1. steve.milan@ion.le.ac.uk >> European Cluster Assimilation Technology

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3. steve.milan@ion.le.ac.uk >> The Cluster Active Archive ESA initiative to store in perpetuity all Cluster data Efforts are made to ensure the data are “final” Extensive validation and cross-calibration effort Online data portal, including quick-look plots Continuously growing user-base and download history

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6. steve.milan@ion.le.ac.uk >> The role of ECLAT ECLAT provides context for the Cluster observations How do Cluster observations relate to other observations of the magnetosphere, made from the ground or other space-borne observatories? The Cluster Ground-based Working Group has provided contextual information for the duration of the Cluster mission to date on an ad hoc basis This will be formalized, improved, and combined with a data-serving functionality within ECLAT

7. steve.milan@ion.le.ac.uk >> Who is involved? University of Leicester, UK Steve Milan (coordinator), Mark Lester Oesterreichische Akademie der Wissenschaften, Austria Rumi Nakamura Finnish Meteorological Institute, Finland Kirsti Kauristie, Minna Palmroth Institutet för rymdfysik, Sweden Hermann Opgenoorth St. Petersburg State University, Russia Victor Sergeev European Commission Stefano D’Orilia European Space Agency Matt Taylor, Harri Laakso, Arnaud Masson

8. steve.milan@ion.le.ac.uk >> What is needed? 1) A knowledge of the magnetospheric regions and boundaries Cluster is encountering Region and boundary identification (OEAW) 2) An ability to know where Cluster is relative to other observatories in space or on the ground Magnetic field tracing (SPSU)

9. steve.milan@ion.le.ac.uk >> What is needed? 3) The ionospheric conditions at the mapped footprint of the Cluster spacecraft Miracle equivalent current mapping (FMI) 4) Knowledge of the large-scale magnetospheric state and behaviour SuperDARN ionospheric flow patterns and global auroral imagery (ULEIC)

10. steve.milan@ion.le.ac.uk >> What is needed? 5) Physics-based modelling of the magnetosphere as context and as re-analysis GUMICs long runs and re-analysis development (FMI) 6) Archive validation, science exploitation, and out-reach Science and validation workshops, networking with science community, public out-reach (IRF)

11. steve.milan@ion.le.ac.uk >> Validation; exploitation; out-reach

12. steve.milan@ion.le.ac.uk >> OEAW FMI / SPSU ULEIC FMI IRF ULEIC

13. steve.milan@ion.le.ac.uk >> Jan 20 2010

14. steve.milan@ion.le.ac.uk >> SuperDARN IMAGE

15. steve.milan@ion.le.ac.uk >> Common grid for SuperDARN and IMAGE data products Grid resolution? current plan: 2°  2° capacity for 1°  1°?

16. steve.milan@ion.le.ac.uk >> IMAGE Mission lasted from mid-2000 to mid-2005 3 cameras: WIC, SI12, SI13 Cadence: 123 s Northern hemisphere: 2000 to 2002 Southern hemisphere: 2004 to 2005

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19. steve.milan@ion.le.ac.uk >> IMAGE – other issues Additional parameters? Oval radius Overall brightness Open flux Feature recognition?

20. steve.milan@ion.le.ac.uk >> SuperDARN Data available for whole Cluster mission duration Cadence: 120 s Both northern and southern hemisphere – northern hemisphere of better quality + An increasing number of radars as the mission progresses - Less backscatter during solar minimum Main data product is electrostatic potential pattern – electric field / drift velocity Provide electrostatic potential on grid Also provide spherical harmonic coefficients for high resolution work and derivation of electric fields and drift velocities

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25. steve.milan@ion.le.ac.uk >> Software IDL software package Provide basic routines for reading and visualizing the IMAGE and SuperDARN and auxiliary data products Allow combined plotting The software will include a GUI front-end which will call these routines

