1. II. MAGNETOHYDRODYNAMICS (Space Climate School, Lapland, March, 2009) Eric Priest (St Andrews)

2. CONTENTS 1.Introduction 2.Flux Tubes 3. MHD Equations 4. Induction Equation 5.Equation of Motion 6.Solar MHD 7.2D magnetic reconnection 8.3D reconnection Conclusions

3. 1. INTRODUCTION -- exerts a force (creates structure) -- provides insulation -- stores energy (released in CME or flare) Magnetic Field Effects:

4. Magnetohydrodynamics  MHD - the study of the interaction between a magnetic field and a plasma, treated as a continuous medium  Chromosphere  Corona  This assumption of a continuous medium is valid for length-scales

5. 2. FLUX TUBES Magnetic Field Line -- Curve w. tangent in direction of B. or in 3D:In 2D: *_ _ _ _ _ _* Equation:

6. Magnetic Flux Tube Surface generated by set of field lines intersecting simple closed curve. (i)Strength (F) -- magnetic flux crossing a section i.e., *_ _ _ _ __ _ _ _ * (ii) But---> F is constant along tube (iii) If cross-section is small, * _ _ _ _ _ _ _ *

7. Eqns of Magnetohydrodynamics Model interaction of B and plasma (cont s medium)

8. 3. FUNDAMENTAL EQUATIONS of MHD  Unification of Eqns of: (i) Maxwell

9. (ii) Fluid Mechanics or (D / Dt)

10. In MHD  1. Assume v Neglect *_ _ _ *  2. Extra E on plasma moving *_ _ _ _*  3. Add magnetic force *_ _ _ _*  Eliminate E and j: take curl (2), use (1) for j

11. 4. INDUCTION EQUATION *

12. Induction Equation N.B.: (i) --> B if v is known (ii) In MHD, v and B are * *: induction eqn + eqn of motion --> basic physics (iii) are secondary variables primary variables (iv) B changes due to transport + diffusion

13. Induction Equation ABAB (v) -- * * eg, L 0 = 10 5 m, v 0 = 10 3 m/s --> R m = 10 8 (vi) A >> B in most of Universe --> B moves with plasma -- keeps its energy Except SINGULARITIES -- j & B large Form at NULL POINTS, B = 0 --> reconnection magnetic Reynolds number

14. (a) If R m << 1  The induction equation reduces to  B is governed by a diffusion equation --> field variations on a scale L 0 diffuse away on time * * with speed

15. (b) If R m >> 1 The induction equation reduces to and Ohm's law --> Magnetic field is “**”frozen to the plasma

16. 5. EQUATION of MOTION (1) (2) (3) (4)  In most of corona, (3) dominates  Along B, (3) = 0, so (2) + (4) important

17. Magnetic force: Tension B 2 /----> force when lines curved Magnetic field lines have a Pressure B 2 /(2 )----> force from high to low B 2

18. Ex Expect physically: (check mathematically)

19. Ex (check mathematically) Expect physically:

20. Equation of Motion (1) (2) (3) (4) Plasma beta Alfvén speed * *

21. Typical Values on Sun PhotosphereChromosphereCorona N (m -3 )10 23 10 20 10 15 T (K)600010 4 10 6 B (G)5 - 10 3 10010 10 6 - 110 -1 10 -3 v A (km/s)0.05 - 101010 3 N (m -3 ) = 10 6 N (cm -3 ),B (G) = 10 4 B (tesla) = 3.5 x 10 -21 N T/B 2, v A = 2 x 10 9 B/N 1/2

22. 6. In Solar MHD We study Equilibria, Waves,Instabilities, Magnetic reconnection in dynamos, magnetoconvection, sunspots, prominences, coronal loops, solar wind, coronal mass ejections, solar flares

23. Example Shapes - Fineness -small scale of heating process + small caused by magnetic field (force-free) Structure along loops -hydrostatics/hydrodynamics (--H)

24. 7. MAGNETIC RECONNECITON  Reconnection is a fundamental process in a plasma:  Changes the topology  Converts magnetic energy to heat/K.E  Accelerates fast particles  In Sun ---> Solar flares, CME’s / heats Corona

25. In 2D takes place only at an X-Point -- Current very large --> ohmic heating -- Strong diffusion allows field-lines to break / change connectivity and diffuse through plasma

26. Reconnection can occur when X-point collapses Small current sheet width --> magnetic field diffuses outwards at speed v d = _ _ _ *

27. If magnetic field is brought in by a flow (v x = - Ux/a v y = Uy/a) then a steady balance can be set up

28. Sweet- Parker (1958) Simple current sheet - uniform inflow

29. Petschek (1964)  Sheet bifurcates - Slow shocks - most of energy  Reconnection speed v e -- any rate up to maximum

30. 8. 3D RECONNECTION Simplest B = (x, y, -2z) Spine Field Line Fan Surface (i) Structure of Null Point Many New Features 2 families of field lines through null point:

31. (ii) Global Topology of Complex Fields In 2D -- Separatrix curves In 3D -- Separatrix surfaces

32. transfers flux from one 2D region to another. In 3D, reconnection at separator transfers flux from one 3D region to another. In 2D, reconnection at X In complex fields we form the SKELETON -- set of nulls, separatrices -- from fans

33. (iii) 3D Reconnection At Null -- 3 Types of Reconnection: Can occur at a null point or in absence of null Spine reconnection Fan reconnection Separator reconnection

34. Numerical Exp t (Linton & Priest) [3D pseudo- spectral code, 256 3 modes.] Impose initial stag n -pt flow v = v A /30 R m = 5600 Isosurfaces of B 2 :

35. B-Lines for 1 Tube Colour shows locations of strong E p stronger E p Final twist

36. 9. CONCLUSIONS  Reconnection fundamental process - - 2D theory well-developed - 3D new voyage of discovery: topology reconnection regimes (+ or - null)  Coronal heating Solar flares