PARTICIPATING UNIVERSITIES

1
MURI REVIEWMarch 3, 2008
Dennis Papadopoulos
PARTICIPATING UNIVERSITIES UNIVERSITY OF
MARYLAND, COLLEGE PARK STANFORD
UNIVERSITY UNIVERSITY OF CALIFORNIA, LOS
ANGELES DARTMOUTH COLLEGE VIRGINIA TECH BOSTON
COLLEGE
2
THE MURI TEAM - UMCP

• DENNIS PAPADOPOULOS
• ROALD SAGDEEV
• GENNADY MILIKH
• XI SHAO
• NAIL GUMEROV
• WALLY MANHEIMER
• GLEN JOYCE
• LEONID RUDAKOV
• BENGT ELIASSON
• ANDREW DEMEKHOV
• OLEG POKHOTELOV
• ALEXEY KARAVAEV
• HIRA SCHROFF
• BIRU TESFAYE
• LUKE JOHNSON
• Visitor
• Student

3
RESOURCES
DEMETER
HAARP
LAPD
CONJUGATE BUOYS
DMSP
WIDE RANGE OF CODES THAT COUPLE TO THE ABOVE
EXPERIMENTS
4
Relevant Wave Modes
5
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
6
AIP Code Validation (T. Chevalier)

• Science Issues
• The sheath surrounding an electric dipole antenna
  operating in a plasma has a significant effect on
  the tuning properties.
• Terminal impedance characteristics vary with
  applied voltage.
• Active tuning may be needed.
• Stanford will use existing Antenna-In-Plasma
  (AIP) code to determine sheath effects on
  radiation process and validate using UCLA LAPD.
• MURI Task Status
• Stanford group has made a number of visits to the
  UCLA LAPD to assist in setting up the experiments
  necessary to validate the AIP code.
• Preliminary impedance and pattern measurements
  have been obtained.
• Stanford has begun simulating near-field
  properties of dipole antennas operating in
  conditions representative of LAPD environment.

7
Alpha Field Tests (M.Golkowski)

• Wave Injection at Low Latitudes
• Investigate wave injection from Russian Alpha
  Navigation transmitter in Komsomolsk, Russia
• Observe 1-hop signals at Conjugate point in
  Adelaide Australia
• Results show growth and variation with
  geomagnetic conditions

8
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF UM - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Field Experiment Lab Experiment Theory Data
Analysis
9
Ducts From Streltsov et al.
Low density duct
High density ducts
No duct
Asymmetric Ducts
10
Plasmaspheric ducts formation (E. Mishin)
Why should one care? Necessary for
VLF triggering
APPROACH Compare plasmaspheric structures with
electric fields in the ring current-plasmasphere
overlap (Sub Auroral Polarization Streams Ion
Drifts)
Plasmaspheric ducts created by the SAPS Wave
Structures (left) during the substorm ring
current injection event from CRRES
11
Artificial Ducts Driven by F-Region Heating (G.
Milikh)
2D MODELING SHOWING S THAT TRANSIONOSPHERIC DUCTS
WITH dn/ngt .5 FORM IN 15 MINUTES WITH FULL HAARP
F-REGION HEATING
12
O-mode, 3.2 MHz .1 Hz Modulation Detection by
DEMETER 650 km altitude
13
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
14
TOWARD PREDICTING VLF TRIGGERING (E. Mishin A.
Gibby )
APPROACH Compare the occurrence of VLF triggering
from the Siple transmitter with the magnetic
activity and background hiss and chorus emissions
Database Siple June 1986 campaign

• Most favorable conditions for VLF triggering in
  the morning sector seem to be satisfied after
  weak/moderate substorms.
• The triggering occurred when broad-band hiss
  emissions were present and the pump frequency was
  above the top of the hiss band.
• Consistent with the step-like background electron
  distribution.

