physics department, university of l’aquila, italy
DESCRIPTION
ULF FIELD-LINE RESONANCES IN THE EARTH’S MAGNETOSPHERE. Massimo Vellante. Physics Department, University of L’Aquila, Italy. BG - URSI School on Waves and Turbulence Phenomena in Space Plasmas 1-9 July, 2006, Kiten, Bulgaria. 1. ULF FIELD-LINE RESONANCES IN THE EARTH’S MAGNETOSPHERE. - PowerPoint PPT PresentationTRANSCRIPT
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Physics Department, University of L’Aquila, Italy
ULF FIELD-LINE RESONANCES
IN THE EARTH’S MAGNETOSPHERE
Massimo Vellante
BG - URSI School onWaves and Turbulence Phenomena in Space Plasmas1-9 July, 2006, Kiten, Bulgaria
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OUTLINE
• MHD wave modes in a uniform, cold plasma;
• MHD wave modes in a dipole field;
• Uncoupled toroidal and poloidal modes, eigenfunctions
calculation for the Earth’s magnetosphere;
• Field line resonance (FLR): basic theoretical characteristics
(Southwood’s box model);
• Effect of the ionosphere;
• Methods for detecting FLRs: gradient technique;
• Experimental observations of FLRs in space and on the ground;
• Monitoring the magnetospheric dynamics by FLRs.
ULF FIELD-LINE RESONANCESIN THE EARTH’S MAGNETOSPHERE
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The Magnetosphere
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Geomagnetic pulsations
ULF (1 mHz – 1 Hz) oscillations of the geomagnetic field observed
both in space and on the ground.
In 1954, Dungey suggested that the common occurrence of regular
geomagnetic pulsations with distinct periods could be the signature of
wave resonances in the magnetospheric plasma.
Magnetospheric waves in the ULF frequency range can be described
using the MHD approximation: frequency lower than the ion girofrequency.
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1) e = b/t Faraday’s law
2) b = o j Ampère’s law
3) e = v B Ohm’s law (frozen field)
4) v/t = j B Momentum equation
Basic MHD equations for small amplitude perturbations (b, e, v, j)
in a cold, highly conducting, collisionless, magnetized fluid:
In the ionosphere, where collisions are
important:
3’) j = o e// + P e + H e (B/B)
o: parallel conductivity
P: Pedersen conductivity
H: Hall conductivity
2e/t2 = VA VA e
VA = B/(o)1/2 = Alfvén velocity
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MHD WAVE MODES IN A UNIFORM, COLD PLASMA
1) ALFVEN (TRANSVERSE) MODENon-compressional, guided along the ambient field
2) FAST (COMPRESSIONAL) MODENo preferencial guidance: isotropic mode
b B
Poynting vector S // B
= k// VA VA = B/(o)1/2
b// 0
S 0
= k VA
v,b
e
jk
B
B
kv
b
j,e
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A typical Alfvén velocity in the magnetosphere is 103 km/s,
while typical periods of ULF waves (geomagnetic pulsations)
are in the range 10 – 500 s.
Thus, typical wavelengths are in the range 1 -100 RE:
comparable or even greater than the size of the magnetosphere.
Therefore, the uniform cold plasma approximation is not
appropriate.
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MHD WAVE MODES IN A DIPOLE FIELD
)1
( 2
2
221tV
ggA
h2 e = )( 1 t
g
h3 b
)1
(2
2
212tV
ggA
h1 e = )( 2 t
g
h3 b
t
(h3 b ) = (h1 e ) (h2 e )
g1, g2, h1, h2, h3: dipole metric functions
Transverse and compressional modes are coupled
1)
2)
3)
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Axial symmetry: / = 0
)1
(2
2
221tV
ggA
h2 e = 0
TOROIDAL MODE
Polarization: e , b , v
Azimuthal oscillations of plasma and field lines.
Independent, in-phase torsional oscillation of
individual magnetic shells.
Poynting vector S e b along B
Wave guided along the field line.
h1 e = 0
POLOIDAL MODE
2
2
22
2
2121
tVggg
A
Polarization: e , b , b , v
Plasma and field line oscillations in the
meridian plane.
Propagation across the magnetic field.
b = b// 0 compressional mode
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Localised mode: /
Polarization: e , b , v
GUIDED POLOIDAL MODE
)1
(2
2
212tV
ggA
h1 e = 0
b,vS
e
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SCHEMATIC PLOT OF THE GUIDED STANDING
OSCILLATIONS IN THE MAGNETOSPHERE
Magnetic field lines have fixed ends in the ionosphere, assumed as a perfect conductor.
Multiple reflections of the guided Alfvén wave generate a standing structure.
POLOIDAL TOROIDAL
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Symmetry relations of wave hodograms at conjugate stations allow to determine
if the mode is odd (case a) or even (case b). Lanzerotti et al. (1972).
