1. Space Weather Studies with EISCAT_3D: Developing the Science Case Ian McCrea on behalf of the EISCAT_3D Project Team

2. Five key capabilities: Volumetric imaging ( enabled by digital beam forming ) Aperture Synthesis imaging => sub-beamwidth structures Multistatic configuration => 3D vector velocities Greatly improved sensitivity (e.g. 32 000 antenna elements in transmitter, 16 000 in receivers) Transmitter flexibility (e.g. coding, beam-forming) These abilities have never before been combined in a single radar! EISCAT_3D Key Capabilities

3. EISCAT_3D Design Principles Distributed phased array with multiple sites At least one active site Multiple receive sites, with optimised geometry Support for co-located instruments Highly flexible transmitter High VHF frequencies (e.g. 233 MHz) Narrow bandwidth on transmit Wider bandwidth on receive Possibly different arrays for Tx and Rx Rx array distributed for imaging Low-elevation capability Capable of continuous operations Unattended operations at remote sites Possibility to adapt experiments in real-time Significant data processing at central site

4. Location of EISCAT_3D EISCAT_3D will be located within the auroral oval and on the equatorward edge of the polar vortex: key regions for global atmosphere-ionosphere system! Statistical auroral oval (depends on UT and Kp index). Schematic figure of winter polar vortex (courtesy of M. Clilverd).

5. 69.4 N 30.0 E 69.58 N 19.22 E 68.2 N 14.3 E One possible site orientation Final site selection still undecided Site surveys in progress

6. EISCAT_3D Transmitters Centre frequency 220-250 MHz Peak output power > 2 MW -1 dB power bandwidth > 5 MHz Pulse length 0.5 to 2000 us Pulse repetition frequency 0 to 3000 Hz Arbitrary waveform generation Must be rugged and mass-producible at low cost

7. EISCAT_3D Antennas The “Renkwitz Yagi” Centre frequency 235 MHz Bandwidth 12 MHz (>20 dB) Opening angle 40 o (core array), 30 o (receiver arrays) Arbitrary polarisation Good sidelobe supression 7dB gain over 10% relative bandwidth Need to be mechanically robust (e.g. due to snow loading) Bandwidth should not be affected by icing Mutual coupling needs to be acceptable

8. LOFAR HBA Test Array at Kilpisjärvi HBA Array – summer 2011 LBA Array – summer 2012

9. EISCAT_3D Signal Processing Design study did not specify a chosen system due to speed of evolution in DSP technology Preparatory phase will evaluate the use of multi-channel samplers and high performance computing for DSP and beam-forming EISCAT_3D technology can be prototyped on a range of different systems, e.g. the MST radar at Sodankyla.

10. EISCAT_3D Work Packages WP1: Management and reporting WP2: Legal and logistical issues WP3: Science planning and user engagement WP4: Outreach activities WP5: Consortium building WP6: Performance specification WP7: Signal processing WP8: Antenna, front end and timing WP9: Transmitter development WP10: Aperture synthesis imaging WP11: Software theory & implementation WP12: System control WP13: Data handling & distribution WP14: Mass-production & reliability

11. Science Working Group (SWG) Typically 2+5 members Membership rotated on a yearly basis Works to keep the Science Case up-to-date and bring new ideas from the existing and new EISCAT user groups. Helps to compile a list of contact persons/groups for potential new EISCAT_3D user communities WP3: Science Planning and User Engagement Science Working Group after a day’s work with the EISCAT_3D Science Case

12. The Science Case Document: A. Atmospheric physics and global change B. Space and plasma physics C. Solar system research D. Space weather and service applications E. Radar techniques, coding and analysis Appendix A: Table of EISCAT_3D radar performance requirements by science topics

13. EISCAT_3D Science Case, 1 st version 30.6.2011

14. High-Latitude Electron Density: Large-Scale Structure Targets: – TEC structure and variability (for GPS) – Density peak and profile variations (for communications) Wide view field for position of oval, trough etc. Quasi-simultaneous imaging gives real-time maps Continuous operation for effects of geomagnetic disturbance on density Independent TEC information from multi- path Faraday rotation Image Credit: Lucilla Alfonsi, INGV

15. High-Latitude Electron Density: Small-Scale Structure Targets: – Small scale irregularities (scintillation) – Flow/gradient regions (irregularity generation) Large-scale imaging allows potential scintillation regions to be identified Aperture synthesis imaging allows investigation of small structures Continuous operation allows monitoring capability and climatology determination Obvious synergy with satellite measurements and models Phase scintillation signatures on disturbed and active days Image Credit: Lucilla Alfonsi, INGV

16. Targets: o Real-time E-fields o Conductivity, current and heating rate maps o Relationship to irregularity and structure Continuous monitoring provides possibility to separate solar wind, auroral, diurnal effects Long-period data provide climaotology of electrodynamic effects Interaction between monitoring and modelling can improve understanding of hazards e.g. GICs in northern Europe. Electrodynamics Image Credit: Lucilla Alfonsi, INGV

17. Observation Simulation Targets: o Comparison/validation for models o Data input/assimilation techniques o Semi-empirical models from data Broad coverage and long-period data provide a huge resources for modelling community Lots of interesting science from data/model comparisons in IPY Need more engagement with the modelling community on critical parameters to measure; timing and frequency of observations Modellling Image Credit: Frederic Pitout, Toulouse

18. Targets: o Short-term thermospheric change during disturbances o Identification of long-term trends (thermosphere contraction) Long-term data allows monitoring role Continuous operations ensure effects of short-term disturbances are measured. Complement to international modelling community Combination of ion velocity and airglow measurements gives neutral density measurements via momentum equation. Satellite tracking and ranging capabilities provide additional thermosphere moniitoring capabilities. Thermosphere

19. Space Debris Space debris is integral part of EISCAT data (otherwise thrown away) ESA buys EISCAT time for space debris studies Regular monitoring allows identification of “space debris” events (e.g. Cosmos/Iridium) Potential for individual object tracking/ranging using adaptive beams Observation compares and drives modelling (e.g. debris cloud evolution) Obvious synergy with thermosphere measurements Image Credit: Juha Vierinen, SGO

20. Solar wind monitoring via scintillation of radio stars Multi-site observations yield solar wind velocity Single site observations give irregularity content and variability Solar wind acceleration processes Identification of fast/slow streams Irregularity content of solar wind Solar wind tomography and CMEs Solar wind magnetic structure (?) Solar Wind Studies Image Credits: Steve Crothers (STFC-RAL) and Mario Bisi (Aberystwyth)

21. EISCAT_3D has clear potential as a space weather instrument Capabilities go beyond anything available to the radar community Realising this potential needs: Well thought-out plan of operations Well thought-out plan of operations Good connection to other instrument programs Good connection to other instrument programs Better connection to/support for models Better connection to/support for models To do this, we need to involve space weather community at a higher level within EISCAT Conclusions

22. Get involved! In the new EISCAT Scientific Association, new members (at different commitment levels) are welcomed! Welcome also to the 4 th EISCAT_3D User meeting in Uppsala 23–25 May 2012! 1 st day will be dedicated to Space Weather issues. Science case document: http://www.eiscat3d.seContact: anita.aikio@oulu.fi anita.aikio@oulu.fi anita.aikio@oulu.fi anita.aikio@oulu.fi ian.mccrea@stfc.ac.uk ian.mccrea@stfc.ac.uk esa.turunen@eiscat.se esa.turunen@eiscat.se