shine 2006 wg2/3 - cirs & energetic particles 1 review of cir-related particle composition,...
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SHINE 2006WG2/3 - CIRs & Energetic Particles
1
Review of CIR-related Particle Composition, Charge States, &
Energy SpectraJoe Mazur
The Aerospace Corporation
Glenn Mason
Johns Hopkins/APL
Joe Dwyer
Florida Institute of Technology
Mihir Desai
Southwest Research Institute
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After Stone et al., Space Sci Rev., 86, 1, 2000
Processes for 1 AU observationsof solar material
SolarPhotospheric
MaterialFractionation
CoronalMaterial
Solar WindAccelerationMechanism
CoronalMass
Ejections
SolarWind
InterplanetaryShock
Acceleration
Accelerationin CorotatingInt. Regions
Transportto 1 AU
Transportto 1 AU
SolarWind
Interpl.Shock
Particles
C I REvents
GradualSEP
Events
1 keV/nuc 1 MeV/nuc 1 GeV/nuc
SW
ISP
C I R
SEP
ShockAcceleration
by CMEs
ImpulsiveSolar Flare
Acceleration
Transportto 1 AU
ImpulsiveSEP
Events
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Desai et al., JGR, 104, 6705, 1999
10-6
10-4
10-2
100
102
104
339 340 341 342 343 344 345
Day of 1994
0.06 MeV/nucleon
0.24 0.95
1.93
2.85
5.6
EPACT / WIND
300
400
500
600
700
800
SWE / WIND
Mason et al., ApJ Letters, 486, L149, 1997
5 AU 1 AU
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4
0
0.05
0.1
0.15
0.2
0.25
149 150 151 152 153 154 day of 1995
Mg/O ratio
0.1
1
10
100
16O 70 keV/n
Vsw = 666 km/s
Stream interface
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5
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
350 400 450 500 550 600 650 700 750
C/O
Solar wind speed (km/s)
In ecliptic SW
Coronal hole SW
Mason et al., ApJ Letters, 486, L149, 1997see also Richardson et al., JGR 98, 13, 1993
Abundances
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0
0.05
0.1
0.15
0.2
350 400 450 500 550 600 650 700 750
Fe/O
Solar wind speed (km/s)
0
0.05
0.1
0.15
0.2
350 400 450 500 550 600 650 700 750
Si/O
Solar wind speed (km/s)
0
0.05
0.1
0.15
0.2
0.25
0.3
350 400 450 500 550 600 650 700 750
Mg/O
Solar wind speed (km/s)
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
350 400 450 500 550 600 650 700 750
Ne/O
Solar wind speed (km/s)
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
350 400 450 500 550 600 650 700 750
C/O
Solar wind speed (km/s)
In ecliptic SW
Coronal hole SW
50
100
150
200
350 400 450 500 550 600 650 700 750
He/O
Solar wind speed (km/s)
Coronal hole SW
In ecliptic SW
Ratios vs. solar wind speed
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Abundance summary
• similar to solar system except for factor of 2-3 enhancement of He and C/O
• increase of He/O, C/O, and Ne/O with solar wind speed
• He abundance increases from 1 to 5 AU
Mason & von Steiger et al. Space Sci. Rev. 89, 1999 (ISSI CIR Workshop held in 1998)
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Ulysses 4.5 AU
Gloeckler et al., JGR, 99, 17637, 1994.
10-9
10-7
10-5
10-3
10-1
101
103
105
107
109
1 10
F(W) Phase Space Density (s
3
/km6)
W Ion Speed (SC frame)/Vsw
HI-SCALE
SWICS
H+He+
He++
He
1991.292.0400-293.04004.485 AU
Pick up ion He+ increases its contribution to CIRs at greater radial distances
Suggested that other pickup ions (such as inner source) at 1 AU might account for some puzzling composition observations
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v’/Vsw1 0-4
1 0-2
1 00
1 02
1 04
1 06
1 1 0
H+
He+
He2+
CIR 1, F’
Chotoo et al., JGR, 105, 23107, 2000.
