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Review of Observations of Particles From Solar Flares and Their Clues to
the Structure of the IMFJoe Mazur
The Aerospace Corporation
Glenn Mason
Johns Hopkins/APL
Joe Dwyer
Florida Institute of Technology
Joe Giacalone & Randy Jokipii
University of Arizona
Ed Stone
California Institute of Technology
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Introduction• Energetic ions from solar flares sometimes arrive at Earth
with velocity dispersion that allows us to see individual particle injections from active regions at the sun.
• The particle events often have drop-outs in intensity across all energies that are an effect of the structure of the interplanetary magnetic field, and not of particle release at the flare source.
• This talk will briefly review the observations and their interpretation using a model magnetic field that was developed to interpret the transport of energetic particles above the ecliptic plane via meandering field lines.
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Velocity dispersion is common to many acceleration sites
30
100
300
3:00 5:004:00 6:001990 August 21
initialinjection
drift echoes
UT
Field-aligned beams in aurora: propagation distance ~103 km
Drift echoes from substorms: propagation distance ~105 km
~10 secondsGEODESIC rocket flight data courtesy of J. Clemmons
CRRES/MICS data courtesy of J. Fennell
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Velocity dispersion in energetic particles from solar flares
0.1
1
MeV/nucleon
12
3 4
56
7891011
carbon - iron
8/15/98 8/17/98 8/19/98
• Propagation distance ~108 km
• Multiple particle injections from a solar active region
• Particle intensity often varies by >10x during an event
• Sometimes do not observe the entire injection
Mason, Mazur, & Dwyer ApJ Letters 525, L133-L136,1999
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Solar flares & escaping ions
M. Aschwanden, Space Sci. Rev. 101, 1-227, 2002
• Events have been studied since the 1970’s
• Enhanced in 3He (~1000x), Ne-Fe (~10x), trans-Fe (~1000x) compared to solar corona
• Sometimes fully stripped up to Si• Beams of 10-100 keV electrons• Gyroresonant wave-particle
interaction in a 3-5 MK plasma may account for enrichments (3He: Temerin & Roth 1992, Ne-Fe: Miller et al. 1993)
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Glimpses of small-scale (~1 hour) variations in solar energetic particles
Anderson & Dougherty, Solar Phys. 103, 165-175, 1986. Buttighoffer, Astron. & Astrophysics 335, 295-302, 1998
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Glimpses of small-scale variations in solar energetic particles
McCracken & Ness, JGR 71, pp. 3315-3318, 1966
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POSITION-SENSINGANODE
SCALE (cm)
0 10
DETECTOR ARRAYSOLID STATE
TYPICAL SECONDARYELECTRON PATH
ULEIS Telescope Cross Section
ANODEPOSITION-SENSING
THIN FOIL
TYPICAL ION PATH
ELECTROSTATICMIRROR
ACCELERATING HARP
SUNSHADE
START1 MCPs
START2 MCPs
ELECTROSTATICMIRROR
STOP MCPs
SLIDING IRIS(partly open)
Ultra-Low Energy Isotope Spectrometer
• 0.02-10 MeV/nucleon • Dual time-of-flight measurements for improved mass resolution
m/m ~ 0.03
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3He
Time
Mas
s
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10-3
10-2
10-1
100
101 Fe 0.0342 MeV/nuc Fe 0.0683 MeV/nuc Fe 0.1366 MeV/nuc Fe 0.2733 MeV/nuc Fe 0.5466 MeV/nuc
Flux (#/cm
2
-sec-sr-MeV/n)Fe flux
10-2
10-1
100
8 8.5 9 9.5 10 10.5 11
MeV/nucleon
day of 1999
Fe energy vs time
• New views of the time-dependence of solar particle events
• Low-energy threshold so an event lasts many hours
• Large collecting area for low-intensity events that previous instruments would have missed
A new look with ULEIS sensitivity
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0.1
1
MeV/nucleon
12
3 4
56
7891011
carbon - iron
8/15/98 8/17/98 8/19/98
Puzzling cases of “missing” ions
Mason, Mazur, & Dwyer ApJ Letters 525, L133-L136,1999
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Time& spatial scales of events
• 25 events 11/97 to 7/99• Tallied duration of “sub-
intervals”• Factored in solar wind speed
to convert to a spatial size• Edges of drop-outs as sharp
as ~2 minutes (~5x104 km or ~ few gyroradii of 1 MeV/n 56Fe+18)
Mazur et al. ApJ Letters 532, L79-L82, 2000
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CME-related events
• Events associated with large coronal mass ejections do not have drop-outs
Reames et al., ApJ, 466, 1996
