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MULTIPLEX

MULTIPLEX. Ian McCrea, Tim Yeoman, Mike Kosch, Farideh Honary Mike Rietveld, Anita Aikio, Ove Havnes, Ingrid Sandahl. Polar Atmosphere Working Group: Membership. PPARC funded Dr. Ian McCrea (RAL, chair) Prof. Farideh Honary (Lancaster) Dr. Tim Yeoman (Leicester) NERC funded

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MULTIPLEX

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  1. MULTIPLEX Ian McCrea, Tim Yeoman, Mike Kosch, Farideh Honary Mike Rietveld, Anita Aikio, Ove Havnes, Ingrid Sandahl

  2. Polar Atmosphere Working Group: Membership • PPARC funded • Dr. Ian McCrea (RAL, chair) • Prof. Farideh Honary (Lancaster) • Dr. Tim Yeoman (Leicester) • NERC funded • Prof. John Plane (UEA) • Dr. Howard Roscoe (BAS) • Joint funded • Prof. Nick Mitchell (Bath)

  3. Polar Atmosphere Working Group: Context • PPARC “Solar system science strategy” (2002) • Three key themes • Energy flow in the solar system • Fundamental plasma processes • Conditions for life • NERC “Science for a sustainable future” (2002) • Importance of global change • Solar effect on climate identified as a priority • Town Meeting – Coseners House 30/09/2003 • Synergy between PPARC and NERC programmes • Cross-council working group to map out strategy

  4. Polar Atmosphere Working Group: Programmes • MULTIPLEX (PPARC) • Fundamental physics of energy flow • Importance of non-linear coupling • New emphasis on active techniques • Based on facilities already in operating plan • Cost £8m over five years, but only £1m is new money • DEEVERT (PPARC/NERC) • Effects of solar variability on climate • Importance of non-linear coupling and wave processes • Combines PPARC and NERC observation and modelling • Uses many of same facilities as MULTIPLEX • Cost £10m over five years, half from NERC • £0.5m new money from PPARC, leverages £5m from NERC

  5. Solar-terrestrial energy flow • The problem: • Good macroscopic description of energy transfer processes exists….. …but lacks predictive power • Energy flow depends critically on non-linear coupling • Need to know which mechanisms are important and when • Need to understand how system evolves from one state to another

  6. Solar-Terrestrial Energy Flow Anomalous resistivity Solar energy input Solar wind Magnetic reconnection Induced E-fields Ion drift SW energetic particles Plasma irregularities and turbulence Storage and release Neutral wind Electron and proton aurora Acceleration mechanisms Anomalous heating Joule dissipation Conductivity Ionospheric electrodynamics Composition, circulation heat balance Electro-magnetic radiation Chemistry and transport Ionisation and particle heating

  7. Solar-terrestrial energy flow • The problem: • Good macroscopic description of energy transfer processes exists….. …but lacks predictive power • Energy flow depends critically on non-linear coupling • Need to know which mechanisms are important and when • Need to understand how system evolves from one state to another • Strategy for solution: • Active experiments allow us to stimulate non-linear processes • New, improved diagnostics • Synthesis of experimentation and modelling

  8. The MULTIPLEX programme • Why now ? • Paradigm shift from phenomenology to directed experimentation • New active experimental techniques • Major new UK facilities (e.g. SPEAR) • Novel data raising new insights and questions • Why UK ? • UK is world-leading in active experimentation • UK has access to world-class instruments • UK has state-of-the-art numerical models • UK has excellent track record of exploiting international programmes

  9. EISCAT Tromsø HF Heater

  10. Artificial Aurora Rings form initially, collapsing into blobs Rayed structures form along magnetic field

  11. Non-thermal signatures show that collapse of rings corresponds to features descending in altitude

  12. EISCAT shows that strong electron temperature enhancements occur….. ….but these cannot explain the observed emission

  13. CUTLASS observations of plasma waves show which coupling processes are involved.

  14. Dynamics of auroral arcs

  15. Dynamics of auroral arcs

  16. Anomalous echoes from natural aurora • coherent scatter from ion acoustic waves • structure size under 300 m at 500 km altitude • varies on 0.2 second time scale

