1. Summary & Recommendations of EFI Splinter session 3
Lorenzo Trenchi
12/10/2018

2. LP, almost continuous coverage
LP, almost continuous coverage. A number of tests are planned in the future
TII, 3 – 6 orbits per day, water vapour anomaly. the quality of TII data is improving, on all 3 s/c [136 + Lesson Learnt in Jonathan’s talk! and 34+ operations during the last year, Di Betta]

3. Verification of existing EFI products:
Ne (LP)
Comparison probe 1 & 2, both high gain [Burchill]
Te (LP)
Swept mode Vs high / low gain Vs IRI [Truhlik]
Comparison of high-gain, low-gain with Incoherent Scatter Radar [Lomidze et al 2018]
Correlation of high / low gain, blended with electron density, in equatorial plasma depletions [Rodríguez-Zuluaga]
LP probe 1 & 2, both high gain [Burchill]
Faceplate and LP currents (LP)
Model simulations under different plasma conditions [Resendiz]
Vcross (TII)
calibration Zeroing flows at mid latitudes, and Verification with Weimer 2005 model [Lomidze]
Verification with co-rotation at low latitudes + DMSP driftmeter [Kouznetsov]
E field (TII)
validation / optimization [Marghitu]
Possible new EFI products:
about thermosphere-ionosphere coupling [Burchill]
Along-track ion drift from LP’s and faceplate currents [Burchill]
Ion mass estimates from LP [Foerster]

4. [Electron Temperature, Truhlik] armonic mode
Swarm B
Swarm C
Swarm A
armonic mode
Sweep mode
Good agreement of sweep mode with IRI suggests that contamination effect is negligible on Probe 1.
Swarm B
Swarm C
Swarm A

5. [Electron Temperature, Lomidze et al 2018]
This comparison showed instead a good agreement between the high-gain probe temperature & radar temperatures. Larger discrepancies in lower temperature ranges.
Swarm A
Swarm B
Swarm C
Swarm A
Swarm B
Swarm C
Low-gain Te
High-gain Te

6. [Cross track velocity, Lomidze]
This comparison shows:
high correlation ( )
small bias ( -40 m/s)
agreement within ~200 m/s (1-σ)
Often Swarm flow speeds tend to be significantly larger and more highly structured.

7. Swarm cross track velocity at the beginning of the mission
Swarm cross track velocity at the beginning of the mission. Reasonably good agreement with corotation at low latitudes, both on dayside, and nightside.
DMSP cross track velocity follows well the corotation, better than Swarm in the dayside, but not in nightside.
A proper verification doesn’t seem possible, even because of the different inclination of the orbits (DMSP along track velocity quite noisy)

8. [Electric field data, Marghitu]
A successful V/O provides a validated E (with small differences in conductivities already at the beginning), or optimized E (with small differences in conductivities at the end)

9. EFI Swarm A Swarm B ion-neutral momentum transfer collision frequency
thermosphere-ionosphere coupling [Burchill]
EFI
Swarm A
Swarm B
Based on ambipolar diffusion equation
ion-neutral momentum transfer collision frequency

10. [Ion mass estimates, Foerster]
The spatial distribution of m_eff is very similar to the one from IRI model

11. Summary & way forward Recommendations from PIs
A firmware update in order to:
fix the TII automatic gain control;
TII 16 Hz, very usefull for high latitudes (increase frequency as much has possible, reducing the pixels to 32 instead of 64, facilitating the telemetry)
fix the LP bias
Configurable fallback LP bias if tracking failure
Release a new cross-track velocity dataset, to fix offsets and cdf files
Distribute again ‘along track’ velocity dataset, possibly based on both TII and LP measurements
Recommendations from participants to DQW
The estimation of high energy particles flux is also possible from TII data. Provide a new high energy particles product, obtained from TII and Star tracker.
Define the e-POP science mode in order to collect data during conjunctions with Swarm. This will allow cross-calibration of cross track plasma velocity.