15
Propagation/Amplification (A. Streltsov)
New simulation code describes dynamics of
propagation and amplification of 1 kHz (20 mscec
pulse) along entire L4.2 line with spatial
resolution of 1 km. How to maximize injected
whistler amplitude
16
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
17
Whistler Amplification and Stimulated
Emission NRL / Maryland collaboration
Personnel Martin Lampe, NRL Dennis
Papadopoulos, U M Steve Slinker, NRL Glenn
Joyce, U M Guru Ganguli, NRL Wally
Manheimer, U M

• Major accomplishments
• HEMPIC code development (quasineutral
  eliminates c, wp timescales ? very fast)
• Theory and simulation of ducting (with Anatoly
  Streltsov)
• Theory and simulation of whistler growth in
  homogeneous systems
• Nonlinear amplification of wave packets
  propagating along the earth's dipole field
• - Wave growth driven by resonant electrons
  propagating toward equator
• - Large frequency shifts (triggering of fallers)
• - Extensive simulation studies, theory in progress

18
HEMPIC SIMULATIONS OF WHISTLER INSTABILITY

• Realistic non-uniform geomagnetic field
• Single-frequency wave packet (bounded in space)
  initiated at t0
• Fast electron distribution ring distribution of
  constants of the motion v2 and v-2/ B0(z)
• Inflow of fresh electrons from the boundary of
  the simulation domain

V?
V? 0
Electron distribution
V
V 0
cold electrons
fast electrons
19
EVOLUTION OF WAVE AMPLITUDE B- and ELECTRON
MOMENTUM p-
20
WAVE FREQUENCY EVOLUTION
Dashed line indicates the angular frequency
w1200 sec1 that is initiated at t0
21
AN OUTLINE OF THE PHYSICS

• For a ring distribution and a single frequency
  wave,
• electrons are resonant at two discrete
  locations, one on each side of the equator.
• Wave propagates to right, resonant electrons
  propagate (at a much larger velocity) to left.
• Wave initially grows at each of these resonant
  points.
• Resonant electrons are strongly phase-bunched at
  each resonant point.
• As these bunched electrons propagate to the
  left,
• they drive waves, at lower frequency than the
  initial triggering wave.
• Electrons propagating toward the equator lose
  energy and drive wave growth.
• Electrons propagating away from the equator gain
  energy and damp the waves.
• Resonant electrons remain resonant for a long
  time, because
• the wave frequency adjusts to the changing
  magnetic field, so as to maintain resonance.
• However very few electrons are phase trapped.
• The unstable waves are triggered by resonant
  untrapped electrons.

22
WHISTLER INSTABILITY STUDIES NEXT STEPS

• Physics
• More realistic thermal, anisotropic and loss cone
  electron distributions
• Can a large-amplitude injected wave grossly
  modify the
• electron phase-space distribution so as to
  trigger rapid growth of new waves?
• Instability of obliquely-propagating waves and
  2-D mode spectra
• Instability of ducted whistlers in 2-D
• Code development
• Will need to parallelize the HEMPIC code (very
  easy)
• Further code development may be necessary. Can
  use Dt gtgt 1/W and Dx gtgt 1/l by
• - Expanding fields in linear normal modes. Very
  efficient if not too many modes needed.
• - For the particle kinetics, writing eqs for the
  deviation from unperturbed gyro motion.
• Using the mode expansion, these eqs can be
  integrated with long time steps.

23
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
24
Electron loss in the inner magnetosphere

• Observations of LEP events using DEMETER and
  worldwide VLF observations. Burst mode
  observations over active thunderstorms (U. Inan)
• WIPP Code Issues (P. Kulkarni)
• What is the precipitation induced by ground-based
  VLF
• transmitters?
• What factor affects most strongly induced
  precipitation Source location, operating
  frequency or radiated power
• Tentative Results
• The NWC transmitter in Australia induces the most
  gt100 keV
• precipitation of the existing ground-based
  VLF sources
• Source location, much more than operating
  frequency or
• radiated power, determines energetic electron
  precipitation

25
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
VLF
LHW SU
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
26
Proton (gt 80 MeV) Belt Dynamics (1979-2005)
(from NOAA 5-14 POES Satellites)
26 years

• Only one (peak near L1.5 ) Proton Belt.
• Stably Trapped for centuries !!