  17. The EISCAT Svalbard Radar

  18. Probing wave and particle populations on open field lines

  19. SPEAR, CUTLASS and the ESR

  20. On Off Off Plasma line amplitude On Off Off Ion line amplitude

  21. The MULTIPLEX programme: Goals • Understand energy exchange between magnetosphere, ionosphere and thermosphere • Move from qualitative to quantitative understanding • Quantify role of non-linear coupling in • Auroral acceleration and structure • Field-aligned currents and waves • Ionospheric irregularities • Non-thermal plasmas • Ion-neutral coupling • Linkages between processes at different scale sizes • Understanding key mechanisms • Proton aurora • Artificial aurora • Coherent echoes

  22. The MULTIPLEX programme: Questions • What processes mediate energy flow ? • How important is non-linearity ? • Which non-linear processes are most important ? • How are they triggered ? • How can we explain observed phenomena ? • Auroral acceleration and structure • Field-aligned currents and waves • Ionospheric irregularities • Non-thermal plasmas • Ion-neutral coupling • Same questions important for whole plasma universe.

  23. The MULTIPLEX programme: Facilities • EISCAT • Definitive measurements of plasma parameters • Active experiment capabilities • SPEAR • Unique new UK facility for active plasma experiments • CUTLASS • Measurements of global electrodynamics • Essential support for SPEAR and EISCAT experiments • SIF/Tromso Imager • Studies of auroral energisation and structure • FPI/SCANDI • Understanding scale sizes in thermosphere dynamics • Magnetometers • Relating ULF waves and field-aligned currents • Riometers • Wide-scale measurements of energetic particles

  24. Polar Mesosphere Summer Echoes (PMSE)  Seen in EISCAT radar in last 15 years  Charged dust/ice? Breaking of upgoing gravity waves?  Early phase in the formation of noctilucent clouds? PMSE

  25. PMSE modulation using the EISCAT Heater Overshoot effect – Lower dust density, or larger dust grains ??

  26. EISCAT

  27. The importance of EISCAT • EISCAT Svalbard Radar • Essential for understanding SPEAR science • Unique new auroral interferometry capability • Invaluable context for optical data • EISCAT UHF Radars • Tristatic capability unique for electrodynamics • Essential for ionosphere-thermosphere coupling • Unique IPS capability for solar wind studies • EISCAT VHF Radar • Optimised for low-density plasma (mesosphere and topside) • Essential for full height profiles of dynamics • Tromso HF Heater • World’s leading facility for active experiments in plasma physics • Unique active experiments on mesopause phenomena

  28. Extended runs of high latitude data… 5-23 February 2001

  29. Present IS Radar Status 10 radars operate routinely

  30. AMISR Advanced Modular Incoherent Scatter Radar 384 Panels, 12,288 AEUs 3 DAQ Systems 3 Scaffold Support Structures

  31. Phased array IS radar 32 AEUs = 1 panel AEU 2 panels on far-field test rig Possible Andøya deployment 128 panels = 1 face (4096 AEUs) at ~2MW

  32. International Polar Year • 2007 is the next International Polar Year (and the 50th, 75th, and 125th anniversaries of the International Geophysical Year and the first two International Polar Years). • Will run (at least) the high-latitude incoherent scatter radars for the entire year as part of the ICESTAR/IHY ‘cluster’.

  33. Aims of MULTIPLEX • Quantify temporal and spatial variability of energy deposition • Study large and small-scale energy transfer processes • Focus on energy coupling and non-linearity • Exploit both natural and artificially-generated processes • Assimilate data into models for predictive studies • Synergy with other studies (CAWSES, LTCS, DEEVERT, ISPAM) • Establish a legacy of instruments available after IPY

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