1. OXYGEN ION ACCELERATION AND CONVECTION IN THE POLAR MAGNETOSPHERE B. Klecker for the CLUSTER Team at MPE G. Paschmann, B. Klecker, M. Förster, H. Vaith, J. Bogdanova, E. Georgescu, S. Haaland, P. Puhl-Quinn A. Blagau, A. Kis, H. Hasegawa, B. Sonnerup Presentation at the Fachbeirat MPE 2002 June 17 - 20, 2002

2. OUTLINE The CLUSTER Mission and Payload The Experiments EDI and CIS Ion Convection Measurements: a Tool – to study spatial and temporal variations – to study wave signatures – to derive spatial scales from time series measurements Summary

3. CLUSTER: CORNERSTONE #1 (WITH SOHO) OF ESA‘S SCIENTIFIC PROGRAM AND PART OF ISTP

4. CLUSTER ORBIT IN FEBRUARY 2001

5. CLUSTER SEPARATION STRATEGY

6. CLUSTER INSTRUMENTATION

7. CLUSTER OPERATION

8. THE ELECTRON DRIFT INSTRUMENT (EDI) Scientific Objectives Measurement of the ambient electric field by a novel technique developed over the last 20 years: Emission and subsequent detection of tracer electrons by two sets of electron gun / detector units, positioned at 180° to each other.

9. THE ELECTRON DRIFT INSTRUMENT (EDI) For any combination of magnetic field B and drift velocity V, only a single electron trajectory exists that connects each electron gun with the detector located on the opposite side of the S/C. Technique: Emission of an electron beam of 1 keV perpendicular to the local magnetic field. Detection of the electrons with the detector on the opposite side of the S/C. Measurement of the times-of-flight, T 1 T 2. Computation of E from the drift step d, and B d = V d T g ~ E / B 2 T 1,2 = T g (1±V d /V e ) T 1 -T 2 = 2 (d/V e ) T 1 +T 2 = 2 T g = 4  m e / e B

10. EDI: Triangulation and Time-of-Flight Technique Triangulation Technique By employing 2 beams and 2 detectors, the two unique directions can be monitored continuously and the displacement d obtained by a triangulation procedure. Time-of-Flight Technique When the magnetic field B becomes small, d ~ E/B 2 becomes very large and cannot be determined accurately any more with the triangulation technique. Then d can be determined with higher precision from the time- of-flight differences. T 1 -T 2 = 2 (d/V e )

11. EDI DATA PRODUCTS Electric field time series V  time series Time resolution: ≥100 msec, standard 1 sec Limitations: magnetic field strength, typically B > 15 nT rapid time variations in E or B signal to background ratio data from S/C-1, S/C-2, S/C-3 Note: EDI provides V  without any additional assumptions

12. THE CLUSTER ION SPECTROMETRY INSTRUMENT (CIS) Scientific Objectives / Instrument Requirements Determination of the 3D Distribution function of ions in the energy range ~ 0 (S/C-potential) to 40 keV/e with 1 spin (4 sec) time resolution. Identification of major ions in the near-Earth plasma environment, i.e. of H +, He 2+, He +, and O +. Technical solution to cover large dynamic range and to provide redundancy: 2 sensors with 2 geometry factors each (factor ~100 ) CIS-1 (CODIF) Composition and Distribution Function Analyzer On-board analysis provides H +, He 2+, He +, and O +. Ground analysis provides in addition O 2+ and O 2 + Energy range 0.020 - 40 keV/e + ~ 0 (S/C-potential) - 20 eV with RPA CIS-2 (HIA) Hot Ion Analyzer Ion energy range 0.005 - 32 keV/e

13. CIS-1: Principle of Operation

14. CIS DATA PRODUCTS ON-BOARD ANALYSIS Moments (N, V, T, P) computed onboard every spin (4 sec) from 3D distributions for H +, He 2+, He +, O + 3D Distributions of H +, He 2+, He +, O + for ≥ 1 spin -> telemetry ANALYSIS ON GROUND 3D Distributions of H +, He 2+, He +, O + with max. 1 spin resolution. Moments (N, V, T, P) computed for selectable energy ranges. Limitations:Counting statistics Data from S/C-1, S/C-3, S/C-4 Plasma Drift / Convection: V  derived from V and magnetic field B

15. PLASMA CONVECTION MEASUREMENTS Measurements with the 4 CLUSTER S/C provide a tool for the study of Spatial and temporal variations Spatial scales Wave signatures

16. OBSERVATIONS IN THE DAYSIDE POLAR CAP  SUN

17. The velocity distribution of O + shows a mono- energetic beam with systematic time dispersion. For B z < 0 the energy is systematically decreasing with increasing latitude. The convection velocity inferred from the O + velocity measurement and V  as measured directly with EDI are in remarkably good agreement. The pole-ward convection is consistent with the 2-cell convection patterns as typically observed in the ionosphere for B z < 0. Typical Signatures of O + Beams in the CUSP and Polar Cap

18. Oxygen Beams in the Cusp and Polar Cap Interpretation Localized (in latitude) source of accelerated ionospheric ions with broad energy spectrum. Velocity, V, from super- position of outward particle motion (V II ) with pole-ward convection (V   ) This results in an apparently mono-energetic beam as observed on CLUSTER

19. MULTISPACERAFT OBSERVATIONS CLUSTER CONFIGURATION ON MARCH 4, 2001

20. MULTISPACECRAFT MEASUREMENTS a) Energy-time spectrogram of O +. b) Number density of O+ on S/C 1, 3, 4. c) V || of O + on S/C 1, 3, 4. d) V  of O + on S/C 1, 3, 4. Note: For separation distances of ~ 600 km the convection velocities are essentially identical on all 3 S/C.  Check for time-lag between different S/C provides length-scale of coherence of convection.

