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Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,

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Presentation on theme: "Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,"— Presentation transcript:

1 Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS, Cluster/CIS, Image/FUV teams

2 Magnetic Reconnection Cambridge, Aug., 2004 2 Outline Reconnection: When, Where and Why Where: The Cusp for Northward IMF - Anti-parallel Reconnection - Component Reconnection Where: The Cusp for Southward IMF - Component Reconnection - Anti-parallel Reconnection Summary

3 Magnetic Reconnection Cambridge, Aug., 2004 3 Magnetic Reconnection When does reconnection occur – “all the time” (i.e., it is a “quasi-steady” process) –We have poor knowledge of the changes in the reconnection rate Where does reconnection occur – recent observations appear to favor anti-parallel reconnection but some previous observations suggest component reconnection –Work in progress……. Stay tuned! Why does reconnection occur – DON’T KNOW! –The answer appears to be in the electron diffusion region –Future mission (e.g., MMS) will have the time resolution and instrumentation to fully investigate this region

4 Magnetic Reconnection Cambridge, Aug., 2004 4 Magnetic Reconnection Near the Earth: Field Line Topologies (for Southward IMF) Blue - Solar Wind Field Lines Green - Closed Field Lines Red - Open Field Lines Focus on “dayside” reconnection Magnetopause Current Sheet

5 Magnetic Reconnection Cambridge, Aug., 2004 5 Observe Reconnection In Two Locations Cusp: “foot” of the reconnected field lines Does reconnection stop? Where does reconnection occur? Magnetopause: “up close and personal” What is the reconnection rate? Where does reconnection occur? Each location has its advantages and disadvantages

6 When is Magnetic Reconnection Occurring?

7 Magnetic Reconnection Cambridge, Aug., 2004 7 WHEN Cusp Ion Energy Dispersion for Southward IMF

8 Magnetic Reconnection Cambridge, Aug., 2004 8  MLT = 3h  UT = 5h Trattner et al. [2002] WHEN: Low- and High Altitude Cusp Observations

9 Magnetic Reconnection Cambridge, Aug., 2004 9 Direct Confirmation of Images of the Foot of a Reconnecting Field Line Images of the footpoint from the IMAGE spacecraft Simultaneous observations at the reconnection site from the Cluster spacecraft (bi-directional ion flows) Magnetic field mapping confirms the location of the ionospheric “spot” Observations Mapping

10 Magnetic Reconnection Cambridge, Aug., 2004 10 Does Reconnection Stop? You Decide…..

11 Magnetic Reconnection Cambridge, Aug., 2004 11 IMF Rotation from North to South: Observations and Predictions Although there is a delay, in general, there is a simple change in the location of the reconnection site

12 Magnetic Reconnection Cambridge, Aug., 2004 12 IMF Rotation from South to North: Observations and Predictions Similar for south to north transition – a delay but reconnection does not stop, even when conditions change

13 Where is Magnetic Reconnection Occurring?

14 Magnetic Reconnection Cambridge, Aug., 2004 14 “WHERE is reconnection occurring?” boils down to two models….

15 Magnetic Reconnection Cambridge, Aug., 2004 15 Remote Sensing the High Latitude Reconnection Site Magnetopause Sunward Convection Produces Two Effects: Auroral “Spot” in the Ionosphere Velocity Dispersion in the Cusp IMAGE spacecraft

16 Magnetic Reconnection Cambridge, Aug., 2004 16 Proton aurora images from IMAGE/FUV taken just before and after the arrival of an interplanetary disturbance in the ionosphere. Fuselier et al. [2002]

17 Magnetic Reconnection Cambridge, Aug., 2004 17 Mapping cusp foot points along geomagnetic field lines into the magnetosphere (Fuselier et al. [1994]).

18 Magnetic Reconnection Cambridge, Aug., 2004 18 Comparison of the location of field lines mapped from the cusp foot points with the location of anti-parallel reconnection sites.

19 Magnetic Reconnection Cambridge, Aug., 2004 19 The Location of the Reconnection Line for Northward IMF Polar/TIMAS Cusp Crossings 240 Cusp Events for Northward IMF. 81 events analyzed. Calculate the Distance to the X-Line. Mapping the Distance along the Geomagnetic Field.