CONJUGATE OBSERVATIONS
(a), odd mode (b), even mode
H North
D East
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GUIDED EIGENMODES CALCULATION
AXISYMMETRIC TOROIDAL MODE LOCALISED POLOIDAL MODE
0)(
)31(2
222
2
2
νν εε
zVzr
dz
d
Aeq
0
)()31(
31
62
222
22
2
εεε
zVzr
dz
d
z
z
dz
d
Aeq
r
req
r = req sin2
RE
z = cos
VA = B/(o)1/2 = Alfvén velocity1) specifying a model for the plasma
density distribution (z);
2) using boundary conditions for the electric field
, = 0 at r RE (ionospheric level);
3) equations can be solved numerically
to find the eigenfrequencies .
Temporal variations: exp(-it)
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WKB / TIME-OF-FLIGHT APPROXIMATION
P1
P2
n = 1,2,3,…
field-line eigenperiods time-of-flight :
2
1 )(
2 P
P sV
dsn
AnT
2
1
2/1
2/1
)(
)(2 P
Pods
sB
sn
nT
VA(s) = B(s) / [o (s)]1/2 = field-aligned Alfvén velocity
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f5 / f1 = 6.09 8.33
f4 / f1 = 4.82 6.59
f3 / f1 = 3.55 4.84
f2 / f1 = 2.28 3.08
TOR POL
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Latitudinal variation of the fundamental field-line eigen-period
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EIGEN-OSCILLATIONS OF LOW-LATITUDE FIELD LINES
only H+
both H+ and O+
South Africa array
(Hattingh and Sutcliffe, 1987)
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Space observations of field-line eigen-scillations
Anderson et al., 1989
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An example of a pulsation event with latitude-dependent period
Φ = 52°
Φ = 47°
Φ = 41° Miletits et al., 1990
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L
3.83
3.28
3.04
2.75
2.44
3.83
3.28
3.04
2.75
2.44
167- 200 s 117- 133 s 87- 105 s 69 - 80 s
167- 200 s 117- 133 s
87- 105 s 69 - 80 s
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Diurnal and latitudinal polarization pattern
Polarization reversals across:
- noon meridian
- latitude of maximum amplitude
Kelvin-Helmholtz instability
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Field line resonance model
(Southwood; Chen and Hasegawa, 1974)
IONOSPHERE
IONOSPHERE
l
EARTH
x -H
z
MAGNETOPAUSE
y D
Plasma density = (x)
eigenfrequency
R(x) = ( π / l ) VA (x) =
= ( π / l ) B [o (x)]-1/2
B
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IONOSPHERE
IONOSPHERE
monochromatic wave: e - i t
l
x xR
z
y
R= R(x) resonance: R=
assuming magnetic perturbations of the form:
b = b (x) exp [i (k// z + my - t)],
near the resonance:
0)]([
222
2
2
2
xx
R
x bmdx
db
xdx
bd
1
)( 1
dx
d
scale length of the inhomogeneity
singularity at x = xRbecause of dissipative effects: - i
By expanding R(x) around R(xR):
01 2
2
2
xx
R
x bmdx
db
ixxdx
bd
= 2γδ/ω = resonance width
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01 2
2
2
xx
R
x bmdx
db
ixxdx
bd
Solutions are given by the modified Bessel functions,
bx bo log [m (x – xR – i ) ]
close to xR : i bo by (xR) by = m (x – xR - i) 1+ i (x - xR) /
At the resonant latitude xR :
a) More pronounced peak and sharper phase change for by, i.e. in the azimuthal direction:
Toroidal mode dominates;
b) The horizontal polarization is predicted to reverse the sense across the resonance where
becomes almost linear;
c) The horizontal polarization changes sense according to the sign of the azimuthal wave
number m: if the driving source is due to the Kelvin Helmholtz instability polarization reversal
across the noon meridian.
AMPLITUDE (by)
PHASE (by)
x
x
xR
xR
-π/2
π/2
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CW CCW CW
Theory Observations
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IONOSPHERIC EFFECT (Hughes, Southwood, 1976)
The Pedersen current shields the incident signal. On the ground, we observe the signal
generated in the E-region (altitude ~120 km) by the Hall current.26
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On the ground, the signal is rotated through 90° and smoothed: features with
scale lengths less than ~120 km (E-region altitude) are strongly attenuated.
