effects of coronal mass ejections and solar wind streams on the earth’s radiation belts
DESCRIPTION
Effects of Coronal Mass Ejections and Solar Wind Streams on the Earth’s Radiation Belts. D.N. Baker , S. Kanekal, X. Li, S. Elkington Laboratory for Atmospheric and Space Physics Department of Astrophysical and Planetary Sciences University of Colorado - Boulder. Adiabatic Invariants. - PowerPoint PPT PresentationTRANSCRIPT
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Effects of Coronal Mass Ejections and Solar Wind Streams on the Earth’s
Radiation BeltsD.N. Baker, S. Kanekal, X. Li, S. Elkington
Laboratory for Atmospheric and Space Physics
Department of Astrophysical and Planetary Sciences
University of Colorado - Boulder
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Adiabatic Invariants
• M: perpendicular motion
• K: parallel motion
• L: radial distance of eq-crossing in a dipole field
Associated with each motion is a corresponding adiabatic invariant:
If the fields guiding the particle change slowly compared to the characteristic motion, the corresponding invariant is conserved.
•Gyro: M=p2/2m0B•Bounce: K•Drift: L
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The Earth’s Radiation Belts
Contours of the omnidirectional flux (particles per square centimeter per second) of protons with energies greater than 10 MeV
Contours of the omnidirectional flux of electrons with energies greater than 0.5 MeV
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TOPEX (1992-1998) and TERRA-MODIS (2001)
The South Atlantic Anomaly Region
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Solar Activity Cycle
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The Disturbed Solar Wind: Coronal Mass Ejections (CMEs)
• Occur most often near the peak of the Sun’s 11-year activity cycle
• Propel >109 tons of matter into interplanetary space
• Can travel at speeds exceeding 2000 km/s
• Drive interplanetary shocks• Can trigger geomagnetic
storms when they impact Earth’s magnetosphere
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Coronal Mass Ejection - Earth ImpactC
ourt
esy
of N
AS
A
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Impulsive Injection Due to Shock Wave
[Li et al., 1993]
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Outer Belt Electrons: 1992-2002
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Mapping of the Radiation Belt
SAMPEX: 18 August 1993
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Dynamic Radiation Belts: 1993-1995
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Acceleration by Radial Transport
30
L
MBW
Nonrelativistically, and in a dipole,
or
0
3
0
2
2 B
WL
Bm
pM
so transport in L while conserving M willnecessarily lead to change in energy, W.
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Transport in M, K: Local Heating
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Local Heating Example:Resonant Interactions with VLF Waves
• Whistler mode chorus at dawn combined with EMIC interactions heat and isotropize particles
• Leads to transport in M, K, and L
Summers et al. (JGR 103, 20487, 1998) proposed that resonant interactions with VLF waves could heat particles:
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MHD Simulations of ULF Power, 09/24/1998
• ULF power in MHD shows expected radial, frequency dependence
• Azimuthal dependence: frequently see structure in local time
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Shear Waves and Particle Acceleration
• Limited local time: propagating waves dusk and counterpropagating waves dawn still lead to energization
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MHD Simulation of a Strong Storm
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MHD/Particle Simulations of Energetic Electron Trapping
• 60 keV test electrons, constant M
• Started 20 RE downtail, 15s intervals
• Evolves naturally under MHD E and B fields
• Removed from simulation at magnetopause
• Color coded by energy
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LWS CDAW Workshop 14 March 2005High-Energy Electrons
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High-Energy Electrons: Deep-Dielectric Charging
3. Influx of electrons increases to levels higher than the leakage rate
2. Electrons slowly leak out of the insulator
1. Electrons bury themselves in the insulator 4. Electrons build up faster than they leak off
5. Discharge (electrical spark) that damages or destroys the material
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Star Tracker Anomalies at GEO
0
5
10
15
20
25
600 700 800 900 1000 1100 1200
Ele
ctro
ns/c
m2-s
-sr-
keV
Days from 1 January 1979
1.4 - 2.0 MeV Electrons
Geostationary OrbitStar Tracker Upsets
1980 1981 1982
Baker et al. (1987)
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Probability of discharges goes up dramatically with increasing electron fluence.
