1. Morphology of Inner Magnetospheric low-energy ions M. Yamauchi, et al. Swedish Institute of Space Physics (IRF), Kiruna

2. Ion drift under strong B-field (e.g. inner magnetosphere) Magnetic drift (Energy dependent) * gradient-B drift * curvature drift ⇒ dominant for > 10 keV ExB drift (Energy independent) * co-roration E-field * external E-field ⇒ dominant for < 0.1 keV

3. Ion drift Energy dependent for magnetic drift and Energy independent for ExB drift/corotation external E-field

4. Ion drift Westward drift for high energy/evening and Eastward drift for low-energy/morning

5. Ion drift Variation in the source and E-field makes the ion population a zoo of various patterns

6. Characteristic of Cluster Perigee * North-South symmetric * Quick scan of all latitude

8. The examined ion signatures (1) (b) Wedge-like energy-latitude dispersed ions at sub-keV range: predominantly found in the morning sector some hours after a substorm. The source population is much colder than the plasma sheet. (both symmetric/asymmetric) (e) Internal asymmetry of (b)

9. (c) Vertical stripes: similar to the wedge-like structure but dispersion is weak (nearly vertical in the spectrogram). The energy extends from the about 10 keV to sub-keV. (both symmetric/asymmetric) The examined ion signatures (2)

10. The examined ion signatures (3) (d) Short bursts of low-energy ions isolated from the above structures: a peak energy flux less than 100 eV but not thermal. (both symmetric/asymmetric)

11. The examined ion signatures (4) (f) Warm trapped ions confined near equator: ~ tens eV to a few hundred eV.

12. (b) Wedge-like energy-latitude dispersed ions at sub-keV range: predominantly found in the morning sector some hours after a substorm. The source population is much colder than the plasma sheet. (c) Vertical stripes: similar to the wedge-like structure but dispersion is weak (nearly vertical in the spectrogram). The energy extends from the about 10 keV to sub-keV. (d) Short bursts of low-energy ions isolated from the above structures: a peak energy flux less than 100 eV but not thermal. (e) Internal asymmetry of (b) (f) Warm trapped ions confined near equator: tens eV to a few hundred eV. The examined ion signatures (1)-(4)

14. Characteristic of Cluster Perigee * North-South symmetric * Quick scan of all latitude + north-south symmetric nature of trapped ions (due to bouncing)  Distribution must be north-south symmetric

15. Where? Inner Magnetosphere at 4~6 R E (Cluster perigee) Species? H + of 10 eV ~ 10 keV (CIS/CODIF energy range) Distribution? Intense ion population (except plasma sheet) In this work: (a) Statistics distribution, (b) 1-2 hour scale evolution/decay (using inbound-outbound asymmetry), (c) relation to substorms (using elapsed time from high AE), (d) modeling (using Ebihara’s simulation code). We examined all SC-4 perigee pass during 2001-2006 (about 670 traversals, with relatively clean data of 460 traversals). Analyses

16. Before analyses, we have to examine possible “biases” such as Instrument Degradation or Solar Cycle phase Database quality check  We examine both “inbound-outbound” symmetric & asymmetric cases

17. Decrease of “wedge-like” is not due to solar cycle ! Occurrence of substorm is rather constant 

18. The same for “low-energy burst” Occurrence of substorm is rather constant 

19. But “vertical stripes” show some solar cycle effect

20. Rather, the decrease is due to instrumental effect  Rapid degradation of the sensor Occurrence of substorm is rather constant 

21. Impossible to take statistics during 2003-2004 because of radiation dose. Otherwise large decrease. How about warmed trapped ions?  Rapid degradation of the sensor Occurrence of substorm is rather constant 

22. (1) Both 2001-2003 & 2004-2006 show morning peak  We can safely use 2001-2006 data together. (2) Very high observation frequency in the morning (> 80%) Next check: Is Local Time distribution affected by this bias?

