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
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
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
Geomagnetic Field Line Resonances
amplitúdó arány
amplitude ratio ~ 1
1.4
1.2
1
0.8
fáziskülönbség [°]
0.6
0
Gradient-method
(Baransky et al. 1985
20
40
80
100
Waters
et al.601991)phase
diff.
maximum
frekvencia [mHz]
60
40
20
0
Guglielmi,
0
20 198940
60
frekvencia [mHz]
Menk et al., 2004
80
100
FLRID (for PLASMON EMMA)
FLRID: finding the resonance frequency
FLRID uses both cross
phase and amplitude
information to detect FLRS
amplitude
ratio
FLRID checks for amplitude
ratio (value and trend)
FLRID detects both cross
phase maxima and minima
cross
phase
OUJ-HAN
L = 4.1
ESWW 10, Antwerp, Belgium, 22 November, 2013
EMMA: plasmapause observations
Case study: 28 Sep – 15 Oct, 2012
ESWW 10, Antwerp, Belgium, 22 November, 2013
PP position from equatorial density profiles
KEV-IVA
L = 6.1
SOD-OUJ
L = 4.9
15 October, 2012
EMMA 15 Oct 2012, 08:00-09:00
HAN-NUR
L = 3.6
NUR-TAR
L = 3.2
4
log (eq) [cm -3]
OUJ-HAN
L = 4.1
3
2
1
0
-1
2
3
log(eq) / L
BRZ-SUW
L = 2.6
6
5
6
2
1
0
-1
BEL-ZAG
L = 2.2
5
L [R E]
3
TAR-BRZ
L = 2.9
4
2
3
4
L [R E]
PP position from equatorial density profiles
EMMA 15 Oct 2012, 08:00-09:00
3
2
EMMA 3 Oct 2012, 08:00-09:00
log(eq) / L
3
-1
2
1
4
L [R E]
2
0
-1
31
4
0
L [R E]
2
EMMA 2 Oct 2012, 10:00-13:00
2
2
-1
6
4
3 1
2
3
0
-1
0
EMMA 10 Oct 2012, 08:00-09:00
4
5
3
L [R E]
2
3
3
5
6
2
1
4
5
0
L [R E]
2
2.5
3
6
3.5
4
4.5
5
5.5
6
6.5
4.5
5
5.5
6
6.5
L [R E]
1
4
3
-1
3
-1
1.5
2
0
6
5
4
log (eq) [cm -3]
2
2
3
1
L [R E]
2
5
log(eq) / L
-1
3
log (eq) [cm -3]
0
log(eq) / L
1
log (eq) [cm -3]
4
log(eq) / L
log (eq) [cm -3]
4
3
3
6
2
1
0
-1
1.5
4
5
6
L [R E]
2
2.5
3
3.5
4
L [R E]
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
50
Dst [nT]
0
-50
-100
-150
272
274
276
278
280
282
284
286
288
290
DoY 2012
PPCH2012
OM2003
HL
PP position from phase reversals
HAN-NUR
L = 3.6
NUR-TAR
L = 3.2
TAR-BRZ
L = 2.9
Kp
6
4
2
0
130
131
132
133
134
135
136
137
DoY 2012
Milling, Mann and Menk, GRL, 2001
PP position from FLRs
Summary
v
PP from
phase
reversals
EMMA and VAP PP 28 Sep - 15 Oct, 2012
6.5
6
5.5
5
L[RE]
4.5
4
3.5
3
2.5
2
1.5
272
274
276
278
280
282
DOY 2012
284
286
288
290
PP position from abrupt changes of density
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
15 October 2012
PP position from abrupt changes of
density
EMMA and VAP PP 28 Sep - 15 Oct, 2012
5.5
5
c
4.5
L[RE]
4
3.5
3
2.5
2
286
286.5
287
287.5
288
DOY 2012
288.5
289
289.5
290
PP from
abrupt
density
changes
PP position from FLRs
Summary
EMMA and VAP PP 28 Sep - 15 Oct, 2012
6.5
6
5.5
5
L[RE]
4.5
4
3.5
3
2.5
2
1.5
272
274
276
278
280
282
DOY 2012
284
286
288
290
Validation using in-situ
PP-crossings
ESWW 10, Antwerp, Belgium, 22 November, 2013
Van Allen Probes
Comparison with in-situ PP observations
EMFISIS: Electric and Magnetic Field Instrument Suite and Integrated Science
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
Van Allen Probes
Comparison with in-situ PP observations
EMMA and VAP PP 28 Sep - 15 Oct, 2012
6.5
6
5.5
5
L[RE]
4.5
4
3.5
3
2.5
2
1.5
272
274
276
278
280
282
DOY 2012
284
286
288
290
Van Allen Probes
Comparison with in-situ PP observations
EMMA 2 Oct 2012, 10:00-13:00
log (eq) [cm -3]
4
3
2
EMMA and VAP PP
1 28 Sep - 15 Oct, 2012
6.5
6
0
-1
1.5
2
2.5
3
3.5
4
4.5
5
5.5
6
6.5
4.5
5
5.5
6
6.5
L [R E]
5.5
log(eq) / L
3
5
L[RE]
4.5
4
2
1
0
-1
1.5
3.5
2
2.5
3
3.5
4
L [R E]
3
2.5
2
1.5
272
274
276
278
280
282
DOY 2012
284
286
288
290
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
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