Direct Measurements of Cosmic Rays · Even Briefer History of Cosmic Rays Update Start life as a...
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Direct Measurements of Cosmic Rays
TeV Particle Astrophysics II - UW Madison 2006
Simon Swordy - U. Chicago ([email protected])
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Direct Measurements of Cosmic Raysthis Century
TeV Particle Astrophysics II - UW Madison 2006
Simon Swordy - U. Chicago ([email protected])
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99.999999999%of cosmic ray action
Cosmic Ray Roadmap
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Even Briefer History of Cosmic Rays
Start life as a nucleus in some star or other
Become a part of a supra-thermal stellar wind
Hit hard by some humungous shock wave
Mince around in Galactic magnetic field structure
Leave Galaxy Die by nuclear interaction
Fade
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Cosmic Ray Source Material and History?
Best measurements of this come from ACE experiment - NASA/Explorer, 1997-2000CRIS instrument silicon detectors for Z, A in the ~100MeV range.
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Lifetime of Cosmic Rays from ACE (15±1.6 Myr)
(Secondary radioactive nuclei with comparable half-lives)
(Yanasak et al. - ApJ 2001, 768)
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Also can determine mean density of propagation volume n = 0.34±0.04 atoms per cc(Because nuclei loss occurs by both fragmentation and decay)
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ACE - Time between nucleosynthesis and acceleration >105 years(Absence of electron capture nucleus Ni59)
(Wiedenbeck et al., Ap. J. 1999, L61)
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Even Briefer History of Cosmic Rays Update
Start life as a nucleus in some star or other
Become a part of a supra-thermal stellar wind
Hit hard by some humungous shock wave
Mince around in Galactic magnetic field structure
Leave Galaxy Die by nuclear interaction
Fade
>10,000 years
~1.5 M years
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Cosmic Ray Source Isotopic Abundances ~400MeV/N very similar to Solar System(but there are some differences….)
(Wiedenbeck, SpScRev, 2001, 15)
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Correlation between CR source Isotopes and Solar System
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Correlations of CR/LGA source material at ~100GeV/n with atomic energy level
Also shows up in solar flare composition/photosphere
But, FIP or volatility?
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Even Briefer History of Cosmic Rays Update
Start life as a nucleus in some star or other
Become a part of a supra-thermal stellar wind
Hit hard by some humungous shock wave
Mince around in Galactic magnetic field structure
Leave Galaxy Die by nuclear interaction
Fade
>10,000 years
~1.5 M years
Isotopic similarities with SS andFIP correlation (but FIP/volatility?)
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SN shock waves accelerate particles (HESS RXJ…)
(electrons/hadrons?)
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Even Briefer History of Cosmic Rays Update
Start life as a nucleus in some star or other
Become a part of a supra-thermal stellar wind
Hit hard by some humungous shock wave
Mince around in Galactic magnetic field structure
Leave Galaxy Die by nuclear interaction
Fade
>10,000 years
~1.5 M years
Isotopic similarities with SS andFIP correlation (but FIP/volatility?)
SN diffusive shock acceleration
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Pros and Cons of SN diffusive shock acceleration
Pros - enough power available
- working theory exists which produces power law of particles in magnetic rigidity
- SNR certainly have extensive non-thermal particle populations
- power law index ~2 close to that observed in CR source (see later) up to ~50GeV
Cons - because of strong shock lifetime, maximum particle energy is limited
- indirectly observed cosmic rays seem to exceed this limit
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Magnet Spectrometer Data (>2000) Similar spectra at high energy - same magnetic rigidity spectraResidual systematic flux uncertainty ~10%
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Thin Calorimetry data, passive (JACEE, RUNJOB) and active (ATIC)Some differences here…..
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Mean ln(A) versus Energy - RUNJOB essentially constant into knee region
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Heavy Nuclei: TRACER (trd) sees magnetic rigidity spectra, constant slope
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TRACER measurements into knee regionConsistent with RUNJOB
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Escape from the Galaxy is energy dependent (secondary/primaryratio decreases with energy, if E-0.6 the source is dN/dE~E2.1
New measurements on B/C from RUNJOB (blue) seem high(red -HEAO, Black-CRN)
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CREAM -I 2004-2005(42 days)Cosmic Ray EnergeticsAnd Mass
Maryland, Penn State,Chicago, Ohio St., INFNItaly, Korea
Also CREAM-II 2005-2006 (28 days)
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Charge Resolution from TRD/Cerenkov in CREAM-I
PreliminaryPreliminary
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CREAM-I, Hi-Z with Silicon, TCD and Cerenkov
CREAM-I, Lo-Z trig
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CREAM HiZ Oxygen Spectrum
PreliminaryPreliminary
Total Particle Energy (eV)
Flu
x (m
2 s
sr G
eV)-
1
HEAO
CRN
CREAM TRDCREAM Cerenkov
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CREAM HiZ Carbon Spectrum
PreliminaryPreliminary
Total Particle Energy (eV)
Flu
x (m
2 s
sr G
eV)-
1
HEAO
CRN
CREAM TRDCREAM Cerenkov
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Electrons at high energy loose energy mostly by synchrotronPlaces limits on the distance and age of source
100TeV
30TeV
10TeV
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Electron Models with stochastic SN (Galprop -Strong and Moskalenko)
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New electron measurements from ATIC - 2005 -> Feature?
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Conclusions:
• SNR shock acceleration of most of the cosmicrays seems to be in good shape.
• Nuclei spectra are power laws in rigidity
• Source spectra have power law index 2.1-2.3
• Newer measurements (RUNJOB, TRACER) showmean mass at the knee may be lighter thanpreviously thought
• Electrons at high energy could be very interesting