21. CROSS - CORRELATION: CIS CIS S/C-3 - S/C-4 Cross-correlation of V  as measured with CIS with 16 s resolution. Maximum correlation is obtained for zero time lag.

22. CROSS - CORRELATION: EDI Cross-correlation of V  as measured with EDI with 1 s resolution. Maximum correlation is obtained for zero time lag.

23. SUMMARY-1 The convection velocities derived from the O + moments are in remarkable agreement with the drift velocity measured directly with the EDI experiment onboard CLUSTER. Thus, the combination of CIS and EDI measurements provide a full set of 4 S/C measurements with redundancy (2 x S/C-1, S/C-2, 2 x S/C-3, S/C-4) For separation distances of ~ 600 km the convection velocities are essentially identical on all spacecraft. This implies that the observed variations in V  are temporal in nature, i.e. due to changes in the convection pattern probably caused by substorm related activity.

24. Energy step structures of O + and H + ions in the cusp and polar cap O + distribution functions, S/C 1 At 02:25:20 the O + distribution function shows a beam-like behavior, at 02:35:40 the distribution function shows high perpendicular heating.

25. NEXT STEPS Convected O + Ions Correlate variations in convection velocity with substorm activity. Compare the O + energy dispersion with model calculations (trajectory tracing). This method can be used, together with the information on the convection velocity, to infer the altitude distribution of ion injection and acceleration (e.g. Dubouloz et al., 2001, Bouhram et al., 2002). Use the multi-spacecraft measurements to infer the latitude and longitude distribution of ion injection (for larger separation distances). Perpendicular Heating Detailed correlation with wave measurements onboard Cluster

26. CONVERSION OF TIME SERIES DATA INTO SPATIAL PROFILES AT THE MAGNETOPAUSE The 4 MP crossings provide the magnetopause orientation and velocity at discrete instances in time. Continuous sensing of the magnetopause velocity is possible with the measurement of the plasma drift velocity made with EDI and CIS. Panel 3: V N, the drift velocity along the MP normal (EDI and CIS). Integration of V N defines the distance from the MP to the S/C (Panel 4). This distance scale can then be used to convert the time series data into a spatial profile.

27. STANDIG ULF WAVES IN THE POLAR REGION Phase shift between  B and  V = 90°  STANDING WAVE Positive Pointing Flux  Energy Input into Ionosphere  SUN

28. C4 C1 C3 C1 C3 C2 C4 From OVT 16 UT Tsy87, KP=3 X GSM Z GSM Ion UT 15:00 15:30 16:00 16:30 17:00 17:30 18:00 ILAT 66.20 73.00 79.90 85.80 89.50 86.30 83.70 MLT 12.40 12.50 12.70 12.90 23.40 00.40 00.80 UT 15:00 15:30 16:00 16:30 17:00 17:30 18:00 ILAT 66.80 72.70 78.80 84.30 88.80 88.10 85.10 MLT 12.40 12.50 12.60 12.70 12.80 00.90 00.90 UT 15:00 15:30 16:00 16:30 17:00 17:30 18:00 ILAT 61.80 64.90 70.70 77.40 83.50 88.40 87.70 MLT 12.20 12.30 12.40 12.40 12.30 11.00 01.80 CUSTER-CIS Day 30 - 08 - 2001 STUDY OF TIME VARIATIONS

29. Cluster C3 Ion 15:00 15:30 16:00 16:30 17:00 17:30 18:00 Time UT (HH:MM) IMF SuperDarn C3 Geotail + 10mn Vc CIS 12 MHD

30. Cluster C3 Ion 15:00 15:30 16:00 16:30 17:00 17:30 18:00 Time UT (HH:MM) IMF Geotail + 10min SuperDarn MHD C3 12

31. Summary-2 Double cusp observed when IMF turned from South to North and dominant IMF-By negative. Second cusp observed on CLUSTER-3 is the cusp for B z >0 that moved poleward. CIS and EDI measurements of plasma convection in the polar region can be used to investigate in detail changes of the convection pattern in response to solar wind conditions.

32. C3 C4,C2,C1 Start of cusp at C4,C2,C1 SuperDarn MHD simulation C4 12

33. Cluster C3 Ion 15:00 15:30 16:00 16:30 17:00 17:30 18:00 Time UT (HH:MM) IMF C3 Geotail + 10min SuperDarn 12 MHD

34. Cluster C3 Ion 15:00 15:30 16:00 16:30 17:00 17:30 18:00 Time UT (HH:MM) IMF C3 Geotail + 10min SuperDarn MHD 12

35. OBSERVATIONS The dayside cusp region of the Earth‘s magnetosphere is known as a major source of ionospheric ions (e.g. Lockwood et al., 1985). The study of these ions provides information on energization processes (e.g. transverse ion heating by electrostatic, electromagnetic waves, parallel acceleration by DC electric fields)

36. DMSP-F15 16:12 UT DMSP-F15 17:52 UT 15:30 16:18 16:48

37. Sketch of cusp motion Bz<0, By<0 Cluster 3 Cusp Cleft/LLBL Bz>0, By<0

38. ONOING STUDIES Cusp: Magnetopause Tail

39. Energy step structures of O + and H + ions in the cusp and polar cap, Ions transverse heating mechanisms The heating can be associated with broadband extra low frequency (BBELF) wave fields,waves near the lower hybrid (LH) frequency, or electromagnetic ion cyclotron (EMIC) waves near 0.5 f H+. The heating can also be correlated with auroral electrons, suprathermal electron burst (STEBs), or precipitating H + ions. Furthermore, types 1 and 2 are often associated with field- aligned currents.