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27. Highlights of the new modeling project 1.A completely overhauled and vastly expanded space magnetometer database: (i) Four Themis probes (2007-2011), (ii) Cluster (2004-2010), (iii), GOES-8,...,-12 (1995-2010), (iv) Polar (1994-2007), (v) Geotail (1995-2010) Sample coverage by GOES 12, Imp-8, Polar, Geotail, and Cluster: POLAR (red) GOES-12 (yellow) Cluster (magenta) Geotail (blue) IMP 8 (black)

28. Themis A, B, C, D, and E

29. Highlights of the new modeling project (cont.) 2.A new magnetopause model: a tilt-dependent data-based boundary by Lin et al. [JGRA, 2010] with an improved shape near cusps, driven by interplanetary parameters.

30. ECLAT, FMI March 24,2011 Example of Modeling Results (Kubyshkina et al., JGR 2011, Themis special issue) AM03 T96 MLT=22.5; first line 65.5 (11 lines with 0.5 o latitude step) Different spacecraft – magnetic field relative position, mapping to lower latitudes  05:00 UT pre-substorm  05:14 UT stretching/TCS  05:24 UT TCS disruption Substorm growth/expansion phase  Large difference with standard model – importance of adaptive modeling  SC footprints differ by -2 o CGLat during GP and by +2 o during expansion; overall variation ~4 o resembles typical auroral keogram.  Strong stretching/TCS catched in AM03  Coverage is essential to catch both TCS tilt and TCS growth Advanced Adaptive Modeling only has a sense for special events

31. Isotropy boundaries: a tool for probing magnetospheric configuration and error estimation Adiabaticity if R c /ρ>>1, empty loss cone Loss of adidbaticity if (G=B∙ρ)  isotropy loss cone precipitation from nightside current sheet Controlled by equatorial B-field (mostly Bz), but observed near the ionosphere  a tool to sense remotely configuration and to control the mapping Previous work: scattering threshold (…), correlation between IBLatitude and MF stretching (…), EQ boundary of proton precipitation/aurora (…) ; first attempts to use the IBs for remote sensing and mapping error control Problems : compete with wave-induced precipitation (important during strong activity) Polar-orb. spacecraft, h~800 км || ┴ B

32. steve.milan@ion.le.ac.uk >> Magnetotail magnetic flux estimate based on simultaneous solar wind and magnetotail observations Petrinec & Russell,1996; Shukhtina et al. 2004, 2009 … Assumptions: 1. P ressure balance -at magnetopause 0.88Pd sin 2  + B SW 2 /2  0 +nk(T isw + T e sw ) = B L 2 /2  0 - i n the magnetotail : B 2 /2  0 +nkT  B L 2 /2  0 ( valid tailward of ~15 Re, tail approximation) 2. Presumed magnetopause shape: sin 2  = A 2 exp (-0.0714 X) and B L isolines shape  RT  FT = BL *  RT 2 MagnetoTail magnetic Flux MTF – a Global State Parameter 3. Other assumptions : circular tail cross-section, zero dipole tilt, B(x)=BL (no PS),.. Large Pd jumps are dangerous  2RT

33. steve.milan@ion.le.ac.uk >> MTF comparison with PC magnetic flux from global auroral images (Shukhtina et al.,2010) Fe: UVI LBHL from Polar, and FUV (WIC) from IMAGE spacecraft ( DeJong et al., 2007 ). Fp: FUV(SI12) from the IMAGE ( Hubert et al., 2006 ). Fp FeFpFe MTF - Optical methods are not absolute - MTF T > Fp, Fe (provides overestimated full (open+closed) MTFlux value,  ~0.2 GW) - F T correlation with Fp worse, than with Fe (more disturbed Fp periods) Comparative investigation to be continued in ECLAT the ultimate goal - provide the Global State Parameter for Magnetosphere

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35. steve.milan@ion.le.ac.uk >> ECLAT Boundary identifications Contextual data Space-/ground-based comparisons Statistical studies Workshops