1. Andrew W. Yau University of Calgary, Canada CASSIOPE Enhanced Polar Outflow Probe (e-POP) University of Alberta, October 25, 2007

2. Outline 1.e-POP Mission Objective 2.CASSIOPE and e-POP 3.e-POP Science Targets 4.e-POP Mission Strategy 5.e-POP Instruments & Measurements 6.Conclusions

3. e-POP Mission Objective Observations of space weather processes –Micro- and meso-scale processes –In topside polar ionosphere –At highest possible resolution –Focus on plasma outflow, neutral escape, auroral currents, irregularities, radio propagation

4. The CASSIOPE Small Satellite e-POP Science Payload High resolution studies of space plasma processes; wave-particle interactions Small Satellite Bus Generic, low-cost bus for Canadian small-sat missions Cascade Tech Payload High bandwidth store-and- forward data delivery demo

5. ENHANCED POLAR OUTFLOW PROBE (e-POP) Science Plasma outflow Acceleration; WPI; auroral connection Wave propagation 3D structure of ionospheric irregularities Neutral escape Temperature enhancement, non-thermal escape Mission Concept Highest-resolution in-situ measurements Radio wave propagation 3D studies Fast imaging of meso-scale aurora Mission Design Polar orbit: 325 × 1500 km; 80° incl. 3-axis stabilized Large data storage and downlink bandwidth (>1 TB, 300 Mbps)

6. Science Objective #1: Plasma Outflow Facts Significant energetic ionospheric ion injection to magnetosphere: ≥10 26 s -1 Topside polar ionosphere is source of multiple “cold” ion populations Questions Cold ions and driving processes: What is (are) the critical first step(s) in ionosphere- magnetosphere mass transfer? e-POP Objectives Plasma outflow and waves: Micro-scale ion upflow/acceleration; wave particle interaction; auroral connection

7. Science Objective #2: Radio Propagation Facts Plasma can refract, scatter, amplify, damp, or decompose electromagnetic waves. Refraction depends on ionospheric conditions. Questions How does M-I energy-mass coupling manifest in ionospheric irregularities? How do irregularities interact with waves - and affect radio wave propagation? SuperDARN e-POP Objectives Waves propagation in plasma: 3D structure of ionospheric irregularities; radio/GPS occultation studies

8. Science Objective #3: Neutral Escape Facts Charged/neutral H, He, and O rapidly charge- exchange in laboratory – and in space Questions Role of thermosphere in magnetosphere- ionosphere-thermosphere mass transfer? e-POP Objectives Explore neutral atmospheric escape: Temperature enhancement; non-thermal escape

9. ENHANCED POLAR OUTFLOW PROBE (e-POP) Science Plasma outflow Acceleration; WPI; auroral connection Wave propagation 3D structure of ionospheric irregularities Neutral escape Temperature enhancement, non-thermal escape Mission Concept Highest-resolution in-situ measurements Radio wave propagation 3D studies Fast imaging of meso-scale aurora Mission Design Polar orbit: 325 × 1500 km; 80° incl. 3-axis stabilized Large data storage and downlink bandwidth (>1 TB, 300 Mbps)

10. Sub-Decameter Scale Structures in Topside Ionosphere MARIE rocket, 500-600 km altitude, large substorm (LaBelle 1986) “Spikelets” –Localized lower hybrid waves –Lower hybrid solitary structures Often coincided with localized regions of TAI (“perpendicular ion conics”)  1 ms time scale and/or  1 m horizontal/vertical extent

11. Dynamic Small-scale Structures in Visual Aurora Auroral spatial scales: 10-100 km (bands), to 0.1-1 km (curtains) Auroral curls (Trondsen 1998): –1-2 km spatial scale –Anti-clockwise rotation and motion (when viewed anti-parallel to B)  13.5 km   10.1 km   10.8 km  W N