Acceleration of suprathermal He+
in CIRs: enhanced 103 - 104 over solar wind
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Mobius et al. Geophysical Research Letters, 29, 2001
Mazur et al. ApJ 566, 2002
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Mobius et al. Geophysical Research Letters, 29, 2001
Species SAMPEX ACE
He 2.00±0.12 -
C 4.83±0.27 5.1±0.3
O 6.12±0.37 6.1±0.35
Ne 7.25±0.25 7.8±0.5
Fe 13.00±0.48 10.5±0.6
Mazur et al. ApJ 566, 2002
Averaged CIR charge states: ~0.5 MeV/n
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Charge state summary
• More pickup He at 4.5 AU than 1 AI (at 1 AU the pickup He is ~15% He++, while at 4.5 AU it is twice as abundant)
• Heavy ions at 1 AU show little evidence of pickup species
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10-7
10-5
10-3
10-1
101
103
0.01 0.1 1 10
WIND/ STEP & LEMT - SAMPEX / LICA12/6/94 18:00 - 12/7/94 18:00
MeV/nucleon
H
HeCNO
Fe
Mason et al., ApJ Letters, 486, L149, 1997
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SummaryAbundances
Ion composition similar to solar system but with some differencesStill puzzling dependence of some ratios on solar wind speed
Charge statesLittle evidence of Z>2 pickup ions at 1 AULarge abundance of pickup helium at 5 AU
Energy spectraPower law from tens of keV/n to ~1 MeV/nSteepening above ~1 MeV/nSpectral forms do not change out to 10’s of AU
The source population is coming from the suprathermal region, but that population is not just heated solar wind; other constituents are important
Most often the 1 AU particles are not accelerated at shocks requiring another mechanism (Jokipii et al. 2003) As we approach solar minimum we have the opportunity to revisit some of these observables with ACE
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Essential new work needed:
• Complete ACE surveys with much larger number of species identified
• fully characterize properties of suprathermal / pick-up ion distributions
• detailed theoretical models to probe injection issues
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10-7
10-5
10-3
10-1
101
103
105
107
1 10
MASS, STICS, and STEPCIR 2: May 30, 1995 10:00-22:30 UT
Helium Spectra
V/Vsw (SC Frame)
MASS
STICS
STEP
C. Chotoo, Ph.D. thesis, U of Maryland 1998
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10 -39
10 -37
10 -35
10 -33
10 -31
10 -29
10 -27
10 -25
0.001 0.01 0.1 1 10 100
Fisk & Lee 1 AU spectral form vs. distance to shock
1 AU1.5 AU2 AU3 AU4 AU5 AU6 AU
Energy/n
Shock location:
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10-5
10-4
10-3
10-2
10-1
100
101
102
103
0.01 0.1 1 10
WIND/STEP Spectra5/30/95 9:39:04 to 5/31/95 14:19:28
MeV/nucleon
STEP C+N+O Flux
Fisk & Lee (1980) Spectral Form(numerical solution)
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Energy spectra summary
• power law from tens of keV/n to ~1 MeV/n• steepening above ~1 MeV/n• spectral forms do not change out to 10’s of AU
See also Mason & von Steiger et al. Space Sci. Rev. 89, 1999 (ISSI CIR Workshop held in 1998)
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Solar WindAccelerationMechanism
CoronalMass
Ejections
3He-rich Solar Flare
Accelelration
Slow SolarWind
TransientShock
Acceleration
CorotatingInt. Regions
Transportto 1 AU
Transportto 1 AU
SolarWind
ESPEvents
C I REvents
SolarPhotospheric
Material
Fractionation
CoronalMaterial
Fast SolarWind
InterstellarPick up
Ions
InnerSource(dust?)
Q = 1pick up
ions
Transportto 1 AU
3He-richSEP
Events
InterplanetarySuprathermal Ions
Transportto 1 AU
C M EAssocSEPs
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Energy spectra summary
• More pickup He at 4.5 AU than 1 AI (at 1 AU the pickup He is ~15% He++, while at 4.5 AU it is twice as abundant)
• Heavy ions at 1 AU show little evidence of pickup species
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C N Ne Mg Si S Fe0.01
0.10
1.00shock
CIR
solar wind
Dwyer et al, in preparation, 2002
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Fisk & Lee acceleration model--
• particles in CIRs accelerated by compression at forward and reverse shocks at several AU: propagate in to 1 AU
• adiabatic deceleration in solar wind included• yields distribution function spectra and gradients similar to
observations above ~100 keV/n• injection energy > 5 keV required, ie from postulated
suprathermal tail of the solar wind• composition similar to source material (assumed to be solar
wind suprathermal tail) -- (note: no systematic measurements of solar wind comp. available at that time)
L. A. Fisk and M. A. Lee, Astrophys. J., 237, 620, 1980
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Suprathermals as a seed population--
• SEP related events– “super events” in the inner solar-system (Dröge et al. 1992.)– Peak intensities in August 1972 (Smart et al. 1990)
• Interplanetary shocks– Aug 1978 shock (Gosling et al. 1981)
– IP shock survey (Tsurutani & Lin 1985)
• Sources?
