O mist

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Introdução Raios Cósmicos

Mário Pimenta Lisboa, 3/2007
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Uma história já longa...

• As esferas descarregam-se...

Coulomb, 1785
Finais do século XIX
Radioactividade ?
3
Viktor Hess, 1912

• Diversos vôos até 6 Km
• Dia/noite, eclipse, ...

I
h
600 m
Raios Cósmicos ! (Milikan)
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Cascatas de partículas

• Pierre Auger, 1938

Coincidências

d
d
Primeiras estimativas da energia das cascatas!
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Na Origem da física de partículas
e

• Positrão (Anderson, 1932)

Antimatéria! (Dirac)
g -gt ee- (Einstein)
m (Anderson,1937)
Rossi, 1940 Tempo de vida do muão. Dilatação do
tempo!
p (Latter, 1947)
Cloud Chamber picture
Interacções fortes (Yukawa)
Anos 50 K, L, S, X, W ...
6

• Inúmeros desenvolvimentos até aos anos 50...

Aceleradores Física de partículas

• Raios Cósmicos
• Origem
• Aceleração
• Composição
• ...

Year of completion
Única fonte a energias muito altas!!
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O Espectro de energia
F l u x o
joelho
tornozelo
LHC
Tevatron
Energia (eV)
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Escalas de energia
by A.Letessier-Selvon
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O espectro de energia II
by V.Ptuskin
109 eV Sol 109 a 1015 eV
Origem Galáctica (SNR) 1015 a 5x1018 eV
Situação confusa 1019 eV
Origem desconhecida (Extragaláctica)
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O espectro de energia III

• Composição

p, He, ...., Fe, ... g, e, n
Raios Cósmicos
Sol
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Do espectro primário ao espectro observado...

• Produção
• Fontes
• Espectro
• Composição
• Aceleração

• Sistema Solar
• Solar wind
• Magnetosfera
• Atmosfera

• Propagação
• Campo magnético
• Interacção no meio interestelar

w 1 eV/cm3
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Origem
AGN
Densidade de energia
by V.Ptuskin
1049 erg por SN 1 SN em 30 anos
Potencia libertada na explosão de uma SN 1042
erg/s
Pulsar 2.1046 T-2 erg (T periodo (s))
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Aceleração
Mecanismo de Fermi Ganho de energia estocástico
em Colisões com nuvens de plasma
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Basic acceleration mechanism
Solar coronal mass ejection 9 Mar 2000

• Shock formation
• Sudden release of Energy
• (CMEs, SNRs, GRBs,)
• Supersonic flow hits an obstacle
• (AGNs jets, pulsar winds, )

First-order Fermi acceleration process
Particles gain energy by consecutive crossings of
the shock front. Nonrelativistic
case well understood. Relativistic case
much more difficult!
Needs a (non-uniform) magnetic field !
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Propagação
Difusão...
... Interacção
t107 anos (E1 GeV)
by T.Gaisser
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Confinamento e Composição
Campo magnético Galáctico 6-10
mG Intergaláctico nG
Raio de Larmor
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Detecção

• Os raios cósmicos primarios interagem com a
• atmosfera originando cascatas de partículas

• Baixas energias detecção no Espaço!

• Energias mais altas
• baixo fluxo...

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No Espaço

• AMS Alpha Magnetic Spectrometer

• Raios cósmicos
• Anti-matéria
• Matéria escura

AMS-I 1998 Space Shuttle AMS-II 2008 ISS
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Debaixo de Terra

• Os muões
• são as partículas detectáveis
• mais prenetrantes da cascata

À superfície da Terra 70 m-2 s-1 sr-1 1 cm-2
min-1 (Wp)
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Cascatas de partículas
Nmax? E Xmax ? ln E Luz ? E
Ground level 99 EM (10 MeV)
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Cascatas de partículas II
v c
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Cascatas de partículas detecção
Luz de fluorescência
Luz de Cherenkov

• Partículas

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EAS longitudinal profiles
Gaisser
Nemax ? E Xmax ? ln E
Iron ? 56 nucl(E/56)
Smaller fluctuactions
Smaller Xmax
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EAS transverse profiles
NKG (Nishimura, Kamata, Greisen)
r0 Moliére radius
s shower age
EAS-TOP E1015 eV
Pt distributions Multiple Coulomb scattering
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Hard and soft hadronic interactions
J. Knapp
Perturbative QCD
Pomeron exchange GRT
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Percolation ?
J.Dias de Deus et al.
At high energy the number of strings increases
and percolation in the transverse plane may occur
!
Xmax X0
inelasticity
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EAS Monte Carlo simulations
J.Knapp et al. Astrop. Physics 19 (2003)
e.m. and weak interations
- well known !
hadronic interations
- large uncertainties !
- forward region, small pt, very high
- main parameters sin, kin
computing power
- Always limited
- statistical thinning E gt 1015 eV
Agreement better than 20
codes
- CORSIKA, AIRES
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AGASA
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Energia

• ... Proporcional ao tamanho da cascata Ne

AGASA
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Direcção
... diferenças temporais na detecção da frente da
cascata
zenith
cDt
a
a
r
Dt lt10 ns
Da lt 8o
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Composição

• Identificação de muões massa do primário!

