high latitude scintillation analysis for marine and aviation...
TRANSCRIPT
High Latitude Scintillation Analysis for
Marine and Aviation Applications
F. Ghafoori and S. Skone
University of Calgary
2
Outline
• Auroral/polar scintillation mechanisms
• Scintillation data set
• Simulation tools
• Results
• Summary
Ionospheric Scintillation
Irregularities in
electron density
Wave propagation
Wavefront
Emerging
wavefront
0 10 20 30 40 50 60-1
-0.5
0
0.5
1
Time (Second)
Am
pli
tud
e (
dB
)
Realization of Amplitude @ f =1575 MHz
σχ=0.0359
0 10 20 30 40 50 60-1
-0.5
0
0.5
1
Time (Second)
Ph
ase
(R
ad
ian
)
Realization of Phase for Signal @ f =1575 MHz
σφ=0.31
3
4
High Latitude Scintillations
Polar Cap
Auroral Oval
Auroral Irregularities
E-region:
October 1, 2006
Polar Irregularities
E- & F-region:
January 7, 2005
7
The CANGIM receivers measure
• 50 Hz raw GPS observations
• Phase scintillation index (σ)
• Amplitude scintillation index (S4)
Calg
Athb
Yell
Sub-auroral
Station Geographic Geomagnetic
Lat. Long. Lat. Long.
Yell 62.48º -114.48º 68.80º 298.37º
Athb 54.72º -113.31º 61.52º 305.67º
Calg 51.08º -114.13º 57.86º 306.43º
Note: - The coverage areas for IPP above 20º
are indicated as circles.
CANGIM Database
To develop flexible tools to study high latitude
scintillation impact on receiver performance for
various user groups (marine, aviation)
Objective
Method
• Determine scintillation characteristics for auroral and polar regions (CANGIM)
• Develop simulation based on observed high latitude characteristics
• Develop flexible tracking loops to assess impact – determine thresholds for loss of lock
• Quantify duration and frequency of receiver impact, number of satellites affected, etc.
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Auroral Substorm Current Wedge
Magnetometer signature
9
10
00
12
06 18
Auroral Oval 08 : 00 UT
ESKIFCHUGILLISLL
PINA
RANK
TALO
135 ° W
120 ° W
105° W 90° W
75° W
60° W
45 ° N
60 ° N
75 ° N
Churchill Line --(CARISMA)
-500
-250
0
250
500TALO
H-Component
04:00 08:00 12:00 16:00 20:00 24:00-500
-250
0
250
500PINA
UT (Hours)
-500
-250
0
250
500ISLL
-500
-250
0
250
500GILL
-500
-250
0
250
500FCHU
20070928;
Polar Scintillation
Auroral Scintillation
Auroral Boundary Estimation
Event Selection
2002 2003 2004 2005 2006 20070
100
200
SS
N
Daily SSN variation
2003 2004 2005 2006 20070
200
400
Year
Number of Phase and Amplitude Scintillation >= 0.2 (Elevation Cutoff = 20o)
No
. o
f O
bs.
Aurora Phase Obs.
Polar Phase Obs.
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• Phase scintillation is dominant
• Low amplitude scintillation (S4<0.1) for all events
Auroral Scintillation Characteristics
Weak Scintillation Moderate Scintillation Strong Scintillation
[Yell], PRN29, 10-Jan-2003
0 0.5 1 1.50.04
0.045
0.05
0.055
0.06
0.065
0.07S
4
σφ60
[Yell], PRN25, 29-Oct-2003
0 0.5 1 1.50.02
0.03
0.04
0.05
0.06
0.07
S4
σφ60
0 0.5 1 1.5
0.03
0.04
0.05
0.06
0.07
S4
σφ60
[Yell], PRN23, 12-Feb-2003
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Polar Scintillation Characteristics
0 0.2 0.4 0.6 0.8 10
0.2
0.4
0.6
0.8
1
Phi 1Sec
Co
rr S
4
S4 and Phase Scintillation Correlation on 26 August 2005
• Amplitude scintillation is significant
• S4 in range 0.4 to 0.8 for severe events
• Pairs (σ, S4) determined for scintillation simulations
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0 200 400 600 800 1000 1200 1400 1600 1800 2000
-5
0
5
Representation of 2000 samples of the simulated GPS signal for PRN # 1, 3, 7 and 11 (without scintillation)
samples
2000 samples (PRN 1,3,7,11)
Discrete-time
VCO
Look-up table
C/A-code
System
dynamics
Cosine wave
1.023 MHz Counter C/A-code
Look-up
navigation data
Discrete-time
VCO
Counter navigation
period
Counter navigation
message
10.23 MHz
-3 dB
Q
I
Thermal
noise
GPS
signal
Navigation
message
Scintillation
Scintillation
System
dynamics
Sine wave
Multipath
Scintillation
Thermal noise
Multipath
System dynamics
Conventional
parameters for low-
cost receivers
GPS Signal Simulator
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Ionospheric phase scintillation follows zero-mean Gaussian distribution with
standard deviation σφ.