– long lived remnants of solar flares
– planetary bow shocks
– corotating interaction regions
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Fisk & Lee CIR spectral form--
CIR spectral form:
where: v = particle speed; r = radius of observer; rs = shock radius;
= shock strength; diffusion coefficientV = solar wind speed
f =
r
rs
⎛
⎝
⎜⎞
⎠
⎟
2 / ( 1 − ) + V / ( o
v )
v− 3 / ( 1 − )
exp −
6 o
v
V ( 1 − )2
⎛
⎝
⎜⎞
⎠
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CIR model status 1970s-80s
• Successful:– spectra above ~100 keV/n
– composition “similar” to (unmeasured) solar wind
– origin at several AU, and gradients
• Not successful / unaddressed:– C/O ratio
– spectral forms vs. compression ratios
– intensities
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New CIR energetic particle observations & challenges to standard model--
• Particle spectra continue to rise down to ~10 keV/nucleon at 1 AU
• C/O ratio dependence on solar wind speed• Mg/O shows no FIP effect • large abundance of He+ at 1 and several AU• 3He abundance enhanced compared to solar wind
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Butter Garlic Croutons: Enriched unbleached flour (wheat flour, malted barley flour, niacin, reduced iron, thiamine mononitrate, riboflavin, folic acid), partially hydrogenated soybean oil, salt, high fructose corn syrup, corn syrup solids, yeast, salt, contains 2% or less of the following: whey, maltodextrin, wheat gluten, ascorbic acid, dough conditioners (sodium stearoyl lactylate, calcium stearoyl lactylate, calcium peroxide, calcium sulfate, ammonium sulfate, calcium iodate, ascorbic acid), garlic powder, dehydrated parsley, annatto (color), sugar, natural (vegetable and dairy source) and artificial flavors, butter oil, alpha-tocopherol (antioxidant), smoke flavor, enzymes, L-cysteine, TBHQ (to preserve freshness).
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0.05
0.1
0.15
pre-FS FS to SI SI to RS post-RS
Solar Wind Mg/O Abundance Variations in CIRsSWICS/ Ulysses: 15 CIRs (4.5 - 5.4 AU)
Mg/O
from: Wimmer-Schweingruber et al., JGR vol 102, 17407,1997
SHINE 2006WG2/3 - CIRs & Energetic Particles
34Hilchenbach et al., Trnas. Am.Geophys. U., 78, F554, 1997
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Interstellar Gas Flow in Inner Solar System
From: University of New Hampshire group WWW pagehttp://www-ssg.sr.unh.edu/tof/Missions/Ace/aceset.html
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0.01
0.1
1
10
100
103
1 3 5 7 9 11 13
Seasonal Variation of CIR abundances(filled circles = STEP; open circles = LICA)He/O
C/ONe/O4He/OC/ONe/O
Month of Year
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2 3 4 5 6mass (nucleons)
0
100
200
300
3He/4He =0.0016 ± 0.0002
ACE/ULEIS 0.4-1.0 MeV/nsum of 6 CIRs
Dwyer et al, in preparation, 2002
3He is enriched in CIRs -- about 4 times the solar wind value compared to 4He
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Role of pick up ions --
• consistent with He+ abundance• tempting explanation for C/O ratio, but
– no seasonal variation of heavy ion abundances detected, but data is sparse
– at 1 AU C+ is a small fraction of CIR carbon
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39Gloeckler & Geiss, Space Sci. Rev, 86, 127, 1998CY 1994, <r> = 2.8AU; <latitude> = -65°<vsw>=784 km/s
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10
-1
10
0
relative flux
(a) CIR
He
O
Fe
10
-1
10
0
60 62 64 66 68 70
relative flux
adjusted invariant latitude
(b) SEP
HeO
Fe
Mazur, Mason & Mewaldt, 2002, ApJ, in press
SAMPEX:
geomagnetic latitude cutoffs of:
(a) 14 CIRs (1992- 95), and
(b) all 1998 SEP events
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10
1
10
2
10
3
62 63 64 65 66 67
Rigidity (MV)
adjusted invariant latitude
He
C
O
Ne
Fe
Fe
Ne
O
C
He SEP
CIR
Mazur, Mason & Mewaldt, 2002, ApJ, in press
SAMPEX:
Calibration of adjusted magnetic invariant latitude cutoffs for CIRs and SEP events
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10
-3
10
-2
10
-1
10
0
carbon
C
+1
10
-3
10
-2
10
-1
10
0
oxygen
O
+1
flux (#/cm
2
-sec-sr-MeV/n)
10
-3
10
-2
10
-1
10
0
55 60 65 70 75
adjusted invariant latitude
neon
Ne
+1
Mazur, Mason & Mewaldt, 2002, ApJ, in press
SAMPEX:
Observed magnetic cutoffs for CIR events, vs inferred cutoff if ions were singly ionized.