Kascade
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Detectores de fluorescência

• Cascata de electrões na Atmosfera
• Excitação das moléculas de N2

Emissão de luz de fluorescência (UV)
O olho da mosca (Flys Eye)
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Fluorescence

• EAS electrons moving in the atmosphere excite N2
  molecules
• de-excitation fluorescence
  light

Accurate knowledge of conversion from
fluorescence yield to ionization energy loss by
EAS particles is key to this technique
There are open questions (pressure, energy,
wavelength dependence) and differences between
measurements 15-20 uncertainty
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AIRFLY at Argonne
Paolo Privitera, Air fluorescence Workshop 2006
Chemistry Division Van de Graaf (0.6-3 MeV)
HEP Division Advanced Wakefield Accelerator (3
MeV-15 MeV)
Advanced Photon Source (6-30 KeV)
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AIRFLY
Paolo Privitera, Air fluorescence Workshop 2006
Highest precision measurements ever
obtained Preliminary results
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Fluorescence detectors
Flys Eye
Air shower stereo image
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Fluorescence detectors measurements
The direction The Xmax The Energy
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Profundidade do máximo da cascata
Xmax
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Systematics
ground
fluorescence
- Light yield, ? ? 10-5
Rely heavily on the Monte Carlo simulations of
the shower development
Transverse profile
- Atmosphere
T
RH
P, dust, clouds
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Energias muito altas (Egt5x1019eV)
Cerca de 30 acontecimentos em 40 anos
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Volcano Ranch
Primeiro raio cósmico de muito alta energia!

• John Linsley, 1962

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The end of the spectrum...
6 experiments in the last 40 years
20 events !
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AGASA versus HIRES
Not so dramatic ...
20 on energy scale
Small nb of events a 2 ? effect

Wait for the next generation of experiments !
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The Greisen-Zatsepin-Kuzmin (GZK) cutoff
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GZK is model dependent
GZK and magnetic fields (protons) Deligny,
Parizot, Letessier-Selvon
GZK cutoff Energy Stecker and Scully
Energy (in EeV)
1 z
Sources type and distribution
Not a true cutoff !
Primary composition
Pileup
Recovery of the spectrum at higher energies ?
Magnetic fields
46
Evading GZK Bottom-up scenarios
Neutrinos

• Z burst ? ?rel ? Z , E ? 4.1021 /(m ?
  /eV) eV

• enhanced neutrino-nucleon cross-section

New neutral particles
axion, glueballino, ...
Violation of Lorentz simmetry
different p?CMB resonant cross-section tresholds
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Evading GZK Top-down scenarios
Decay products of super-heavy X particles GUT
scale
( right after inflation...)
Short lived
produced continously by topological defects left
over from cosmological phase transitions (cosmic
strings, necklaces, magnetic monopoles... )
Long lived
produced directly in the early Universe (Gauge
bosons, Higgs bosons, super-heavy fermions ...)
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Possible signatures...
Bottom-up
Top-down

• Protons/nuclei, ...
• E-a power law
• Other wavelengths
• Localized sources

• Photons/neutrinos, ...
• Particle decay spectrum
• Distribution in the halo ...
• Isotropy ...

Increase the statistics !

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Possible astrophysical sources
Pulsar
SNR
AGN
Hillas-plot
GRB
confinement!
EmaxbZBL
Radio Galaxy Lobe
by M.Teshima
Be aware of energy losses !
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Energias muito altas II
Astronomia!
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Anisotropies Galactic Center I
AGASA
22 excess 4.5 s
SUGAR
85 excess 2.9 s
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Anisotropies Galactic Center II
AUGER no excess !
Coverage
Significance (1.5º)
Significance (3.7º)
Significance (13.3º)
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Clustering/correlations?
AGASA E gt 4 1019 eV
5 pairs and 1 triplet within 3o
No clear astronomical counterparts within ? 100
Mpc
Correlations with BL-Lacs
AUGER All sky searches
Several claims but no firm
evidence so far
No excess so far
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The Pierre Auger Observatory