20 Magnetic Reconnection Cambridge, Aug., 2004 20 Cusp Ion Energy Dispersion for Northward IMF

21 Magnetic Reconnection Cambridge, Aug., 2004 21 Ion Dispersion in the Cusp: Distance to the Reconnection Site Assumes: “Instantaneous” Acceleration Simple Field Line Structure

22 Magnetic Reconnection Cambridge, Aug., 2004 22 Xr/Xm = 2Ve/(Vm-Ve) Onsager et al. [1990] Fuselier et al. [2000]

23 Magnetic Reconnection Cambridge, Aug., 2004 23 The Location of the Reconnection Line for Northward IMF Event 1: Sept. 22, 1997

24 Magnetic Reconnection Cambridge, Aug., 2004 24 Time (UT) Convection time to the MP: 22min

25 Magnetic Reconnection Cambridge, Aug., 2004 25

26 Magnetic Reconnection Cambridge, Aug., 2004 26

27 Magnetic Reconnection Cambridge, Aug., 2004 27

28 Magnetic Reconnection Cambridge, Aug., 2004 28 Tsyganenko [1996] together with Cooling [2001] IMF draping model

29 Magnetic Reconnection Cambridge, Aug., 2004 29 The Location of the Reconnection Line for Northward IMF Event 2: Oct. 30, 1997

30 Magnetic Reconnection Cambridge, Aug., 2004 30

31 Magnetic Reconnection Cambridge, Aug., 2004 31

32 Magnetic Reconnection Cambridge, Aug., 2004 32

33 Magnetic Reconnection Cambridge, Aug., 2004 33

34 Magnetic Reconnection Cambridge, Aug., 2004 34 -Bx, +By+Bx, +By-Bx, -By+Bx, -By Antiparallel Reconnection 29 events 9 events 1200-1430 MLT 15 events 0900-1200 MLT 5 events 1000-1140 MLT Component Reconnection 23 events 3 events 0830-1030 MLT 2 events 0930-1130 MLT 2 events 1700-1730 MLT 16 events 1700-1730 MLT 81 events analysed 67 events with useable 3D cutoffs 29 antiparallel, 23 component, 15 >>Bx

35 Magnetic Reconnection Cambridge, Aug., 2004 35 Southward IMF: Anti-Parallel and Component Reconnection Can we determine the distance THAT accurately? View from the Sun

36 Magnetic Reconnection Cambridge, Aug., 2004 36 Precipitation is Different for the Two Types of Reconnection Anti-Parallel Tilted Line The Key Difference is The Flux Near Noon

37 Magnetic Reconnection Cambridge, Aug., 2004 37 Fuselier et al. [2002]

38 Magnetic Reconnection Cambridge, Aug., 2004 38

39 Magnetic Reconnection Cambridge, Aug., 2004 39

40 Magnetic Reconnection Cambridge, Aug., 2004 40 Example: “Double Cusp” Interval – Component or Anti-Parallel? Trattner et al. (2003) showed these are spatial features (energy-time(latitude) dispersion indicative of reconnection) Compute the distance to the reconnection site for the two dispersions and see if they are different First dispersion Second dispersion

41 Magnetic Reconnection Cambridge, Aug., 2004 41

42 Magnetic Reconnection Cambridge, Aug., 2004 42 Two Different Distances for the Two Dispersions View from the Sun First Dispersion Second Dispersion The second dispersion occurred closer to the spacecraft than the first dispersion Compare these distances to predictions from anti- Parallel reconnection (One distance for each measured distribution function) Cluster

43 Magnetic Reconnection Cambridge, Aug., 2004 43 How Do the Distances Compare with Anti-Parallel Reconnection? Second Dispersion First Dispersion “Red” = Anti-Parallel Reconnection Doesn’t compare Exactly with Anti- Parallel Reconnection Get Some Help With the Interpretation….

44 Magnetic Reconnection Cambridge, Aug., 2004 44 The Cusp Images Tell the Difference Looks more like anti- parallel reconnection but with a shift relative to local noon Observations Anti-Parallel Tilted Neutral Line

45 Magnetic Reconnection Cambridge, Aug., 2004 45 Conclusion: Anti-Parallel Reconnection (with a Local Noon Shift) Second Dispersion First Dispersion The pure T96 model does not show how the northern hemisphere reconnection line is shifted ~1/2 hour pre-noon However, the cusp images do!

46 Magnetic Reconnection Cambridge, Aug., 2004 46 Summary NORTHWARD IMF: Image/FUV and Polar/TIMAS observations reveal that both reconnection scenarios occur simultaneously. SOUTHWARD IMF: Both reconnection scenarios observed. Unclear what triggers one or the other.

47 Magnetic Reconnection Cambridge, Aug., 2004 47 WHEN: Multiple Cusps

48 Magnetic Reconnection Cambridge, Aug., 2004 48 Anti-Parallel Reconnection for Northward IMF antiparallel reconnection sites Z magnetosheath field cusps Y View of the Dayside magnetopause from the Sun Magnetopause Earth's Magnetic Field in the Magnetosphere Solar Wind Magnetic Field Solar Wind Northward IMF

49 Magnetic Reconnection Cambridge, Aug., 2004 49 Northward IMF Poleward Reconnection SiteEquatorward Reconnection Site Observations in the cusp have indicated the possibility of component reconnection for northward IMF (e.g., Onsager and Fuselier, 1994; Chandler et al., 1999; Fuselier et al., 2000)

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