1. Dark Energy in the Solar Corona H.S. Hudson, UCB & SPRC LMSAL, January 31, 2002

2. Dark energy in the solar corona Not the "dark energy" of the cosmos, but B! MHD equilibrium Imperturbable compact event Imperturbable cusp Two CMEs Blow-out of LPS

3. The corona is surprisingly stable. What is the nature of this equilibrium?

4. The corona exhibits a "stick-slip" variability, as shown on any GOES plot

5. The open fraction of coronal field lines (v. roughly the area of the coronal holes) remains approximately constant

6. A. There isn't much braiding observed in quiet-Sun magnetic fields (K. Schrijver, 2001) B. Predictions of the solar wind are happy with a “potential field” source-surface model REMARKS C. So how does “energy build-up” happen?

7. Imperturbability on a compact scale Flares often involve multiple loops that don’t appear to touch. One loop brightening (pressure pulse) usually doesn’t affect its neighbors geometrically. Sorry not to have any good examples readily at hand.

8. Imperturbability on a large scale The same principle applies - often the distant corona ignores what looks to us like a titanic explosion. Excellent example from June 6-7, 2000 (see APOD).

9. A beautiful coronal cusp resulting from a flare/CME on June 6, 2000

10. The GOES time history for June 6-7, 2000

11. Before… After

12. 500 DN 100 DN 15:36:23 minus 14:52:27 UT Remember the movie!

13. Measurement geometry Measurement results

14. Photosphere “Source Surface” Solar wind: radial field lines Corona: force-free field Minimal model for a CME: initial conditions

15. Photosphere “Source Surface” Minimal model for a CME: a flare has happened! FF Radial field

16. Minimal model of a CME A force-free coronal equilibrium interfaces to a radial field in the solar wind, initially. A flare happens and a CME opens a large new swathe of field lines. The MHD equilibrium prior should adjust to a new equilibrium state outside the CME. We don’t see this happening.

17. How “massive” is the corona? 1. Total magnetic energy = 10 34 ergs, hence a major CME is a 1% effect. 2. A major CME occupies 1 steradian hence a major CME is a 10% effect. 3. In any case there should be a local effect on the equilibrium.

18. Seemingly identical interplanetary CMEs can have very different coronal origins.

19. Impulsive flare North of equator Filament Dimming Giant arcade South of equator Filament No dimming

20. Ulysses ICME observations (Gosling et al., 1994) 12

21. Inferences The solar-wind structures resulting from a CME may have little to do with the coronal structure causing it. The energy involved is hard to trace, because the dominant term is the coronal B field, especially if it is low 

22. An exception to prove the rule: the disruption of a post-flare arcade - v. unusual

23. FFIs first...

25. Dark energy in the solar corona Apparently great perturbations can occur without disrupting the basic equilibrium of the corona. Great perturbations often do not permanently displace nearby coronal structures. Extremely different solar perturbations can cause nearly identical ICMEs. The bottom line: coronal MHD equilibrium is not easy to understand intuitively.

26. Once again, I’ve managed to give a talk, the main point of which is that I don’t understand what is going on...