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3rd Swarm Science Meeting, Copenhagen, 19 May 2014

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Presentation on theme: "3rd Swarm Science Meeting, Copenhagen, 19 May 2014"— Presentation transcript:

1 3rd Swarm Science Meeting, Copenhagen, 19 May 2014
Swarm EFI Overview and Science Highlights Image: ESA David Knudsen on behalf of the EFI Team 3rd Swarm Science Meeting, Copenhagen, 19 May 2014

2 EFI Team: U Calgary COM DEV International ESA IRF, Uppsala
David Knudsen Johnathan Burchill Alexei Kouznetsov Bill Archer, Matthew Patrick COM DEV International Mike Smith, Project Manger ESA ESTEC, Project Team ESOC, Flight Operations Team ESRIN, Mission Team IRF, Uppsala Stephan Buchert Anders Eriksson Mats André, Jan-Erik Wahlund Lennart Ahlen, Reine Gill, Thomas Nilsson

3 Imaging electrostatic analyzer, electro-optical detection
TII sensors on Swarm CCD Phosphor MCPs FO Taper Ions Imaging electrostatic analyzer, electro-optical detection Langmuir probe x 2 per satellite LPs O+ H+ Simulation Ion focusing scheme: Whalen et al., [1994] (Freja CPA)

4 Full distributions every ~1 minute
TII sensors on Swarm E = -vixB CCD Phosphor MCPs FO Taper Ions LPs O+ H+ 3D velocity from orthogonal analyzers Calibrated 2Hz Full distributions every ~1 minute Ion temperature in 3 directions

5 Swarm TII “first light”
vertical flows horizontal cross-track flows along-track flows along-track flows

6 On-board processing: along-track
Position  velocity width temperature determined on ground (Level 1B) ram direction

7 Cross-track velocity (slope) and temperature (width)
determined on ground from on-board moments (1st and 2nd) simulated image

8 Performance – electric field resolution
0.3 mV/m (10 m/s) resolution achieved for n > 5x104 cm-3

9 EFI Science examples – this talk
Ionospheric dissipation [Patrick et al., poster] Ion heating [Archer et al., poster] Ion upflow [Burchill et al., talk] Auroral studies [Jackel et al., talk] Also: see presentations by Balasis, Fiori, Foerster, Forbes,

10 A: Magnetospheric forcing
1000 km 500 km Ionosphere 100 km B0 Thermosphere

11 B: Ionospheric currents
1000 km E 500 km Ionosphere 100 km B0 Thermosphere

12 C: Field-aligned currents
j|| 1000 km j|| 500 km Ionosphere 100 km B0 Thermosphere

13 B,ext j|| j|| D. External Fields δB E ~ 101-2 nT B0 1000 km 500 km
Ionosphere 100 km B0 Thermosphere

14 1) Dissipation (JE) B0 JOULE-II sounding rocket 1000 km
Sangalli et al., JGR [2009] 500 km 100 km B0

15 1) Dissipation – “remote sensing”
Energy inflow and dissipation: E Poynting’s Thm for static ionospheric fields [Kelley et al., 1991] B,ext ~ nT j|| 1000 km j|| 500 km Ionosphere 100 km B0 Thermosphere

16 B A C Dec 13, 2013 Dayside cusp ExδH (kW/km2) (field-aligned)
M. Patrick et al., poster

17 2: Ion Heating Tperp > T|| H V ~10,000 K See: Archer et al. poster

18 EFI Science Topic 3: Ion upflow
“Cusp ion fountain” Ion loss to space: 10’s TONS per day Requires : 10 eV per (O+) ion UPFLOW at Swarm altitudes to feed high-altitude acceleration after D. Gallagher

19 Swarm shows cusp upflows of 100’s m/s
See: Burchill et al. talk Burchill et al. 3rd Swarm Science Meeting

20 Level 1b products – prototype processor
vion E Ti ne

21 vion E Note excellent rejection of horizontal flows in vertical flow (yellow) measurement Ti ne

22 EFI Science Topic 4: Auroral science
The relation between auroral currents, auroral flows and auroral forms is only beginning to be explored! Eric Donovan Emma Spanswick

23 Ground-based arrays for auroral studies
Eric Donovan

24 Swarm EFI – New Capabilities
High-precision ExdB on multiple stable platforms Tri-directional ion temperature Dedicated vertical drift measurement Unprecedented opportunity for auroral science when combined with ground-based arrays Thank you:

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