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Magnetometer

Magnetometer. M.Yamauchi <at> irf.se Daria Mikhaylova Mats Luspa Lars-Göran Vanhainen Peter Dalin Csilla Szasz Peje Nilsson (Umeå) Fredrik Rutqvist (Umeå) Urban Braendström. 1. Magnetic observatories. IRF owns. SGU took over from IRF. Why do we measure. Ionospheric activity

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Magnetometer

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  1. Magnetometer M.Yamauchi <at> irf.se Daria Mikhaylova Mats Luspa Lars-Göran Vanhainen Peter Dalin Csilla Szasz Peje Nilsson (Umeå) Fredrik Rutqvist (Umeå) Urban Braendström 1

  2. Magnetic observatories IRF owns SGU took over from IRF

  3. Why do we measure Ionospheric activity aurora ~ current ~ conductivity etc. Earth evolution dynamo ~ polarity change Ground current spaceweather & condctivity

  4. Real-time page keogram Magnetogram aurora northward component (BX) eastward component (By) vertical downward component (BZ) http://www.irf.se/mag

  5. keogram Proccesed page northward component (BX) Magnetogram http://www.irf.se/mag eastward component (By) vertical downward component (BZ)

  6. Coordinate System Measurement: Horizontal-Declination-Inclination convert to XYZ Horizontal plane Vertical plane

  7. How to measure (equipment)

  8. What do we have at Kiruna? Vector field (1 sec): Flux gate magnetometer # Primary # Secondary (but just call “backup”) Absolute measurement (weekly): DI flux magnetometer # in operation # spair Total field = scalar value (every 4 sec): Proton magnetometer # in operation # spair Higher frequency than 1 Hz: Pulsation magnetometer # 3 sensors (XYZ) in oparation # one spair We also have a set at Lycksele, which is operated in collaboration with SGU

  9. Main building Variometer FGE 91 DMI

  10. Absolute House Proton magnetometer GSM-90 Gem Sys DI-flux DMI Zeiss Jena Backup GemSys och MinGeo

  11. Other magnetometers Pulsations Magnetometer Backup EDA 85B/94B UiT

  12. Proton Magnetometer Fluxgate Magnetometer

  13. Why do we measure Ionospheric activity aurora ~ current ~ conductivity etc. Earth evolution dynamo ~ polarity change Ground current spaceweather & condctivity

  14. Aurora ~ Magnetic field

  15. Old time without digital archive 1-hour values or 3-hour range index (K) for “digital data” K ~log(∆B) Running average of local K index 1962 1970 1980 1990 2000 2010

  16. Problem is baseline (due to convection) Sq curve 0 UT 12 UT 24 UT Raw data – Sq curve

  17. But, absolute measurement is difficult because we must measure the offset ! 2000 2005 2010 2015

  18. Another reason for absolute measurement 11200 nT northward (BX) 10600 nT 1980 1990 2000 2010 0 nT eastward (By) Kiruna By  0 ! -1400 nT 52000 nT vertical downward (BZ) 50600 nT 1980 1990 2000 2010

  19. Earth evolution

  20. Magnetic observatories with Invariant Latitude counter (h=200km)

  21. Large-scale induction current > 100 km scale high conductance 1. Electric power line  high grid stress 2. Searching underground property using auroral energy

  22. 3D plot (quiet day) Lycksele Kiruna quiet day trajectories

  23. 3D plot (disturbed day) Kiruna disturbed day trajectory

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