Reconnection: Geometry and Dynamics

1. Reconnection: Geometry and Dynamics A. Bhattacharjee, N. Bessho, J. Dorelli, S. Hu, J. M. Greene, Z. W. Ma, C. S. Ng, and P. Zhu Space Science Center Institute for the Study of Earth, Oceans, and Space University of New Hampshire Isaac Newton Institute, Cambridge University, August 19, 2004

2. Geometry of 3D Reconnection • Brief review of 2D and 2.5D models: “anti-parallel” and “component” reconnection. Applicable to toroidal devices with closed field lines. • 3D reconnection in the presence of magnetic nulls. Applicable to the Earth’s magnetosphere. • 3D reconnection without nulls or closed field lines. Applicable to Parker’s model of the solar corona.

3. Resistive Tearing Modes in 2D/2.5D Geometry Equilibrium magnetic field assumed to be either infinite or periodic along z x Neutral line at y=0 y Time Scales Lundquist Number Tearing modes (Furth, Killeen and Rosenbluth, 1963)

4. Collisionless Tearing Modes at the Magnetopause (Quest and Coroniti, 1981) • Electron inertia, rather than resistivity, provided the mechanism for breaking field lines, but the magnetic geometry is still 2D/2.5D. • Growth rates calculated for “anti-parallel” ( ) and “component” ( ) tearing. It was shown that growth rates for “anti-parallel” merging were significantly higher. • Model provided theoretical support for global models in which global merging lines were envisioned to be the locus of points where the reconnecting magnetic fields were locally “anti-parallel” (e.g. Crooker, 1979)

5. Magnetic nulls in 3D: Building blocks for separatrices Spine Fan (Lau and Finn, 1990)

6. Towards a fully 3D model of reconnection • Greene (1988) and Lau and Finn (1990): in 3D, a topological configuration of great interest is one that has magnetic nulls with loops composed of field lines connecting the nulls. • The null-null lines are called separators, and the “spines” and “fans” associated with them are the global 3D separatrices where reconnection occurs (cf. Priest and Forbes, 2000). • For the magnetosphere, the geometrical content of these ideas were implicit in the vacuum superposition models of Dungey (1963), Cowley (1973), Stern (1973). However, the vacuum model carries no current, and hence has no spontaneous tearing instability. The real magnetopause carries current, and is amenable to the tearing instability.

7. Dungey’s Model for Southward and Northward IMF

8. Equilbrium B-field

9. Perturbed B-lines produced by the Spherical Tearing mode

10. Equilibrium Perturbed Field lines penetrating the spherical tearing surface

11. Equilbrium Current Density, J

13. Features of the spherical tearing mode • The mode growth rate is faster than classical 2D tearing modes, scales as S-1/4 (determined numerically from compressible resistive MHD equations). • Perturbed configuration has three classes of field lines: closed, external, and open (penetrates into the surface from the outside). • Tearing eigenfunction has global support along the separatrix surface, not necessarily localized at the nulls. • The separatrix is global, and connects the cusp regions. Reconnection along the separatrix is spatially inhomogeneous. Provides a new framework for analysis of satellite and ground-based observations at the dayside magnetopause.

14. Solar corona astron.berkeley.edu/~jrg/ ay202/img1731.gif www.geophys.washington.edu/ Space/gifs/yokohflscl.gif

15. Solar corona: heating problem photosphere corona Temperature Density Time scale Magnetic fields (~100G) --- role in heating? ~ ~  Alfvén wave  current sheets

16. Parker's Model (1972) Straighten a curved magnetic loop Photosphere

17. Parker’s original model has been questioned • van Ballegooijen (1985) • Zweibel and Li (1987) • Longcope and Strauss (1994) • Cowley, Longcope, and Sudan (1997) Did all these papers, which are technically correct (given their assumptions), consider current sheets of sufficiently complex topology?

18. Reduced MHD equations low  limit of MHD

19. Magnetostatic equilibrium (current density fixed on a field line) c. f. 2D Euler equation A, J, zt Existence theorem: If is smooth initially, it is so for all Time. However, Parker problem is not an initial value problem, but a two-point boundary value problem.

20. Footpoint Mapping Identity mapping: e. g. uniform field For a given smooth footpoint mapping, does more than one smooth equilibrium exist?

21. A theorem onParker's model For any given footpoint mapping connected with the identity mapping, there is at most one smooth equilibrium. Caveat :A proof for reduced MHD, periodic boundary condition in x (Ng & Bhattacharjee,1998) Remark: Aly(2004) has shown recently, using the full resistive MHD equations, that the identity mapping has only one smooth solution.

22. Implications of our theorem An unstable but smooth equilibrium cannot relax to a second smooth equilibrium, hence must have current sheets.

23. Reconnection without nulls or closed field lines Formation of a true singularity (current sheet) thwarted by the presence of dissipation and reconnection. Classical reconnection geometries involve: (i) closed field lines in toroidal devices (ii) magnetic nulls in 3D • Parker’s model is interesting because it fall under • neither class (i) or (ii). Questions: • Where do singularities form? What are the geometric • properties of singularity sites and reconnection? Are these • Quasi-Separatrix Layers (QSL’s)? How do we characterize • mathematically such singularities globally? • Need more analysis and high-resolution simulations.

24. In 3-D torii (such as stellarators), current singularities are present where field lines close on themselves • Solutions to the quasineutrality equation, • General solution has two classes of singular currents at rational surface [i(ymn) = n/m] (Cary and Kotschenreuther, 1985; Hegna and Bhattacharjee, 1989). • Resonant Pfirsch-Schluter current • Current sheet

25. Impulsive Reconnection: The Trigger Problem Dynamics exhibits an impulsiveness, that is, a sudden change in the time-derivative of the reconnection rate. The magnetic configuration evolves slowly for a long period of time, only to undergo a sudden dynamical change over a much shorter period of time. Dynamics is characterized by the formation of near-singular current sheets in finite time. Examples Sawtooth oscillations in tokamaks and RFPs Magnetospheric substorms Impulsive solar and stellar flares

26. Magnetospheric Substorms

28. Current Disruption in the Near-Earth Magnetotail (Ohtani et al., 1992)

34. J y y

35. Observations (Ohtani et al. 1992) Hall MHD Simulation Cluster observations: Mouikis et al., 2004

37. Ux Uz Highly Compressible Ballooning Mode in Magnetotail (Voigt model) x = -1 to -16 RE z = -3 to 3 RE ky= 25*2 e = 126 growth rate:0.2 t=5.8 t=29

38. ky and Dependence

39. Possible Scenario of Substorm Onset:Near-Earth Ballooning Instability Induced by Current Sheet Thinning and/or Reconnection

40. The start of large magnetic fluctuations and the modulation of energetic ion fluxes observed in Earth's magnetotail plasma sheet coincides with the onset of an isolated substorm.Note the impulsive relaxation of the radial pressure gradient signified by the sudden reduction of the differences between the duskward (90) and dawnward (270) fluxes -- consistent with the feature of ballooning instabilities.[L.-J. Chen, et al., 2003]

41. Power spectrograms of the magnetic field show impulsive enhancement of the wave power in the ballooning frequency range.The enhancement is broadband, bursty, and simultaneous with the impulsive pressure gradient reduction.[L.-J. Chen, et al., 2003]

42. Simulations of Parker's model

43. - + Simulations of Parker's model bottom middle top

44. - + Simulations of Parker's model bottom middle top

45. Simulations of Parker's model

46. More general topology Parker's optical analogy (1990)

47. Main current sheet