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Lepton - Photon 01 Francis Halzen

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Lepton - Photon 01 Francis Halzen the sky 10 GeV photon energy 108 TeV particles exist Fly s Eye/Hires they should not – PowerPoint PPT presentation

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Title: Lepton - Photon 01 Francis Halzen


1
Lepton - Photon 01Francis Halzen
  • the sky gt 10 GeV photon energy
  • lt 10-14 cm wavelength
  • gt 108 TeV particles exist
  • Flys Eye/Hires
  • they should not
  • more/better data
  • arrays of air Cherenkov telescopes
  • 104 km2 air shower arrays
  • km3 neutrino detectors

2
Energy (eV)
1 TeV
Radio
CMB
Visibe
GeV g-rays
Flux
3
n
/ / / / / / / / / / / / / / / / /
TeV sources!
cosmic rays
4
With 103 TeV energy, photons do not reach us from
the edge of our galaxy because of their small
mean free path in the microwave background.
  • ?g g??? ?????e e-

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fluorescence from atmospheric nitrogen
_
cosmic ray
_
?o??????????? ?????????????
fluorescent light
electromagnetic shower
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Acceleration to 1021eV? 102
Joules 0.01 MGUT
  • dense regions with exceptional
  • gravitational force creating relativistic
  • flows of charged particles, e.g.
  • annihilating black holes/neutron stars
  • dense cores of exploding stars
  • supermassive black holes

13
Cosmic Accelerators
E GcBR
R GM/c2
magnetic field
energy
E GBM
mass
boost factor
14
E G?B M
E gt 1019 eV ?
  • quasars G _at_ 1 B _at_ 103G M _at_?109
    Msun
  • blasars G 10
  • neutron stars G _at_ 1 B _at_ 1012G M _at_ Msun
  • black holes
  • .
  • .
  • grb G 102

gt
gt
emit highest energy gs!
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Profile of Gamma Ray Bursts
  • Total energy one solar mass
  • Photon energy 0.1 MeV to TeV
  • Duration 0.1 secs -- 20 min
  • Several per day
  • Brightest object in the sky
  • Complicated temporal structure
  • no typical burst profile

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A few more results
  • Gamma Ray Bursts (GRBs)
  • Observation of single 3 s excess (GRB 970417a)
    within 1997 BATSE trigger.
  • Flux limit for unidentified TeV point sources
  • For E spectrum

Flux (gt1 TeV) lt 2 30 x 10-7 cm-2 s-1 _at_ 90
AMANDA II will probe this flux for
n/g 1
However, g spectrum probably softer due to
reprocessing (core) and absorption in photon BG
20
Particles gt 1020 eV ?
  • not protons
  • cannot reach us from cosmic accelerators
  • lint lt 50 Mpc
  • no diffusion in magnetic fields
  • doublets, triplet
  • not photons
  • g Bearth e e- not seen
  • showers not muon-poor
  • not neutrinos
  • snp ? 10-5 spp ????? no air showers

21
Interaction length of protons in microwave
backgroundp gCMB p .
?????lgp (?nCMB s? ????? ) -1 _at_
10 Mpc
pgCMB
GZK cutoff
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Forthcoming AGASA Results
  • The highest energy cosmic rays do come from point
    sources 5 sigma correlation between directions
    of pairs of particles. Birth of proton astronomy!
  • Are the highest energy cosmic rays Fe?
  • GKZ cutoff at 2 1020 eV ?

24
Particles gt 1020 eV ?
new astrophysics?
  • not protons
  • cannot reach us from cosmic accelerators
  • lint lt 50 Mpc
  • no diffusion in magnetic fields
  • doublets, triplet
  • not photons
  • g Bearth e e- not seen
  • showers not muon-poor
  • not neutrinos
  • snp ? 10-5 spp ?? no air showers

trouble for top-down scenarios
sn p _at_ spp with TeV - gravity unitarity?
25
1024 eV 1015 GeV MGUT
_
are cosmic rays the decay product of
  • topological defects
  • (vibrating string, annihilating monopoles)
  • heavy relics?

Top. Def. ?? X,Y ?? W, Z ?? quark leptons
?? gtgt p
?? ?? g
  • top-down spectrum
  • hierarchy n ??? g???? p

26
black hole
radiation enveloping black hole
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cosmic ray puzzle
neutrinos
protons
TeV g - rays
1 km3 high energy detectors
104 km2 air shower arrays
  • atmospheric Cherenkov
  • space-based
  • AMANDA / Ice Cube
  • Antares, Nestor,
  • NEMO
  • Veritas, Hess, Magic
  • GLAST
  • Hi Res, Auger,
  • Airwatch,
  • OWL, TA

e.g.
  • particle physics
  • and cosmology
  • dark matter search
  • discovery
  • short-wavelength
  • study of supernova
  • remnants and galaxies

also
30
Array gt Very large effective area (105 m2)
gt 3-dim shower reconstruction gt Dramatic
improvements in - Energy Resolution
- Background Rejection
31
STACEE
Solar Tower Atmospheric Cherenkov Effect
Experiment
Gamma-ray Astrophysics between 50-500 GeV
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ne e W m? nm 6400 TeV
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nt t
PeV t(300m)
t decays
44
Why is Searching for ns from GRBs of Interest?
  • Search for vacuum oscillations (n??????nt)
  • Dm2 ?? 10-17 eV2
  • Test weak equivalence principle 10-6
  • Test 10-16

gt
Cphoton - Cn Cn
45
Lepton - Photon 01Francis Halzen
  • the sky gt 10 GeV photon energy
  • lt 10-14 cm wavelength
  • gt 108 TeV particles exist
  • Flys Eye/Hires
  • they should not
  • more/better data
  • arrays of air Cherenkov telescopes
  • 104 km2 air shower arrays
  • km3 neutrino detectors

46
n
/ / / / / / / / / / / / / / / / /
TeV sources!
cosmic rays
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