Anomalies Due to Dielectric Charging
Vampola (1977)
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1020
1021
1022
1023
1024
Radiation Belt Content Index
Tota
l Num
ber
of E
lect
rons
Year92 94 96 98 00 02
2.5 < L < 6.5E > 2 MeV
[Derived from SAMPEX / ELO]
Radiation Belt Content Index
• Gives a single “Radiation Belt Electron content” Index (RBI)
• Idea introduced in Baker et al. (1999)
• Integrates over energy spectrum and 2.5 < L < 6.5
1019
1020
1021
1022
1023
1024
.01 .1 1 5 10 20 30 50 70 80 90 95 99 99.9 99.99
Cumulative Probability
Rad
iatio
n B
elt I
ndex
Percent
Log-normal Gaussian Fit
Probability Distribution2.5 < L < 6.5 [ Derive from SAMPEX]
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300
400
500
600
700
800
1020
1021
1022
1023
1024
Sol
ar W
ind
Spe
ed [k
m/s
] Radiation B
elt Index
Year
1992 1995 1998 2001
E > 2 MeV Electrons2.5 < L < 6.5
Vsw
[OMNITAPE]27-day Running Averages
RBI-Solar Wind Speed Comparison
• Many operational anomalies in 1994 period
• Late 1993 and early 1994 were remarkable times for VSW
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ANIK Failures: Deep-Dielectric Charging
1020
1021
1022
1023
1024Total Radiation Belt Content Index
Tota
l Num
ber
of E
lect
rons
Year
1992 1994 1996 1998 2000 2002
E > 2 MeV[Derived from SAMPEX / ELO] 2.5 < L < 6.5
27-day Running Average
ANIK Anomalies
ANIK/Intelsat failures in January1994 occurredduring the highestradiation beltcontent intervalof the last decade
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The RBI Allows Averaging and Superposition
• Builds on idea of radiation belt “coherence”
• Annual and seasonal averaging is readily done
• Gives a true global view
0
2
4
6
8
10
12
14
16
1992 1993 1994 1995 1996 1997 1998 1999 2000 2001
Nu
mb
er o
f E
lect
ron
s (
X 1
0-2
2)
Year
E > 2 MeV 2.5 < L < 6.5Outer Radiation Belt
2003 2005 2007 2009 2011
Years of Next Cycle (+ 11 Years):
0.0
0.5
1.0
1.5
2.0
Seasonal Average Fluxes : 1992 - 1999
No
rmai
lize
d E
lec
tro
n F
lux
February - April
May - July
August -October
November - January
SAMPEX Electrons 2.5 < L < 6.5 2 - 6 MeV
Spring
Summer
Fall
Winter
Baker et al., GRL (1999)
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10-1
100
101
100
101
102
1992 1993 1994 1995 1996 1997 1998 1999
Annual Relativistic Electron Acceleration Efficiency
Pow
er [x
10
-9 W
] Efficiency [x 10
-3]
Year
Electron (E > 0.5 MeV) Power 2.5 < L < 6.5
Solar Wind Input Power
( < > x 10-2 )
Relativistic ElectronProduction Efficiency
Radiation Belt Content : POLAR/SAMPEX
Baker et al., JGR (2001)
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October 2003 Events
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The Halloween Storm in the Heliosphere
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D. N
. Bak
er e
t al.,
Nat
ure,
16
Dec
200
4
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KODAMA, Mars Odyssey
Spacecraft Anomalies: October-November
Genesis
ADEOS-2, Stardust, Chandra, Various GOES
RHESSI INTEGRAL, Chandra, SMART-1
NOAA-17
POLAR
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Day-to-Day Variation of the Radiation Belts
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Selected Days: Outer Belt Properties
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30.4 nm EUV
(Cou
rtes
y of
J. G
olds
tein
)
Resonant Scattering
Plasmasphere
He+ 15%
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EUV Images of the Plasmasphere
Plasmasphere
He+ 15%
plasmasphere
Global EUV He+ Image
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Extreme Plasmasphere Erosion
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D. N. Baker et al., Nature, 16 Dec 2004
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Regions of Wave-Particle Interactions
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X-28 Class Flare
SEP
Fast CME, 2657 km/s
Glancing Blow
Largest Flare in Recorded History, Extremely Fast CME - Narrow Miss at Earth