• The south hemisphere observatory

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Auger status
Surface Detector Array (for a a total of 1600
tanks) 1185 surface detector stations
deployed 1165 surface detector stations with
water 989 surface detector stations with
electronics
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Auger status
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telescope building Los Leones
LIDAR station
communication tower
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Surface detectors
1600 water Cerenkov detectors
autonomous systems solar panel,
batteries, GPS timing Radio communication, 40
MHz FADC, e/µ discrimination
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The fluorescence detectors
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A stereo hybrid event
Coihueco
Los Leones
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Auger FD/SD energy inter-calibration
Log (E/EeV)
A.Watson
1019 eV
Hybrid Events with strict event selection
Good correlation !
Log S(1000)
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Enhancements

• AMIGA

• HEAT

Auger Muons and Infill for the Ground Array (2009)
HEA Telescope (2008)

• Aims of the proposed enhancements for the Auger
  south observatory
• extend the FD angular acceptance
• measure directly the muon content of the EAS
• lower the energy threshold to 1017 eV.

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AUGER North - Colorado
In Project
22,000 km2
Telescope Array Utah
576 plastic scintillators
3 FD sites
3,800 km2
20km
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next to next .
Increase the statistics
Increase the resolution
- Space (EUSO, )
- A 2d profile
Fluorescence detectors Smaller pixels Faster
electronics
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Coherent radio detection
E. Zas
Radio wavelength (?) gt Emission length (l,W)
e, ? interactions have charge symmetry But matter
only has electrons!!
10 charge excess
many projects under consideration
FORTE
ANITA
GLUE
LOPES
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Ultra High Energy Neutrinos
D.F.Torres, L.A.Anchordoqui
can escape from dense astrophysical environments
and propagate to the Earth unscattered !
BUT no measurements above E gt 106 GeV !
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The Neutrino Connection
F. Halzen
Cosmic beam dumps
Black Hole
Radiation or dense clouds enveloping black hole
or CMB photons
? ?
Intense secondary ? and ? beams!
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Expected Fluxes
Cosmogenic neutrinos
P? CMB? n p p ? µ ? µ
Cosmic Zevatrons
AGN, GRB, supernovae,
Z-bursts
? ?r ? Z ? hadrons
Top-down
Superheavy relic particles, supermassive dark
matter, topological defects,

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Constraints from EGRET
An example The Z-burst
mechanism neutrino-?-ray sources
Fargion,Weiler,Yoshida
Can lead to an overproduction of ?s in the GeVs
Kalashev, Kuzmin, Semikoz, Sigl, hep-ph/0112351
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?? regeneration
?? energy degradation
109 GeV
106 GeV
Fraction of Earth diameter
(hep-ph/0405056)
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Horizontal air showers
?e quasi- horizontal
Up going (?? regeneration)
High energy neutrinos can be detected !
(see D.Fargion talk, E. Zas recent
review)
?? Earth-skimming
S.Bottai
AUGER is well suited to study very inclined air
showers but the expected ? rates are small
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Particle Physics with UHECR beams
High Energies
mGUT ? 1024 eV ?Lorentz ? 1011
Ebeam ? 1019 1020 eV
vsLHC ? 14 TeV
vs ? 100 400 TeV
But
Low fluxes
0.1 event/km2/year
xF? 0
Limited kinematic region
Large statistical fluctuations
Poor detection capabilities
Huge detection area
Auger ? 3000 km2
Earth surface ? 108 km2
EUSO ? 200 000 Km2 . 0.1
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proton (anti)proton cross-sections
High heavy quark production
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Sokolsky 2004
Standard Physics
Cross-section measurements
sp-air
Gonzalez-Garcia et al.. 1994
Poniatowski 2003
sCharm
sp-p
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New Physics
New Particles
Extra Dimensions
Higgs
Gravity can be much stronger if there are n
compactified extra dimensions. Planck mass can be
as low as 1 TeV !
SUSY
Excited leptons
BH can be created !
Leptoquarks

Tests of Lorentz Invariance
Radiactive ? decay ? ? e ?
Ultra high energy stable Pions
Longitudinal development of UHECR air showers
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Excited leptons, Leptoquarks
sensitivity for e (f - f )
hep-ph/0412345
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Black Hole decay and detection
Instantaneous, thermal and democratic decay
through Hawking evaporation.
BH gives horizontal EAS starting deep in the
atmosphere
bounds (MD, n) from Flys Eye and AGASA
Expected nb of events (Auger)
MD
Feng, Shapere (2001)
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The double bang signature
(hep-ph/0405056)
The production and decay of a BH is followed by
the decay of an energetic tau lepton
At EUSO a few of BH events have a double bang
topology
A BH double bang viewed by EUSO
of BH double bang events in EUSO
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