27
South Atlantic Anomaly
Over the south Atlantic, the inner proton belt is
closest to the surface Protons in this region are
the largest radiation source for LEO satellites
28
Compared to HANE Remediation

• Proton remediation can be done much more slowly
• Years instead of weeks to remove particles
• Particles take decades or centuries to return
• Because it can be done more slowly, it may be
  cheaper and easier
• Proton remediation would have immediate
  operational impact

29
T. Bell
30
SAW Proton Precipitation (X. Shao)
L1.5
Input power required for ltbgt25 pT at few Hz at
L1.5 is 600 Watts per DL/L?.1
31
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
VLF/ULF
RMF SU - UCLA
HAARP F-Region UM
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
EMIC UM
ULF
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
32
Electron Precipitation by ULF waves (X. Shao)
At resonance I can have reflection or absorption
or mode conversion or tunneling. What is R in our
case?
33
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
ULF
EMIC UM
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
34
NOVEL WAVE INJECTION CONCEPTSNEUTRAL GAS
INJECTION
USE ENERGY (30 GJ/Ton) STORED IN RELEASING A
LARGE AMOUNT OF LOW IONIZATION POTENTIAL GAS
(e.g. Li) AT ORBITAL VELOCITY TO GENERATE THE
RESONANT WAVES GANGULI ET AL (2007)
RELEASE
PHOTO IONIZATION

• CONVERSION EFICIENCY FROM FREE ENERGY TO
  RESONANT SPECTRAL ENERGY
• SATURATION LEVEL OF PRIMARY ALFVEN ION CYCLOTRON
  INSTABILITY VT

35
Li Instability Study (J.Wang and W. Scale)
36
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
ULF
EMIC UM
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
37
Ways to Create RMF
The RMF can be generated either by a pair of
poly-phase coils, superconducting or else, or
rotating permanent magnet.
Mech to em energy
RMF driven by mechanically rotating permanent
magnet
RMF driven by two orthogonal phase-delayed
current loops
Oblique Rotator
A. Karavaev, X. Shao, N. Gumerov, G. Joyce UCLA
38
Setup for the Experiments
Device used to create RMF in LAPD
Two independent coils 4 turns each Operation
frequencies 50ltflt500 kHz Current magnitude 100
300 A
39
Configurations to Compare Theoretical and
Computational Results
Case 1
2 wires
w W/10
Dipoles
Case 2
4 wires
Rotating Field
Case 3
x
I0sin(wt)
I0cos(wt)
- I0cos(wt)
z
-I0sin(wt)
40
RMF Basics

• Modifies background magnetic field
• Dependence on n
• Hall term allows field penetration into the
  plasma
• Oscillating collisionless skin depth

Axial Screen Current Jz
Induces Azimuthal E? field
Hall Term
Pondermotive force
41
Setup for the Experiments
Large Plasma Device (LAPD), University of
California, Los Angeles

• Over 450 access ports
• Computer controlled data acquisition system
• Microwave interferometers
• Laser induced fluorescence
• DC Magnetic field 0.05 4 kG, variable on axis
• Highly ionized plasmas up to n5x1012 cm-3
• Plasma column up to 2000Rci across diameter
• Highly reproducible plasma with 1 Hz operation
  frequency

42
Computational Model for 2D/3D Whistlers
HEMPIC Algorithm 1). 3rd order
Predictor-Corrector in time 2). FFT-based solver
for elliptic equations 3). FFT-based spatial
differentiation/convolution to compute the
nonlinear terms
y
x
Lx
B0
z
Lz
Typical Settings Domain Size Lx 80
(c/wpc) 12.5 l Lz 160 (c/wpc) 25 l Grid
Nx 128, Nz 256 Time step ht
1/(10W) Max time tmax 100/W
For a serial CPU code running on PC 1 timestep
takes about 0.7 seconds (1000 time steps 12
min). (For 3D problem on grid 64x64x128 1
timestep takes about 45 seconds (1000 time steps
12.5 hours). Our goal is to reduce this time
by orders of magnitude to enable computation of
larger 2D and 3D problems for reasonable time. To
enable this we will use Graphical Processing
Units (GPU), which realize massively parallel
computing in the scale of PC and algorithmic
improvements (advancing in time in the Fourier
space, use of Adams-type methods,
finite-difference approximations for nonlinear
terms, etc.).
43
Setup for the Experiments
Ambient magnetic field along the chamber
Source position
n7.0x1011 cm-3
n4.5x1010 cm-3
Input currents

