Presentation is loading. Please wait.

Presentation is loading. Please wait.

Plasmapause detection by means of a meridional magnetometer array Balázs HEILIG, GGIH, Tihany, Hungary Massimo VELLANTE, University Of L'Aquila, L'Aquila,

Similar presentations


Presentation on theme: "Plasmapause detection by means of a meridional magnetometer array Balázs HEILIG, GGIH, Tihany, Hungary Massimo VELLANTE, University Of L'Aquila, L'Aquila,"— Presentation transcript:

1 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 PLASMON

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

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

5 FLRID (for PLASMON EMMA) OUJ-HAN L = 4.1 FLRID: finding the resonance frequency cross phase amplitude ratio 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 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 BRZ-SUW L = 2.6 BEL-ZAG L = 2.2 HAN-NUR L = 3.6 NUR-TAR L = 3.2 TAR-BRZ L = 2.9 OUJ-HAN L = 4.1 SOD-OUJ L = 4.9 KEV-IVA L = 6.1 PP position from equatorial density profiles 15 October, 2012

8 PP position from equatorial density profiles

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

10 HL PPCH2012 OM2003

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

12 PP position from FLRs Summary v PP from phase reversals

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

14 c PP from abrupt density changes

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 VAP A 15 Oct, :00-08:00 UT Magnetic footprint VAP Science Gateway, Magnetic Footprint tool (http://athena.jhuapl.edu/)http://athena.jhuapl.edu/ Van Allen Probes 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 ESWW 10, Antwerp, Belgium, 22 November, 2013 The research leading to these results has received funding from the European Community’s Seventh Framework Programme ([FP7/2007–2013]) under grant agreement number

22 Thank you for the attention! SWARM launch today 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


Download ppt "Plasmapause detection by means of a meridional magnetometer array Balázs HEILIG, GGIH, Tihany, Hungary Massimo VELLANTE, University Of L'Aquila, L'Aquila,"

Similar presentations


Ads by Google