24. Local Time distribution symmetric + asymmetric enhanced within traversal Wedge-like: high-occurrence (morning) peak is not midnight enhance > symmetric > decay Vertical stripe: midnight phenomena enhance (midnight) decay ~ enhance (other LT) Low-energy burst: all local time enhance ~ decay  time scale ~ 1 hour enhance/decay  factor 3 change

25. Is enhancement related to substorm? AL AU AL AU

26. eastward drift Viking 14 MLT poleward 6 MLT 9 MLT 12 MLT 15 MLT 18 MLT For the wedge-like dispersion, the relation to substorm has already been studied: After AE>400 nT activity, (1) Moves eastward (2) Decay in time hr from substorm cf. Viking

27. Relation to AE activities Local Time distribution * Strong preference during |AL|>300 nT activity * Outstanding at midnight  Related to substorm-related injction * Optimum at 300 nT threshold (cf. 200, 400 nT) Vertical stripes

28. Relation to AE activities Local Time distribution * Same result as Viking (morning~0h, afternoon>5h) * Less enhancement with elapsed time  stagnation * Yet, enhancements after 5h & aftrnoon  ??? Wedge-like dispersion

29. Relation to AE activities Local Time distribution * slight decrease of “change” with time * but  stagnation Low-energy burst

30. The inner magnetospheric low-energy ion populations (1)-(3) below show significant changes within 1-2 hours. (1) Wedge-like energy-latitude dispersed ions (< a few keV), (2) Vertical stripes (< 10 keV), (3) Short-lived low-energy ion burst (< few hundred eV). For all three patterns, asymmetric cases (large inbound- outbound difference) are found more often than symmetric cases at almost all LT. For vertical stripes, majority of local midnight pass show large inbound-outbound difference when AL<300 nT. For low-energy burst, the lifetime is estimated as short as 1 hour Summary 1

31. Where? Inner Magnetosphere at 4~6 R E (Cluster perigee) Species? H + of 10 eV ~ 10 keV (CIS/CODIF energy range) Distribution? Intense ion population (except plasma sheet) In this work: (a) Statistics distribution, (b) 1-2 hour scale evolution/decay (using inbound-outbound asymmetry), (c) relation to substorms (using elapsed time from high AE), (d) modeling (using Ebihara’s simulation code). We examined all SC-4 perigee pass during 2001-2006 (about 670 traversals, with relatively clean data of 460 traversals). Next

32. Relation to AE activities Local Time distribution * Same result as Viking (morning~0h, afternoon>5h) * Less enhancement with elapsed time  stagnation * Yet, enhancements after 5h & aftrnoon  ??? Wedge-like dispersion

33. Why inbound-outbound difference of “wedge” at Noon-Afternoon sector so often? ⇒ We examine using numerical simulation (Ebihara’s code)

34. The ion drift alone can re-produce significant inbound-outbound difference ! 0.1 keV t ≈ 15 hr

35. Another example: sub-keV (dispersion asymmetry) and a few keV (ion band) 0.1 keV t ≈ 6 hr t ≈ 4 hr

36. The significant changes of the “ Wedge-like dispersed sub-keV ions within only 1-2 hours can be explained by the drift motion even in the noon-afternoon sector. But some signatures are yet naturally explained by the local inflow from ionosphere, that also has short time scale. For both sources, the ion energy is very low (< 0.1 keV) but not cold. Summary 2

37. Future work: * Mass dependence * Pitch-angle dependence

38. note: // >> ⊥ does not necessarily mean ionospheric source but mirroring ions

39. Next

40. equator Confined near equator = Only  direction spin axis 1 2 4 5 7 8 SC motion sectors ≈ PA E(H + ) << E(He + ) : new

41. equator All Local time All AE conditions Energy-time dispersion = new Appearing in 40 min = new! statistics & dynamics

42. Summary 3 We also studied the “equatorially-trapped warm ions” which are basically symmetric between inbound and outbound The energy of He + is often higher than that for H +. Some events show a non-thermal ring distribution rather than superthermal pancake distribution. Some events show energy-time dispersion, indicating drifts from different local times. The time scale of the development is again about 1 hour. At about 4-4.5 R E, the observation probability is about 1/3 (night-dawn) to 1/2 (noon-dusk). The He + /H + ratio is variable and is much less than 5% for the majority of the cases.

43. Future work: (2) (n+(1/2))f ce wave is accompanied * relation to wave

44. Future work: * relation to wave * compare different SC