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260404 Astroparticle Physics 1
Astroparticle PhysicsAstroparticle PhysicsKey IssuesKey Issues
Jan KuijpersJan Kuijpers
Dep. of Astrophysics/ HEFINDep. of Astrophysics/ HEFIN
University of NijmegenUniversity of Nijmegen
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260404 Astroparticle Physics 2
Cosmic Ray Energy SpectrumCosmic Ray Energy Spectrum
LHCLHC ||
_10_10-1-1
FluxFlux (m(m22 sr s GeV) sr s GeV)-1-1
_10_10-25-25
| || |101099 Energy (eV) 10 Energy (eV) 102020
SwordySwordy
Ankle (1 per kmAnkle (1 per km22-year)__-year)__
Knee Knee __(1 per m__(1 per m22-year)-year)
__(1 per m__(1 per m22-sec)-sec)
EE-2.7-2.7 E E-3-3
Flux x EFlux x E2.752.75
| | | | 1 Energy (GeV/n) 101 Energy (GeV/n) 1077
ee-- up to 1 TeV, only 1 % up to 1 TeV, only 1 %
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260404 Astroparticle Physics 3
Cosmic RaysCosmic RaysDirect detection:Direct detection:• Nuclei, power-lawNuclei, power-law• Gamma-rays up to TeV (AGN, pulsars)Gamma-rays up to TeV (AGN, pulsars)• Neutrinos Neutrinos (solar, SN1987a)(solar, SN1987a)
Indirect detection from radiation: optically thinIndirect detection from radiation: optically thin
synchrotron, inverse Compton, bremsstrahlung:synchrotron, inverse Compton, bremsstrahlung:• Electrons: power-law –2/–2.7/-3 over many decades in Electrons: power-law –2/–2.7/-3 over many decades in
extragalactic radio galaxies. Also in extragal. extragalactic radio galaxies. Also in extragal. GRBsGRBs, galactic , galactic SNRs, X-ray binaries, jets.SNRs, X-ray binaries, jets.
• Protons (X-ray and MeV galactic)Protons (X-ray and MeV galactic)
Main question: Main question:
1: UNIVERSAL ACCELERATION PROCESS?1: UNIVERSAL ACCELERATION PROCESS?
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260404 Astroparticle Physics 4
Particle acceleration processesParticle acceleration processes• Shock waves (Bell,..1977; Fermi 1954):Shock waves (Bell,..1977; Fermi 1954):
22 11
uu22 uu11
2
22 2
st
1 2
NR shock 21 order Fermi
v
c cc
c
v v v"
c c
vc c
2 1
1 2
1
2
2
acc
esc
u uu u
N(E ) E
E E
De Hoffmann-De Hoffmann-Teller frameTeller frame
SNRs: SNRs: vvss~few ~few 101044 km/s GRBs: km/s GRBs: ~300~300
Jets: Radio galaxies X-ray binariesJets: Radio galaxies X-ray binaries
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260404 Astroparticle Physics 5
10109 9 G_G_
BB
1010-9-9 G_ G_ 1 AU 1 pc 1 kpc 1 Mpc1 AU 1 pc 1 kpc 1 Mpc | | | || | | |Size (km) 10 10Size (km) 10 10
EEmaxmax==
ZeBLZeBL
Flare stars
MagnetarsPulsars
Stellar mass black holes
Massive black holes
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260404 Astroparticle Physics 6
More questions:More questions:
2
2
sync
radio optical X ray L
IC
e B ( f )
e
��������������
0
( ) ( )
e
... ...p / n N
/ K ... ... e
2: TeV gamma rays from electrons or protons?2: TeV gamma rays from electrons or protons?
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260404 Astroparticle Physics 7
Van den AkkerVan den Akker2004 PhD Thesis 2004 PhD Thesis KUNKUN
Case study: L3+Cosmics: search for TeV photonsCase study: L3+Cosmics: search for TeV photons
from GRBsfrom GRBs
from 64 EGRETfrom 64 EGRETunidentifiedunidentified30 MeV/30 GeV30 MeV/30 GeVGRSsGRSs
GRB 990903GRB 990903
Significance of muon excess
# muons per square degree per sec
not corrected for detector accept.
galacticcoordin.
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260404 Astroparticle Physics 8
Linear acceleration of primary electrons in Linear acceleration of primary electrons in unipolar inductor (neutron stars, unipolar inductor (neutron stars, accretion discs, black hole collapse + accretion discs, black hole collapse + torus) and subsequent pair creation in torus) and subsequent pair creation in strong B or photon background.strong B or photon background.
V v B d ������������������������������������������
Pair plasma productionPair plasma productionin circuit Cin circuit C
3: Origin 3: Origin ee plasma? plasma?
CC
CCRotationRotationaxisaxis
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260404 Astroparticle Physics 9
Fung & Kuijpers,Fung & Kuijpers,2004, A&A subm.2004, A&A subm.
