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Matter/antimatter asymmetry in the Universe?The CR antimatter component and
its direct detection
Baikal summer school, July 2005
P.Spillantini, University and INFN, Florence, Italy
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GeV|
TeV|
PeV|
EeV|
ZeV|
High Z[ENTICE, ECCO]
Light elements and Isotopes
[ACE]
Antiparticlesand Antinuclei
[BESS, PAMELA, AMS]
Elemental Composition[CREAM, BEAR,
ACCESS?,NUCLEON?, INCA?, PROTON-5?]
Direct detectionBalloons &
Satelites
Indirect detection (EAS)
[arrays & florescence]
Extreme Energy CR
AUGER, TUS, EUSO,KLYPVE?,OWL??
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Nucleus
Star
galaxy
Cluster of galaxies
Super-cluster
??
Anti-Nucleus
Anti-Star
Anti-galaxy
Anti-Cluster of galaxies
Anti-Super-cluster
Anti - ??
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Antiparticles and CR
difficulties needed
for antip: secondary production
high energy ( 100 GeV/n)
high energy ( 1 TeV)
long diffusion timelong pathgalactic wind
for antiN:
CP violation Sakharov conditions
All Matter Universe
Matter and antimatterin separated domains
Symmetric Cosmologies
Asymmetric Cosmologies
Both possible inBig Bang theories
It is possible rely only on observationsantip spectrum
antiN search
From e.m. observations Only local asymmetry(~10-8 of the Universe volume)
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(no assumption onantiHe spectrum)
AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)
ANTIMATTER LIMITS
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Antiproton Positron
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International Space Station “FREEDOM”
Hubble Space
Telescope
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CGRO AXAF(CXO)
HST SIRTF
+ Particle-Antiparticle Superconducting Magnet Facility (ASTROMAG)
+Very Long
Base Interferometer
(VLBI)
+
Advanced Composition
Explorer (ACE)
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Experiments approved for the first phase of the ASTROMAG facility
WIZARD: antiparticle spectra, antinuclei, etc..(USA, Italy, Sweden, Germany)
LISA: elemental and isotopic spectra, etc. (USA, other??)
MAGIC-SCINATT: elemental composition at knee (USA, Japan)
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Balloon Flights
-- BESS (93, 95, 97, 98, BESS (93, 95, 97, 98,
2000)2000)
-- Heat (94, 95, 2000) Heat (94, 95, 2000)
-- IMAX (96) IMAX (96)
-- [BESS Long duration flights [BESS Long duration flights
(2004)](2004)]
(Wizard Coll.)
- - MASS – 1,2 (89,91)MASS – 1,2 (89,91)
--TrampSI (93)TrampSI (93)
-- CAPRICE (94, 97, 98) CAPRICE (94, 97, 98)
-- [ [ in flight (2004?)] in flight (2004?)]
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New Generation ofAntimatter Researches
in Cosmic Rays
a) Longer duration ballooning b) Experiments in space
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payload
services
HeAir Air
Class A Balloons2.8 Mm3 @ 5 g/cm2
lifting power ~ 11t
Balloon 5 tservices 3 tpayload 3 t
Open Balloons
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Km
0 C°-100
40
Atmospheric temperature versus Altitude
0
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BESS - Polar
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New Generation ofAntimatter Researches
in Cosmic Rays
b) Experiments in space
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PAMELA
Positrons 50 MeV - 270 GeV
Antiprotons 80 MeV – 190 GeV
Limit on antinuclei ~7 10-8 (He /He)
Electrons 50 MeV – 2TeV
Protons 80 MeV – 700 GeV
Nuclei < 300 GeV/n (Z 8)
study of the solar modulation after the 23rd solar cycle maximum.
GF 20.5 cm2 srMass 480 KgDimensions cm3 120 x 40x45 Power Budget 345W
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Spillover of p on antip = 0.2 of the antip flux
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Distortion of the secondary positron fraction induced by a signal from a heavy neutralino.
Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino.
P.Picozza and A.Morselli,astro-ph/0103117
standard
Expected data from Pamela for two years of operation are shown in red.
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BESS (2004+2006 LDB flights)
ANTIMATTER LIMITS
AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)
(2005-8 )
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Razzo Soyuz
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(no assumption onantiHe spectrum)
AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)
BESS (2004+2006 LDB flights)
AMS 02 (2005-8)
(2003-6 )
ANTIMATTER LIMITS
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End of the movie!!