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0
5
10
15
20
25
0 4 8 12 16 20 24
counts/bin
sub-interval duration (hours)
solar energeticparticles: mean = 3.2 hours
solar wind: 3.4 hours
02468
101214
0 4 8 12 16 20 24 28
counts/bin
sub-interval size (106 km)
solar energeticparticles:
mean = 4.7x106 km
solar wind:
4.9x106 km
Survey results
Solar wind correlation length: Matthaeus, Goldstein, & King, JGR 91, 59-69, 1986
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Suprathermal electrons
Gosling et al. ApJ 614, 412-419, 2004
• Common features in ions and suprathermal electrons (<1.4 keV) (akin to electron obs. of Anderson & Dougherty 1986)
• Gosling et al. (2004) showed 2 events where the ions had dropouts but the electrons did not, possibly indicating a more uniform and/or broad electron source
ions
electrons
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-200
-150
-100
-50
0
50
100
150
200
-100 0 100 200 300 400Xgse
~265 Re
Wind
ACE
solar wind~550 km/sec
Delay from ACEto Wind ~ 50 minutes
12 August 2000
•Simultaneous observations of the same flare injection on 12 August 2000: ACE & Wind spacecraft
•The later arrival of empty flux tubes at Wind is consistent with solar wind convection
UT
Simultaneous Wind/ACE observations
C-Fe
C-Fe
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Numerical simulations of particle transport
• Model field used to study propagation of particles from corotating interaction regions to high heliographic latitudes (Giacalone 1999)
• Model was based on earlier work by Jokipii & Parker (1968) and Jokipii & Kota (1989)
• Random motion of field line footpoints in the photosphere over ~4x104 km, time scales of ~1 day
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Giacalone, Jokipii, & Mazur, ApJ Lett. 532, 2000
•The model followed the trajectories of 8 keV/n to 20 MeV/n oxygen from an impulsive flare
•The particles traveled through pre-existing IMF structures
•After ~1 day, ions were still present inside 1 AU and populated field lines spanning ~10º in longitude
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•Simulated velocity dispersion & time-dependence with two different source sizes
•Same realization of the magnetic field
•Large sources (corresponding to a CME shock) generate continuous event profiles
Giacalone, Jokipii, & Mazur, ApJ Lett. 532, 2000
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Closer look at dropout “edges”: iron
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Closer look at dropout “edges”: iron
At 1700Z:B ~ 24 nTVsw ~ 580 km/sec
More examples, viewed with iron
Questions1. What observables in the 1 AU solar particle data might be used
to establish the source of these dispersionless features (i.e. turbulence or field-line mixing from footpoint motion at the sun)?
2. What inner heliosphere measurements of the IMF and of the energetic particles, on Sentinels for example, would clearly establish the origin of these features?
3. Are the Ulysses observations of Jovian electrons as far as ~2 AU from Jupiter (McKibben et al. 2006) a valuable constraint on either the turbulence or random walk model?
4. What other observables in these data would be of use? (solar cycle dependence; statistics of the scale of the ‘dropout’ edges)
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New Capability: Advanced Composition Explorer
• ACE launched in August 1997
• The ACE objective is to collect samples of matter in the solar system using large instruments
• We do the collecting by letting the matter come to ACE and transmitting the results to Earth
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3He-rich Solar Flares
• Discovered in late 1960s• 3He/4He ratio in solar wind ~5x10-4
• The events drew attention because 3He/4He> 0.1 without any accompanying 2H or other secondaries as one might expect from spallation in the solar atmosphere
• Later found enhancements of heavy ions up to iron by factor of 5-10 as well as: – Impulsive electron events– Scatter-free propagation– Often lack of any flare association on Sun– Sometimes ions fully stripped of electrons
Mason et al. ApJ 574, 1039--1058, 2002
3He4He
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ACE Survey of Flare Spectra• Searched for periods with clear
flare velocity dispersion– Deleted events with local acceleration– Required complete observation of
event (i.e. that ACE remained connected to it) for whole energy range of instrument
• Cases often involved multiple injections; each event separated, and fluences calculated
Mason, Dwyer, & Mazur ApJ Lett. 545, 2000