lines, open and closed. What are the reasons for these processes inside the Sun? What is the physics of magnetic reconnection? How does it relate to solar wind and particle acceleration?

38. Solar Minimum Sources

39. Solar Maximum Sources

40. Summary Understanding and predicting space weather and its engineering consequences has become very important. This will require major progress in fundamental knowledge of solar processes currently not well known. We are at the transition of fundamental research and applications of interest for industry and the Nations economy.

41. That’s it…

42. Space Weather Damages Upsets and failures of space systems due to space radiation Satellite life-time issues due to enhanced atmospheric drag Powergrid disruptions Negative effects on communications systems and GPS.