dynamics of the radiation belts & the ring current
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Dynamics of the Radiation Belts & the Ring Current. Ioannis A. Daglis Institute for Space Applications Athens. Dynamics of the near-space particle radiation environment. Main issue: mechanism(s) that can efficiently accelerate and/or transport charged particles, leading to - PowerPoint PPT PresentationTRANSCRIPT
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Dynamics ofthe Radiation Belts &
the Ring Current
Ioannis A. DaglisInstitute for Space Applications
Athens
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Dynamics of the near-space particle radiation environment
Main issue: mechanism(s) that can efficiently accelerate and/or transport charged particles, leading to
-build-up of storm-time ring current
-enhanced fluxes of MeV radiation belt electrons.
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Dynamics of the near-space particle radiation environment
In both cases, the most obvious driver
the magnetospheric substorm
appears to be insufficient
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Dynamics of Radiation Belts
Substorms produce electrons with
energies of 10s to 100s of keV,
but only few of MeV energies.
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Dynamics of Ring Current
(Individual) Substorms inject plenty of hot ions
to the inner magnetosphere,
but not enough to create/sustain
the ring current.
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Dynamics of the near-space particle radiation environment
Presumably, the ring current build-
up and the radiation belt enhancement,
being processes of a higher level of
complexity,display properties not
evident at the lower levels
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Dynamics of Radiation Belts
Close association
of storm-time enhancements of relativistic electron fluxes
with spacecraft failure.
Spacecraft operational anomalies, SAMPEX data[Baker & Daglis, 2006]
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Dynamics of Radiation Belts
Each new mission in the inner MS brings new insights (SAMPEX, CRRES)
Close correlation with storms / Large dynamic range: 10 to 10^4 (Li et al. 2001).
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Location of the peak electron flux as a function of minimum Dst moves to lower L
O’Brien et al., JGR2003
Dynamics of Radiation Belts
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Association of MeV electrons with ULF waves / radial diffusion [Baker and Daglis, 2006]
Dynamics of Radiation Belts
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Gre
en a
nd K
ivel
son,
200
4 –
Pol
ar/H
IST
dat
a 19
97-1
999
Dynamics of Radiation Belts – Internal/external
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300-500 keV 1.1-1.5 MeV300-500 keV 1.1-1.5 MeV
Dst
Kp
GEO
GPS
1.22 MeVequatorial flux
(L=4.2)
MeV Electron Flux evolution after a Storm
Equatorial fluxes reach max in:- 2.5 days at GEO orbit- 16 hours at GPS orbit
Equatorial fluxes reach max in:- 2 days at GEO orbit- 6 days at GPS orbit
T=0 T=0
GPS max GPS max
GEO max GEO max
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Dynamics of Radiation Belts
[Va
ssili
ad
is e
t a
l., J
GR
20
02
]
Region P1: • Slow (2-3-day) response to hi-speed streams• Characteristic of GEO orbit• Prob. involves ULF waves• Representative study: Paulikas and Blake, 1979.
Region P0: • Rapid (<1-day) response to magnetic clouds/ICMEs.• Characterizes L<4.• Representative events: January 1997, May 1998: - Baker et al., GRL 1998; - Reeves et al., GRL 1998
September 5, 1995 (Solar Min)
May 4, 1998 (Solar Max)
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O’Brien et al., JGR2003 SAMPEX, HEO-3 data / SAMNET, IMAGE
Dynamics of Radiation Belts
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Both ULF waves and microbursts are strongest during the main phase of storms, both progress to lower L during stronger magnetic activity, both continue to be active during the recovery phase of events, and both appear to be more active during intervals of high solar wind velocity.
Dynamics of Radiation Belts
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Close to GEO, ULF-wave enhanced radial diffusion is more important, pushing electrons inward and accelerating them.
Around L~5, VLF chorus waves accelerate electrons (microbursts) without displacing them in L.
Dynamics of Radiation Belts
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1. Radial diffusion only:1. Radial diffusion only:
plasmapause
2100 MeV/G, equator, Kp =1.8
Iteration number
1025
1024
1023
1022
1021
1020
8
7
6
5
4
3
2
L
(MeV-3s-3) 2. Plus chorus waves:2. Plus chorus waves:1025
1024
1023
1022
1021
1020
Iteration number
plasmapause
8
7
6
5
4
3
2
L
2100 MeV/G, equator, Kp =1.8
(MeV-3s-3)
1 MeV
3 MeV
L
L=5.5:L=5.5:Values 100 times Values 100 times higher!higher!
1.E+20
1.E+21
1.E+22
1.E+23
1.E+24
1.E+25
1.E+26
3 4 5 6 7 8
Dis
trib
utio
n F
un
ctio
ns
(Me
V-3s-3
)
DLL and Chorus
DLL
Lpp
Varotsou et al.Varotsou et al.