12. ENHANCED POLAR OUTFLOW PROBE (e-POP) Science Plasma outflow Acceleration; WPI; auroral connection Wave propagation 3D structure of ionospheric irregularities Neutral escape Temperature enhancement, non-thermal escape Mission Concept Highest-resolution in-situ measurements Radio wave propagation 3D studies Fast imaging of meso-scale aurora Mission Design Polar orbit: 325 × 1500 km; 80° incl. 3-axis stabilized Large data storage and downlink bandwidth (>1 TB, 300 Mbps)

13. FAI e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl 0.5-100 eV ions SEI Suprathermal electron imager Calgary Knudsen 1-200 eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 0.1-2 km/s neutrals MGF Magnetic field instrumentCalgary Wallis  B  j // RRI Radio receiver instrumentCRC James HF, VLF E(  ), k(  ) GAP GPS attitude, position, and profiling experiment UNB Langley L1, L2  Irregularity CER Coherent electromagnetic radio tomography NRL Bernhardt VHF  Irregularity FAI Fast auroral imagerCalgary Murphree 630 nm, NIR IRM SEI CER NMS RRI MGF GAP In-situ Instruments

14. e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl 0.5-100 eV ions SEI Suprathermal electron imager Calgary Knudsen 1-200 eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 0.1-2 km/s neutrals MGF Magnetic field instrumentCalgary Wallis  B  j // RRI Radio receiver instrumentCRC James E, k: HF, VLF (10 Hz –18 MHz) GAP GPS attitude, position, and profiling experiment UNB Langley L1, L2  Irregularity CER Coherent electromagnetic radio tomography NRL Bernhardt VHF  Irregularity FAI Fast auroral imagerCalgary Murphree 630 nm, NIR IRM SEI CER FAI NMS RRI MGF GAP Radio Instruments

15. e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl 0.5-70 eV ions SEI Suprathermal electron imager Calgary Knudsen 1-200 eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 0.1-2 km/s neutrals MGF Magnetic field instrumentCalgary Wallis  B  j // RRI Radio receiver instrumentCRC James HF, VLF E(  ), k(  ) GAP GPS attitude, position, and profiling experiment UNB Langley L1, L2  Irregularity CER Coherent electromagnetic radio tomography NRL Bernhardt VHF  Irregularity FAI Fast auroral imagerCalgary Murphree 630 nm, NIR IRM SEI CER FAI NMS RRI MGF GAP Auroral Imager

16. e-POP Science Team and Partner Organizations Communications Research Centre: HG James, P Prikryl Royal Military College: JM Noel U. Alberta: R Rankin, C Watt U. Athabasca: M Connors U. Calgary: PV Amerl, LL Cogger, E Donovan, DJ Knudsen, JS Murphree, TT Trondsen, DD Wallis, AW Yau U. New Brunswick: A Hamza, PT Jayachandran, D Kim, R Langley U. Saskatchewan: G Hussey, S Koustov, G Sofko, JP St Maurice U. Victoria: RE Horita U. Western Ontario: L Kagan, J MacDougall York U: JG Laframboise, J McMahon JAXA/ISAS, Japan: T Abe, H Hayakawa, K Tsuruda NRL, USA: PA Bernhardt, C Siefring UNH, USA: M Lessard

17. Conclusions e-POP … Part of multi-purpose CASSIOPE mission Mission objective: highest-resolution space weather observation –Plasma outflow, wave propagation, and neutral escape Payload: 8 plasma, field, optical, radio instruments Focus: hi-res particle/wave observations and fast auroral imaging Use non-spinning orbiter, large data storage, fast downlink Coordinated operation with ground facilities an essential element

18. For more information, please visit: http://mertensiana.phys.ucalgary.ca Thank You!

19. Lower Hybrid Solitary Structures in Topside Ionosphere LHSS signatures –Density depletion –TAI and/or BB VLF noise GEODESIC rocket, 980 km (Burchill 2004) Low-energy ion distributions –11 ms/13 m resolution –T  0.2 eV (rammed O + ions) –Heated ions at several eV Observed density cavity –  15% depletion –Temporal extent:  10 ms

20. LHSS “Heating” Width “Heating” width of LHSS on GEODESIC –from velocity images Average width: 63 m Standard dev.: 25 m Range: 13 – 190 m “Density depletion” width  20 m Burchill et al., 2004