• Background magnetic field
• 50 Gauss
• 200 Gauss
• Two nearly identical currents with phase shift
  p/2
• Frequency f292 kHz (Oilt?ltltOeltlt?pe)

44
Two-Loop Antenna vs. One-Loop Antenna
Current Jz along ambient magnetic field at t1 and
t2
One loop experiment
Two loops experiment
( , where T is the oscillating
period) One-loop Jz current just oscillates
around 0 with frequency ?. Two-loop Jz always
has non-vanishing amplitude and rotates with the
magnetic field about z-axis.
The graphs are in the same scale.
45
Two-Loop Antenna vs. Single-Loop Antenna in
Magnetized Plasma
One loop antenna The magnitude of magnetic field
oscillates (reaching 0) at twice the rotation
frequency Two loops antenna While x and y
components of magnetic field oscillate, the
magnitude of magnetic field was kept at 0.2-0.4
G. Magnetic field vector rotates around z-axes.
Time dependence of magnetic field at the central
point of xy-plane (Port 33)
One-Loop antenna
t2
t1
Two-Loop antenna
46
Dependence of Induced Magnetic Field on number
density
Modeling shows that the pertiurbed magnetic field
depends on n That is dBn1/2. Validated by
experiment. Can we improve antenna efficiency by
injecting plasma ?
From experiment and
- good agreement with models
Experiment 2 N 7x1011 cm-3
Experiment 1 N4.5x1010 cm-3
Time dependence of magnetic field at central
point of xy-plane (Port 33) for twoloop antenna
in plasma with different plasma densities
47
RMF Modeling
Numerical (Wt 100)
Ey
w W/10
z
x
x
Ey
Theory predicts that the result has reflection
asymmetry about the axis.
z
48
Case 1
Numerical (Wt 100)
Ey
w W/10
z
x
Analytical Integral (stationary)
Ey
Real Part
Theory predicts a maximum on the axis.
Imaginary Part
49
Case 2
Numerical (Wt 100)
Ey
w W/10
z
x
x
Ey
z
Theory predicts a null on the axis.
50
Magnetic field configuration for some moment of
time for ambient magnetic field 50 Gauss
Experiments Results
P27 2.9 m
P31 1.6 m
P32 1.3 m
P33 1 m
p35
51
RMF LAPD exp2 1coil 50G
52
RMF LAPD exp2 2coil 50G
53
Spatial Decay Rates
Decay rate across ambient magnetic field lines
(port 33)
Hall term allows enhanced penetration
Total magnetic field across ambient magnetic
filed line
Decay rate along ambient magnetic field lines
n4.5x1010cm-3
N 7x1011 cm-3
n7.x1011cm-3
N4.5x1010 cm-3
54
Bx Amplitude
Pointing Flux
single loop
2 loops pi/2
2 loops -pi/2
2 loops pi
55
Alfven Wave Generation with Rotating Magnetic
Field (MHD Simulation)
Bz0
Bf
O
Bf
O
n0
O(t)
Constant O
Modulated O(t)
56
Alfven Wave Generation with Modulated Rotating
Magnetic Field (MHD Simulation)
Poynting Fluxes S( n 10 n0) 2?S( n n0)
Bz0
n n0
n 10n0
Bf/Bz0
Bf/Bz0
n n0
n n0
n 10n0
n0
O(t)
Z/?0
n
Z/?0
Bf/Bz0
Vf/VA0
r/?0
r/?0
57
Conclusion

• Demonstrated concepts of new type RMF-based
  antenna/active device for space applications .
• Differences between two-loop and classic
  one-loop antenna
• Two-loop antenna produces RMF and drives
  non-vanishing current along ambient magnetic
  field.
• Induced magnetic field by RMF is proportional to
  plasma frequency (?ltlt?p). That is dBn1/2.
• Spatial decay rate for the perturbation
  propagating across magnetic field much larger
  than c/we
• Second-Order analysis shows excitation of
  azimuthal current perpendicular to the ambient
  magnetic field. This current helps perturbation
  penetrate deep into surrounding plasma.

