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

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

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

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

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)

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

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

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

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)

Sub-Decameter Scale Structures in Topside Ionosphere MARIE rocket, 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

Dynamic Small-scale Structures in Visual Aurora Auroral spatial scales: km (bands), to 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

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)

FAI e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl eV ions SEI Suprathermal electron imager Calgary Knudsen eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 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

e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl eV ions SEI Suprathermal electron imager Calgary Knudsen eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 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

e-POP Instrument Complement Name InstrumentPIMeasurements IRM Imaging and rapid ion mass spectrometer Calgary Amerl eV ions SEI Suprathermal electron imager Calgary Knudsen eV electrons NMS Neutral mass and velocity spectrometer JAXA/ISAS Hayakawa 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

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

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

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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

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