Singly stripped ions must be no more than a few percent of total.
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CIR abundance details show that bulk solar wind source does not fit the new observations--
• Source population is coming from suprathermal region, but that population is not just heated solar wind -- other constituents important
• Do other shock-associated energetic particle observations show evidence for suprathermal seed ions? YES: SEPs, ESPs -- tracer ion is 3He
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10
-4
10
-3
10
-2
10
-1
10
0
10
1
10
2
155 156 157 158 159 160
ACE / ULEIS 0.7 MeV/nucleon
Day of 1999
4
He
3
He
2B N17W69
Mason et al., Ap.J. Letters, 525, L133, 1999
3He and 4He time intensity profiles in large June 4, 1999 solar particle event
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Enhanceed abundances of 3He in large SEP events
ACE/SIS 8-13 MeV/n
0
2,000
4,000
6,000
8,000
10,000
12,000
14,000
0
20
40
60
80
100
120
140
2 3 4 5 6
Mass (AMU)
(a)
"finite" 3He
ACE/ULEIS 0.5-2 MeV/n
Wiedenbeck et al., AIP Conf Proc 528, 107, 2000Mason et al., Ap.J. Letters, 525, L133, 1999
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Suprathermals show 10-100 times more variation in intensity than solar wind -- likely critical issue in energetic particle intensities
0.01
0.1
1
10
100
1000
50 70 90 110 130 150
WIND / EPACT / STEP30 keV/n Fe
Day of 2000
104
105
106
107
108
109
50 70 90 110 130 150
WIND / SWENp * Vsw ^2
Day of 2000
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Conclusions: 1 AU CIRs• CIR source is not bulk solar wind, but rather the
suprathermal region (v/vsw >~ 1.5)• time dependent, multiple ingredients:
• solar wind suprathermal tail
• pick up ions (interstellar)
• pick up ions (inner source)
• other remnants (large SEP events, impulsive SEP events)
• at < few hundred keV/n, CIR ions are “locally accelerated”
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200
300
400
500
600
700
800
900
1000
10 20 30 40 50 60
ACE / SWEPAM solar wind speed
SWEPAM Vsw
Day of 2000
0.001
0.01
0.1
1
10
10 20 30 40 50 60
ACE / ULEIS 270 keV/nucleon
C12 0.2731 MeV/nuc O16 0.2731 MeV/nuc
Day of 2000
27 daysCIRCIR CIRSEP
CIRs observed in early 2000 on ACE
•typical appearance
•note change in C/O ratio in CIRs vs. solar events
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10
100
1000
10 4
10 20 30 40 50 60
ACE / ULEIS E> 200 keV/nCIR and SEP mass histograms
tof_mass -- cir tof_mass -- SEP renormalized
Mass (AMU)
2/6/2002
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50
100
1000
10 4
10 15 20 25 30
ACE / ULEIS E> 200 keV/nCIR and SEP mass histograms
tof_mass -- cir tof_mass -- SEP renormalized
Mass (AMU)
2/6/2002
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Introduction
• Dependence of some abundances on coronal hole speed• No reflection of solar wind abundance changes across stream interface
- pointing to another source (the suprathermals) / Ubiquitous tails • Little influence of Z>2 pickup ions at 1 AU• Most 1 AU events don’t have shocks• complicated time profile that includes local acceleration and transport of
ions from shocks later in the events, as long as a week (Reames)
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