Case study: Coherent emission from particle beamsCase study: Coherent emission from particle beams
Radio pulsars asRadio pulsars asFree Electron Free Electron LasersLasers
10001000
950 950t (10t (10-5-5 sec) sec)
E (V/m)E (V/m)
f (10f (10-10-10 Hz) Hz)
t (10t (10-5-5 sec) sec)
P (10P (101313 W) W)
varyingvaryingmagneticmagneticwigglerwiggler
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260404 Astroparticle Physics 10
DynamoDynamo
22
2 2
2nd
2
1 2
42 order Fermi
c cc
c
v v v"
c c
v
c
accretion disk compact objectaccretion disk compact object
Poynting flux dominatedPoynting flux dominatedMagnetized windMagnetized windJetsJets
5: Origin energy fireball?5: Origin energy fireball?
4: Origin of magnetic field?4: Origin of magnetic field?
- - Magnetic reconnectionMagnetic reconnection
- Plasma turbulence Plasma turbulence - Stochastic accelerationStochastic acceleration
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260404 Astroparticle Physics 11
Case study: Coupling gravitational waves – mhd wavesCase study: Coupling gravitational waves – mhd waves
Magnetosonic waveMagnetosonic wave Alfven waveAlfven waveSSFFGG
AAGG
GWGW++GWGWxx
Moortgat & Kuijpers 2003 A&A 402, 905 ; 2004 Phys Rev D, subm.Moortgat & Kuijpers 2003 A&A 402, 905 ; 2004 Phys Rev D, subm.
zz
xy
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260404 Astroparticle Physics 12
Cronin 2004Cronin 2004
Photopion productionPhotopion production
Photopair productionPhotopair production
6. Is there a high energy CR cut-off?6. Is there a high energy CR cut-off?
||GZK cutoffGZK cutoff
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260404 Astroparticle Physics 13
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260404 Astroparticle Physics 14
Cronin 2004Cronin 2004
7. Origin of highest energy CRs?7. Origin of highest energy CRs?
Conflicting observ.Conflicting observ.Inconclusive statisticsInconclusive statistics
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260404 Astroparticle Physics 15
Wilkens, 2003, Wilkens, 2003, PhD Thesis KUNPhD Thesis KUN
Case study: L3+Cosmics: composition – forward cross-sectionCase study: L3+Cosmics: composition – forward cross-section
muonsmuons
muon mul;tiplicityComparison to Monte Carlo CORSIKAComparison to Monte Carlo CORSIKA
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260404 Astroparticle Physics 16
Case study: L3+Cosmics: muon spectrum at sea levelCase study: L3+Cosmics: muon spectrum at sea level
Petersen, 2002Petersen, 2002PhD Thesis, KUNPhD Thesis, KUN
Charge ratioCharge ratio
Accurate absolute Accurate absolute spectrumspectrum
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260404 Astroparticle Physics 17Cronin 2004Cronin 2004
Gamma ray: -----Gamma ray: -----Fe: _______Fe: _______Protons: Protons: ____________
Air showersAir showers
LOFAR cornerstone:LOFAR cornerstone:study of CRs and their sourcesstudy of CRs and their sources
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260404 Astroparticle Physics 18
High schools & High schools & cosmic rays:cosmic rays:detector construction,detector construction,observations,observations,analysisanalysis
Outreach opportunities: NAHSA – HiSPARC Outreach opportunities: NAHSA – HiSPARC - LOFAR- LOFAR
Timmermans et al,Timmermans et al,2004, KUN2004, KUN
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260404 Astroparticle Physics 19
Key questions in astroparticle physics:Key questions in astroparticle physics:
• ORIGINS CRs (HADRONS+LEPTONS): ORIGINS CRs (HADRONS+LEPTONS): SNRs, BHs, NSs, DARK MATTER, DARK ENERGYSNRs, BHs, NSs, DARK MATTER, DARK ENERGY
• UNIVERSAL ACCELERATION PROCESS? UNIVERSAL ACCELERATION PROCESS? • TeV GAMMA RAYS FROM ELECTRONS OR PROTONS?TeV GAMMA RAYS FROM ELECTRONS OR PROTONS?• ORIGIN ORIGIN ee PLASMA? PLASMA? • ORIGIN OF MAGNETIC FIELD? ORIGIN OF MAGNETIC FIELD? • ENERGY PARTITIONINGENERGY PARTITIONING• IS THERE A HIGH ENERGY CR CUT-OFF?IS THERE A HIGH ENERGY CR CUT-OFF?• QUEST FOR HIGHEST ENERGY CRs AND SOURCESQUEST FOR HIGHEST ENERGY CRs AND SOURCES
2 communities astroparticle detectors2 communities astroparticle detectorsLOFAR + ANTARESLOFAR + ANTARES