Dynamics of Radiation Belts - Salammbô model
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Dynamics of Radiation Belts
Not simply a superposition, but a synergy of various lower-level processes (combined effect > sum of individual effects)- feature of the emergent order of higher levels of complexity
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Fully understand and specify
radiation belt variability
(CRRES, Bernie Blake)
Dynamics of Radiation Belts - Future
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Explain rapid acceleration of electrons to relativistic energies
Identify loss mechanismsDevelop accurate energetic electron
model
Dynamics of Radiation Belts - Future
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The classical ring concept
Image courtesy Hannu Koskinen, FMI
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Ring Current Dynamics
-RC sources (composition) / RC [a]symmetry
-RC formation: IMF driver-RC formation: role of substorms
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Ring Current Sources / Composition
Daglis, Magnetic Storms Monograph [1997]
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Fig. 6 of Daglis et al. JGR2003
Ring current asymmetry
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A very asymmetric ring current distribution during the main and early recovery phases of an intense storm
Near Dst minimum O+ becomes the dominant ion in agreement with previous observations of intense storms
Jordanova et al. [2003]
Ring Current Asymmetry & Ion Composition
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Ring Current Dynamics
-RC sources (composition) / RC [a]symmetry
-RC formation: IMF driver
-RC formation: role of substorms
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Ring Current Formation – IMF Driver
Empirical certainty:Prolonged southward IMF drives strong convection (westward Ey) and therefore storms.Large IMF Bs => intense storms.
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Modeling (RAM Code: Kozyra, Liemohn, et al.)
Comparative study of a solar-max and a solar-min intense
storms: IMF comparable. “Resulting” Dst different.
Ring Current Formation – IMF Driver
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Storm intensity defined by IMF Bs size and duration? Not exclusively!
Ring Current Formation – IMF Driver
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Ring Current Dynamics
-RC sources (composition) / RC [a]symmetry
-RC formation: IMF driver
-RC formation: role of substorms
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Ring Current Formation – Substorms
Role of substorms 1960s Chapman and Akasofu: storms =
cumulative result of substorms 1990s McPherron, Iyemori, et al.:
purely solar driven, no substorm influence
2000s Daglis, Metallinou, Fok, Ganushkina, et al.: substorms act as catalysts
Daglis [1997, 1999]
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Fig. 5 of Ganushkina et al., AnnGeo2005
Ganushkina et al. showed that the observed H+ acceleration at high energies can be reproduced in modeling studies only through substorm-style induced E pulses.
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Fig. 10 of Ganushkina et al., AnnGeo2005
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Substorm-induced transient electric
fields clearly contribute to particle
acceleration
Ring Current Formation – Substorms
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Ring Current Formation – Substorms
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Effect of recurrent (periodic) substorms
on particle acceleration
Ring Current Formation – Substorms
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Ring Current Formation – Substorms
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Ring Current Formation – Substorms
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Dynamics of Ring Current
Not simply a superposition, but a synergy of convection, substorm-induced electric fiels and wave-particle interactions (combined effect > sum of individual effects) - - a feature of the emergent order of higher levels of complexity
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The ring current is a very dynamic population, strongly coupling the inner magnetosphere with the ionosphere, which is an “increasingly important” source and modulator
IMF not the sole ruler: Plasma sheet density, ionospheric outflow, substorm occurrence, all have their role in storm development.
Summary RC
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Substorms act catalytically: they accelerate ions to high(er) energies/ they preferentially accelerate O+ ions, which dominate during intense storms.
Storms, being phenomena of a higher level of complexity display properties not evident at the lower levels (substorms / convection)
Summary RC
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Dynamics ofthe Radiation Belts &
the Ring Current
End
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RB models need better satellite measurements: Particle measurements with full pitch-angle information Comprehensive magnetic field measurementsWave measurementsParticle measurements in inner zone
Dynamics of Radiation Belts - Future
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Radiation belt modeling - Radiation belt modeling - ProblemsProblems
Known problems:Known problems: AE8 models overestimate electron doses: AE8 models overestimate electron doses:
shown by measurements in HEO, MEO shown by measurements in HEO, MEO orbits and by CRRES (Gussenhoven et al., orbits and by CRRES (Gussenhoven et al., 1992). Also by POLE model for GEO.1992). Also by POLE model for GEO.
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Radiation belt modeling - ProblemsKnown problems:Known problems: AE8 models do not specify lower AE8 models do not specify lower
energy environment. Low energy energy environment. Low energy electron (< 100 keV) flux intensity electron (< 100 keV) flux intensity much higher than extrapolation of AE much higher than extrapolation of AE spectra.spectra.
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Radiation belt modeling - Radiation belt modeling - ProblemsProblems
Known problems:Known problems: Magnetic field models are not accurate for Magnetic field models are not accurate for
disturbed timesdisturbed times Radial diffusion models: What is the source Radial diffusion models: What is the source
population? / Can r.d. transport particles population? / Can r.d. transport particles efficiently enough to low L?efficiently enough to low L?
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Ring Current Formation – IMF Driver
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May 4, 1998, medium energies (20-80 keV)
(a) (b)
(c) (d)
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May 4, 1998, high energies (80-200 keV)
(a) (b)
(c) (d)