58
Future Work

• Developing 3D semi-analytical model and 3D EMHD
  code to model RMF-induced whistler-mode wave
  propagation along magnetic field lines. Use the
  model to guide and explain experiments.
• Conducting experiments with various parameters
  (e.g. plasma density, background magnetic field,
  and driving current magnitude), tilted rotating
  magnetic field, locally increased density by
  laser pulse or electron beam
• Conducting experiments with finer spatial
  resolution along ambient magnetic field to
  investigate second-order phenomenon.
• Use simulation to investigate parameter regime
  with perturbed magnetic field larger than ambient
  magnetic field.
• Study energetic particles interaction with RMF

59
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
ULF
EMIC UM
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
60
HAARP ULF Generation
F-region generation does not require ejet
current. Can be located anywhere and operated
continuously. Drives Msonic wave while ejet
modulation drives SAW
Cash et al. 2006
G. Milikh, H. Schroff UM D.Piddyachiy, U.Inan
SU C.Chang, T.Wallace BAE M. Parrot CNRS
61
ULF Signals at Gakona and Juneau
At Juneau wave evanescent 1/R2
IAR
62
SAW detection by DEMETER
Detection time lt 30 sec
63
Msonic wave detection by DEMETER
No ground signals detected
Detection timegt120 sec
64
PSD
Injected ULF power approximately 5-10 kW
65
Msonic wave detection by DEMETER
Detection time gt 100 sec
66
Msonic ground detection in Arecibo
B
S. Ganguly, W. Gordon and K. Papadopoulos PRL 1986
67
Can we drive whistlers with F-region heating?
B. Eliasson K. Papadopoulos
Bill Bristow UAL
68
Space Based
Ground Based
Radiation/Injection
AIP Code Validation SU - UCLA
VLF
Alpha Field Tests SU
RMF SU - UCLA
HAARP F-Region UM
VLF/ULF
Neutral Gas Injection VT
ULF
RMF - HED UM
Propagation
VLF
Natural Ducts BC
Artificial Ducts UM
Amplification
VLF
ASE Triggering - Siple Data BC - SU - DC
ASE Triggering Modeling NRL - UM
Protons
Precipitation
Electrons
LEP SU
LHW SU
VLF
WIPP SU
ULF
EMIC UM
Alfven Waves UM
Field Experiment Lab Experiment Theory Data
Analysis
69
Energetic Proton Removal
Pitch Angle Diffusion Coefficient for Protons at
1 Hz
ltbgt 1 pT
Need1-3 Hz to resonate with 30-100 MeV protons at
L1.5
Scale D at ltbgt 1pT to get lifetime at larger ltbgt
Lifetime vs. ltbgt
L1.5
ltbgt25 pT V 2x1020 m3 Wltbgt2/2?
?3x10-16J/m3 Total Energy 60 kJ Tconf 100-200
sec Power 300-600 Watts
days
Pick lifetime of 103 days and get power needed
1000
reflection
R .90-.95
ltbgt pT
70
Ground Based Antenna Choice

• VED minimal injection

For HMD P300 (M/1010 A-m2)2 Watts
For VMD P(300/4) (M/1010 A-m 2)2 (d/75 km)2
Watts
What about HED ?
HMD
VMD
HED
VED
PIL
M
M
71
Innovative Antenna Design
To inject 600 W we require ltbgt20-25 pT at 75 km,
the bottom of the magnetized ionosphere.
120 km
Rotating Magnetic Field A
superconducting magnet rotating at ULF frequency
has an image in phase and increases its power by
a factor of 4. This innovative antenna design can
give the required 600 W with a magnetic moment of
1010 A-m2
A1010 m2
ltbgt
75 km
R
B
72
Superconducting RMF

• Rotating superconducting magnets are useful for
  frequencies of up to 10 Hz
• They are compact sources of large moments and can
  be used in arrays
• Example design
• Superconducting coil 5 m high x 5 m wide x 5 m
  long
• 25 m2 area
• 100 Amps DC current
• 4 x 104 turns
• M 108 A-m2
• In LTS wire (2/kA-m) this could be a few million
  dollars including Dewar, He refrigeration, and
  rotation (HTS wire is still 50/kA-m, Cu now
  100/kA-m)

