Transcript 1024 eV = 1015 GeV > MGUT - IceCube Neutrino Observatory

Lepton - Photon 01
Francis Halzen
• the sky
> 10 GeV photon energy
< 10-14 cm wavelength
• > 108 TeV particles exist
Fly’s Eye/Hires
• they should not
• more/better data
arrays of air Cherenkov telescopes
104 km2 air shower arrays
~ km3 neutrino detectors
CMB
Radio
Visibe
GeV g-rays
Flux
Energy (eV)
1 TeV
/
/
/
/
/
/ TeV sources!
/
/
/
cosmic
/
/
rays
/
/
/
/
/
/
n
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
fluorescence from atmospheric nitrogen
cosmic ray
o
+
_

+
_
 g
 n
fluorescent light
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
Cosmic Accelerators
E ~ GcBR
R~
2
GM/c
energy
magnetic
field
E ~ GBM
boost
factor
mass
E~GBM
E > 1019 eV ?
•quasars
•blasars
•neutron stars
black holes
..
•grb
G @ 1 B @ 103G
G >~ 10
G @ 1 B @ 1012G
M @ 109 Msun
M @ Msun
G >~ 102
emit highest energy g’s!
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
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 (>1 TeV) < 2 – 30 x 10-7 cm-2 s-1 @ 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
Particles >
20
10
eV ?
•not protons
cannot reach us from cosmic accelerators
lint < 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
Interaction length of protons
in microwave background
p + gCMB
lgp = (
 + ….
nCMB s
p+g
CMB
) -1
@ 10 Mpc
GZK cutoff
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 ?
Particles > 1020 eV ?
•not protons
new
astrophysics?
cannot reach us from cosmic accelerators
lint < 50 Mpc
no diffusion in magnetic fields
doublets, triplet trouble for top-down
scenarios
•not photons
g + Bearth e+ + e- not seen
showers not muon-poor
•not neutrinos
snp @ 10-5 spp
no air showers
sn p @ spp with
TeV - gravity unitarity?
24
10 eV
=
15
10
GeV ~_ MGUT
are cosmic rays the decay product of
•topological defects
(vibrating string, annihilating monopoles)
•heavy relics?
Top. Def.
X,Y
W, Z
g
quark + leptons
n
>> p
g
•top-down spectrum
•hierarchy n
g
p
black hole
radiation
enveloping
black hole
cosmic ray
puzzle
protons
TeV g - rays
neutrinos
3
~
1
km
~
•atmospheric Cherenkov
high energy
air shower
•space-based
detectors
arrays
•AMANDA / Ice Cube
•Veritas,
Hess,
Magic
…
•Hi
Res,
Auger,
e.g.
Antares, Nestor,
•GLAST…
Airwatch,
NEMO
OWL, TA…
•particle physics
•short-wavelength
also
and cosmology
study of supernova
remnants and galaxies
•dark matter search
•discovery
104 km2
Array
=> Very large effective area (105 m2)
=> 3-dim shower reconstruction
=> Dramatic improvements in
- Energy Resolution
- Background Rejection
STACEE
Solar Tower Atmospheric Cherenkov Effect Experiment
Gamma-ray Astrophysics between 50-500 GeV
QuickTime™ and a
GIF decompressor
are needed to see this picture.
ne+ e
W  + n
6400 TeV
PeV
t
(300m)
nt t
t decays
Why is Searching for n’s from GRBs
of Interest?
•Search for vacuum oscillations (n
Dm2 >~
10-17 eV2
•Test weak equivalence principle: 10-6
•Test
Cphoton - Cn : 10-16
Cn
nt):
Lepton - Photon 01
Francis Halzen
• the sky
> 10 GeV photon energy
< 10-14 cm wavelength
• > 108 TeV particles exist
Fly’s Eye/Hires
• they should not
• more/better data
arrays of air Cherenkov telescopes
104 km2 air shower arrays
~ km3 neutrino detectors
/
/
/
/
/
/ TeV sources!
/
/
/
cosmic
/
/
rays
/
/
/
/
/
/
n