Ionospheric effect on the resonance structure
Magnetospheric signal
Ground signal
Hughes and Southwood, 1976800 400 0 - 400 - 800 800 400 0 - 400 - 800
LATITUDE PROFILE (km)resonance
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Observed spectrum
Source spectrum
Resonance response
Resonance effects can be easily masked by:
- peculiarities of the source spectrum
- ionospheric smoothing 28
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Detection of different harmonics at L = 2.3 by the H/D technique(Vellante et al., 1993)
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Gradient method for detecting field line resonances from
ground-based ULF measurements (Baransky et al., 1985)
N
S
Higher latitude field line → Lower resonant frequency ( N )
Lower latitude field line → Higher resonant frequency ( S )
EARTH
Separation: 1°- 3°
1 < 2 < 3
x2
N S
AM
PL
ITU
DE
RE
SP
ON
SE
SOUTH
SOUTH
PH
AS
E R
ES
PO
NS
E
x3x1
x2x1 x3
N S
A N
/A S
1
2
Δx/
2
S -
N2 tan-1(Δx/2)
AMPLITUDE RATIO
CROSS-PHASE
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An example of gradient measurements (Green et al., 1993)
Power spectra at TM, L = 1.59
Power spectra at AK, L = 1.51
H/D
Amplitude ratio
Cross-phase
Δx ~ 240 km
fR = 78 mHz
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CHAMP trajectory and SEGMA lines of force in a meridional plane. CHAMP spends about
1.5 min to cover the latitudinal range of the SEGMA array. The longitudinal difference between
CHAMP and SEGMA is less than 4°.
Ground-satellite comparative studyEvent of July 6, 2002 (Vellante et al., 2004)
CHAMP trajectory
SEGMA array
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Magnetic field data from CHAMP and SEGMA array. The data are filtered in the frequency band 20–100 mHz.
The gray region indicates the time interval of the conjunction. The stars indicate the conjunction to each station.
N C R A
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CHAMP azimuthal
compress.
SEGMA - H
SEGMA - D
NCK
CST
RNC
AQU
NCK
CST
RNC
AQU
Spectral analysis
NCK - CST, L=1.82
CST - RNC, L=1.70
RNC - AQU, L=1.60
azimuthal comp: peak at ~65 mHz
compressional comp: peak at ~55 mHz
ground stations: peak at ~55 mHz
FLR frequency at L=1.60: ~55 mHz
Source frequency: 55 mHz
Resonance at L=1.60
To be explained the
higher frequency of
the azimuthal comp.
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Simulation of the signals observed by the CHAMP satellite
Resonance structure, = 80 km, VSAT = 7.6 km/s
Amplitude
Phase
driving signal
(f = 55 mHz)
forced signal
signal
power spectra
resonance
At the resonant point :
Vphase = 2π f ~ 30 km/s
VSAT = 7.6 km/s
equatorward
Vphase = 30 km/s
poleward
Resonant signal shifted in frequency
in the satellite frame of reference.
The shift expected from the theoretical
FLR structure agrees with that
experimentally observed (~ +20%).
VSAT
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fR (midday)
53 mHz
64 mHz
69 mHz
Dynamic cross-phase analysis at SEGMA array
An example of diurnal variation of the resonant frequency
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An example of harmonics detection
fR (midday) f2 / f1
40 mHz ~ 2.1
52 mHz ~ 2.0
66 mHz ~ 1.8
f2 / f1 < 2 at L = 1.6 in agreement with theoretical expectations (Poulter et al, 1988)37
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Monitoring the plasma dynamics during geomagnetic storms
detection of plasma depletion (Villante et al., 2005)
pre-storm recovery phase
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ANNUAL VARIATION OF THE FLR FREQUENCY AT L = 1.61, YEAR 2003
DAILY AVERAGES (0900 – 1600 LT)
27 Days
a nearly 27-days modulation appears which must be
connected to the recurrence of active regions of the Sun
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SOLAR IRRADIANCE DEPENDENCE OF THE FLR FREQUENCY (L = 1.61)
An increase of the solar EUV/X-ray radiation increases the ionization rate in the ionosphere.
This influences the whole distribution of the plasma along the low-latitude field line.
Vellante et al., 2006
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Solar Cycle Variation of the Field Line Resonant Frequency at L’Aquila (L = 1.56)
Assuming ρmax ≈ 2 ρminfr
2
Vellante et al. (1996)
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Plasmapause identification
3 4 5 6 7 8 9
L value
3 4 5 6 7 8 9
L value
Menk et al., 2004 42
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Mid-continent MAgnetoseismic Chain (McMAC):
A Meridional Magnetometer Chain for Magnetospheric Sounding
1.3 < L < 11.7
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A schematic representation of field line
resonances driven by resonant magnetospheric
cavity modes. The top panel shows the periods
of three harmonics of cavity resonance, which
do not vary with L-shell, and the variation of the
fundamental field line eigenperiod with L shell.
There are three L shells where the fundamental
field line eigenperiod matches one of the cavity
mode eigenperiods. In the lower panel the
variation of wave amplitude at each of the three
cavity eigenperiods with L shell is drawn.
Note how a field line resonance is driven each
time a field line eigenperiod match.
(Hughes, 1994).
FLRs – cavity modes coupling
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