73
What about Tesla Technology HED Revisited
Resistive impedance dominates if
Traditional HED antennae operate in the reactive
impedance region
74
Point HED Design
1 km
75
Supplementary Slides
76
Energy Power Requirements
Total energy E Volumex(b2/2m)20 (b/20 pT)2
kJ Power required PE/T 300 (b/20 pT)2 (60
sec/T) Watts
P300 (M/1010 A-m2) Watts
(5/75)2
4
PIL
M
M
77
Key Points

• First observation of Magnetosonic waves in the
  Pc1 range generated by modulated ionospheric
  heating using the HAARP heater
• Msonic waves generated by modulated collisionless
  F-region electron heating and are independent of
  the presence of elctrojet currents
• Detection by the Demeter satellite flying over
  HAARP indicate ULF power in excess of 5 kW

78
The Fundamentals

• For Pc1 frequencies (.1-7 Hz) the ionosphere
  behaves as
• A resonator for Shear Alfven (SA) waves,
  confined along the B lines with an almost
  vertical structure at high latitudes
• A waveguide for Magnetosonic (MS) waves
  propagating isotropically and ducted horizontally
  over long distances

79
SA Waves Ionospheric Alfven Resonator (IAR)
SA wave is guided along the B field Reflections
create standing wave structure
Notice bB0
Natural SA waves
80
MS (Compressional) Waves Alfvenic Duct
Isotropic Mode
Notice b parallel to B
81
ULF Generation by Ejet Modulation
SA waves do not Excite Ionospheric Duct
D/E region heating Electrojet
Evanescent in EI Waveguide

• Ejet modulation cannot drive b field parallel to
  ambient B. This type of modulation can create
  only SA waves. The waves cannot propagate
  laterally since they are evanescent in the
  Earth-Ionosphere Waveguide and do not couple to
  the Alfvenic Duct
• SA waves can be detected (a) In the near zone
  below the heated spot and (b) By satellites
  over-flying the heated spot but confined to the
  magnetic flux tube that spans the heated spot.

82
ULF Signals at Juneau

• 28 April, 2007 UTC 050100 050545
• Detected 1 Hz 3 Hz peaks
• Amplitudes at 1 Hz 0.28 pT NS 0.23 pT EW

EVANESCENT
83
IAR Excitation - HAARP
84
Satellite SA Detection - EISCAT
Few Watts
(Wright et al., J. Geophys. Res., 2003)
85
F-Region Msonic ULF Generation
Collisionless upper hybrid F-region modulated
heating results in Dp exp(iwt) that drives a b
exp(iwt) with having a component parallel to B (a
msonic mode). The wave propagates isotropically
but is reflected at the D/E region and is much
weaker on the ground. It can be measured by
satellites or at large lateral distances (skip
zone)
b/B?b (Dp/p)?b
Vr
MHD Simulation
86
Example of F-Region Msonic Generation Detected by
the Demeter satellite
O-mode at 4.4 MHz HAARP at 3.5 MW modulated at .1
Hz between 64730 and 65930 UT
No ejet
Demeter pass
No D/E region
No ULF detection on the ground - .1 Hz detection
at Demeter between 65130 and 65300
87
Example 08/24/07 3.3 MHz O-mode .2 Hz
PSD
Demeter Trajectory
88
SA vs Msonic Detection
4 sec vs 90 secs
89
Life Time and Equilibrium Equatorial Particle
Flux Distribution
Equilibrium Distribution Function g(a0) Vs.
Pitch Angle a0
f0 6 Hz, df 0.7 f0
90
Basic Equations for Quasineutral Cold Fluid
Electron Plasma Simulations
Assumptions 1). Stationary ions 2). Negligible
displacement current.
Computational model (Lampe et al. JCP 214(2006)
284-298)
Evolution equation
Elliptic equations for each time step
(Electron plasma frequency)
(Electron cyclotron frequency)