( ) βα
δ
αβ
βδδ /
1
/1
)()()( xIm
m
mm
ex
em
ImxIf
−
−
Ω−−
Γ=
ΩΓ==
1
,1
,1 2
42
4
=Ω
==== SmS
m βα
Nakagami-m Bivariate Gamma
22 2/
2
1)( φσφ
φσπφ
−= ef
Ionospheric intensity scintillation follows Nakagami-m distribution with normalized
standard deviation S4. The intensity scintillation signal can be generated using
bivariate gamma function G(α,β) with marginal density function given as follows:
Scintillation Simulator
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Digital IF
Carrier
wipe off
Code
wipe off
90°
Prompt replica
code
Phase
discriminator
F(s)
VCO
I
Q
Ip
Qp
Replica carrier
Integrate
and dump
1/T ∫dτ
1/T ∫dτ
Generic Costas Carrier Tracking Loop
Tracking loop bandwidth
Pre-detection integration time
Tracking Loops
16
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1
Time (sec)
σ (
rad
ian
s)
Total Error Std = 0.24461 (rad)
Ϭϕ60 = 0.1 radS4 = 0.05
Ϭϕ60 = 0.5 radS4 = 0.05
Ϭϕ60 = 0.7 radS4 = 0.05
Near the tracking threshold
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1
σ (
rad
ian
s)
Total Error Std = 0.19002 (rad)
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1φ60
σ (
rad
ian
s)
Total Error Std = 0.21559 (rad)
Weak Scintillation
Moderate Scintillation
Strong Scintillation
(Bn = 15 Hz, C/N0 = 46 dB-Hz)
Carrier Tracking Error Auroral Region
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1
σ (
radia
ns)
Total Error Std = 0.19918 (rad)
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1
σ (
radia
ns)
Total Error Std = 0.2065 (rad)
0 1 2 3 4 5 6 7 8 9 10-1
-0.5
0
0.5
1
Time (sec)
σ (
radia
ns)
Total Error Std = 0.22977 (rad)
σφ = 0.2 rad
S4 = 0.6
σφ = 0.4 rad
S4 = 0.6
σφ = 0.6 rad
S4 = 0.6
Near the tracking threshold
(Bn = 15 Hz, C/N0 = 46 dB-Hz)
Carrier Tracking Error Polar Region
Weak Scintillation
Moderate Scintillation
Strong Scintillation
Example: Loss of Lock
0 5 10 15 200
0.2
0.4
0.6
0.8
1
[Yellowknife 20-Oct-2003] σφ60
for all visible satellites
Time (hour)
60-s
econd p
hase s
igm
a
[Yellowknife 29-Oct-2003]
Threshold = 0.7
0 5 10 15 20
0
2
4
6
Number of satellites for which σφ60
threshold is exceeded simultaneously
Time (hour)
No.
of
sate
llite
s
Yellowknife 29-Oct-2003
v
Yellowknife
Auroral Polar
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Simultaneous Loss of Lock
0 1 2 3 4 50
200
400
600
800
1000
1200Yellowknife (29-Oct-2003) - Number of simultaneous loss of satellites
No. of Satellites
Num
ber
of
loss (
1-m
in m
easure
ment
epochs)
20
0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9
0.16
0.18
0.2
0.22
0.24
0.26
0.28Tracking Error (C/N0 = 46 dB-Hz, S4 = 0.06)
phase scintillation index (σφ)
trackin
g e
rror
(radia
ns)
Bn = 09 Hz
Bn = 11 Hz
Bn = 15 Hz
Bn = 25 Hz
Optimum loop
bandwidth is
around10-15 Hz.
(C/N0 = 46 dB-Hz, S4 = 0.06)
Optimal Tracking Loop Bandwidth
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Summary
• High latitude scintillations are due to different
physical drivers (auroral versus polar regions)
• Simulations developed for auroral and polar
regions
• Carrier tracking loop performance evaluated for
generic low-cost receiver
• Receiver tracking loops may be challenged during
severe scintillation
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