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Plasmapause detection by means of a meridional magnetometer array

PLASMON. Plasmapause detection by means of a meridional magnetometer array. Balázs HEILIG, GGIH, Tihany, Hungary Massimo VELLANTE, University Of L'Aquila, L'Aquila, Italy Anders JORGENSEN, New Mexico, USA János LICHTENBERGER, Eötvös University, Budapest, Hungary

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Plasmapause detection by means of a meridional magnetometer array

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  1. PLASMON Plasmapause detection by means of a meridional magnetometer array Balázs HEILIG, GGIH, Tihany, Hungary Massimo VELLANTE, University Of L'Aquila, L'Aquila, Italy Anders JORGENSEN, New Mexico, USA János LICHTENBERGER, Eötvös University, Budapest, Hungary Jan REDA, Geophysical Institute of PAS, Warsaw, Poland Mauro REGI, University Of L'Aquila, L'Aquila, Italy Gergely VADÁSZ, GGIH, Budapest, Hungary András CSONTOS, GGIH, Tihany, Hungary ESWW 10, Antwerp, Belgium, 22 November, 2013

  2. Outline Introduction 1) Plasmapause detection by ground magnetometer arrays (case study) a) from density (FLR frequency) profile b) from cross phase reversal c) from sudden changes in density 2) Validation using Van Allen Probes EMFISIS in-situ observations Future plans, conclusions ESWW 10, Antwerp, Belgium, 22 November, 2013

  3. Ground observation of ULF waves PLASMON EU FP7 263618 EMMA (European quasi-Meridional Magnetometer Array) 2012: MM100 + SEGMA FLRID: finding the resonance frequency OUJ-HAN L = 4.1 amplitude ratio cross phase Waters et al., 1991; Berube et al., 2003 FLRINV: Inversion FLR frequency --> plasma mass density ESWW 10, Antwerp, Belgium, 22 November, 2013

  4. Geomagnetic Field Line Resonances amplitude ratio ~ 1 Gradient-method (Baransky et al. 1985 Waters et al. 1991) phase diff. maximum Guglielmi, 1989 Menk et al., 2004

  5. FLRID (for PLASMON EMMA) FLRID: finding the resonance frequency FLRID uses both cross phase and amplitude information to detect FLRS FLRID checks for amplitude ratio (value and trend) FLRID detects both cross phase maxima and minima amplitude ratio cross phase OUJ-HAN L = 4.1 ESWW 10, Antwerp, Belgium, 22 November, 2013

  6. EMMA: plasmapause observations Case study: 28 Sep – 15 Oct, 2012 ESWW 10, Antwerp, Belgium, 22 November, 2013

  7. PP position from equatorial density profiles KEV-IVA L = 6.1 SOD-OUJ L = 4.9 15 October, 2012 OUJ-HAN L = 4.1 HAN-NUR L = 3.6 NUR-TAR L = 3.2 TAR-BRZ L = 2.9 BRZ-SUW L = 2.6 BEL-ZAG L = 2.2

  8. PP position from equatorial density profiles

  9. Empirical models for comparison: 1) PP from CHAMP msFAC observations New empirical PP model based on FAC observations Launch : 15 June, 2000 End of mission: 19 Sept, 2010 Orbit: polar orbit (i=87.3°) Initial altitude: 454 km Orbital period: 93.55 min Orbital speed: 7.6 km/s Drift in LT: 5.5 min/day msFAC boundary as a function of Kp and MLT Heilig and Lühr., AnGeo, 2013 ESWW 10, Antwerp, Belgium, 22 November, 2013

  10. HL PPCH2012 OM2003

  11. PP position from phase reversals HAN-NUR L = 3.6 NUR-TAR L = 3.2 TAR-BRZ L = 2.9 Milling, Mann and Menk, GRL, 2001

  12. PP position from FLRs Summary v PP from phase reversals

  13. PP position from abrupt changes of density 15 October 2012 13 October 2012 OUJ-HAN L = 4.1 HAN-NUR L = 3.6 NUR-TAR L = 3.2 TAR-BRZ L = 2.9 BRZ-SUW L = 2.6

  14. PP position from abrupt changes of density PP from abrupt density changes c

  15. PP position from FLRs Summary

  16. Validation using in-situ PP-crossings ESWW 10, Antwerp, Belgium, 22 November, 2013

  17. Van Allen Probes Comparison with in-situ PP observations EMFISIS: Electric and Magnetic Field Instrument Suite and Integrated Science

  18. Van Allen Probes VAP A 15 Oct, 2012 02:00-08:00 UT Magnetic footprint VAP Science Gateway, Magnetic Footprint tool (http://athena.jhuapl.edu/) ESWW 10, Antwerp, Belgium, 22 November, 2013

  19. Van Allen Probes Comparison with in-situ PP observations

  20. Van Allen Probes Comparison with in-situ PP observations

  21. Summary and future work • Daytime PP can be succesfully detected automatically by a ground-based magnetometer array • PP observations of EMMA are consistent with VAPs' in-situ observation • It would be desirable to increase the density of EMMA near L = 4 • New satellite missions (Van Allen Probes, SWARM) yield a unique opportunity to validate/compare ground based methods and the empirical PPCH2012 model The research leading to these results has received funding from the European Community’s Seventh Framework Programme ([FP7/2007–2013]) under grant agreement number 263218. ESWW 10, Antwerp, Belgium, 22 November, 2013

  22. Thank you for the attention! SWARM launchtoday at 12:02 GMT! 3 CHAMP-like satellites • 2 side-by-side with slowly changing separation • 1 above them (different orbital plane) 5 November, 2013, Plesetsk, Russia

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