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Particles and Cosmic RaysParticles and Cosmic Rays
Particle Physics Group
University of Birmingham
Prof. Cristina Lazzeroni
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Particles in the wildParticles in the wild
Accelerators
Radioactivity
Cosmic rays
E=mcE=mc22 Energy Matter
New particles are produced
Particles in captivity
Particles in the wild}
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Cosmic Ray discoveryCosmic Ray discovery
Hess, 1912: Balloon flight
Electroscope would discharge much faster at higher altitude
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Cosmic Ray discoveryCosmic Ray discovery
Balloon flight in near-total eclipse : Still higher radiation at higher altitude Ruled out Sun as radiation source
"The results of my observation are best explained by the assumption that a radiation of very great penetrating power enters
our atmosphere from above."
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Cosmic Ray discoveryCosmic Ray discovery
1920: Millikan called them “cosmic rays” and believed they were energetic photons
1927: evidence of variation of cosmic rayintensity with altitude indicating deflection by geomagnetic field
Charged particles
1937: Rossi and Auger Primary and secondary cosmic rays
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Cosmic raysCosmic rays
The field of Particle Physics originated fromcosmic ray research
Muon, pion, positron, kaon, Lambdaall discovered in cosmic rays
Cosmic rays: Proof of special relativity !
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A Cosmic ShowerA Cosmic Shower
Primary Cosmic Ray
Pions
Muons, Electrons &Neutrinos
SecondaryCosmicRays
40km
60km
Ground
Impact onnucleus
Decay ofPion
20km
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Particles in the wildParticles in the wild
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Primary high energy cosmicray in upper atmosphere : 85% protons 12% alpha particles 2% electrons Neutrinos, heavier nuclei
Collision with nucleus Initiates “cascade”
Secondary cosmic rays Higher energy primary
⇒ larger secondaryshower
Charged particles at Earth’ssurface are mainly muons.
Particles in the wildParticles in the wild
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ShowersShowers
Some spreadingBut tends to maintain
original direction
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Particle wheelParticle wheel
forces
leptons
quarks
MUON
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MuonsMuonsMuons:Minimum ionising particles
Hence long, straight tracks200 times more massive than electron Sea level: 150 muons/sec
per 1 square metre
classically
Proper timeEarth time
relativistically
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Cosmic rays measurementsFlux of cosmic rays
Detector geometry dependence
Angle wrt vertical
Muon lifetime
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Vast energy rangeVast energy range
knee
ankle
ProtonsAt LHC
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Where they come fromWhere they come from
The Sun’s solar wind neutrinos photons Electrons, positrons
Shock-waves aroundsupernovae in Milky Way
Unknown : extra-galactic ?Neutron stars ? Acceleratedby something ?
Possible sources,in order of energy:
Fusion reactions, only lower energy
Can’t leave Milky Way due to Vast magnetic fields
Abundance of elements similar to Earth, except for large quantity
of Lithium, Beryllium and Boron
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EnergyEnergy
In 1 m2
~1 particle/sec with 1 GeV
1 per km2 1 particle/year with 1020 GeV
108 time the LHC energy
Solar wind
shockwave
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GZK GZK cutoffcutoffCosmic microwave background, 2.7 K : n=400 photons per cm3
Protons in cosmic rays may interact with photons:
p + γ → π0 p p + γ → π+ n
Threshold energy above which the interaction is possible:Particles produced at rest
Cross-section
Mean free path
~650 times the radius of Milky Way
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Cosmic showers measurements
How many cosmic particles with an energyabove 1016 eV reach the earth?
Where do they come from? Are theresources in our Milky Way?
Can one determine the GZK-cut-off?
Variation with latitude, altitude;Night/Day variation; Seasonal variation
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Further research
Improve shower models
Influences from the atmosphere
Correlation with weather
Correlation with Sun activity
International project HiSPARC on cosmic showers detectors for schools: reached ~20 schools in UK
If you are interested, please contact me
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Interaction of charged particlesInteraction of charged particles
Basic physics:
When a high-energy charged particle crosses a material,it may transfer energy to the electrons in
the material’s atoms
This may result into excitation of the atom into a higher energy level; the excited state immediately
decay emitting a scintillation photon
This may also result in ionization if an electron gains enough energy to escape from its orbit, leaving behind a
positively charged ion
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The Scintillation Counter
Charged particle passesthrough plastic scintillatorleaving a trail of ionisation
Ionisation recombines,emitting light in alldirections.
Light bounces aroundscintillator and somefraction enters light guide.
The perspex light guidedirects the light on to thephotomultiplier tube (PMT).
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Photons hit PMT window (metallised glass): cathode.
Via the Photoelectric Effect, electrons are emitted
Electrons are attracted to 1st dynode and from onedynode to the next by an electric field
at each collision with a dynode, 2 or 3 electrons areemitted, i.e. amplification at each stage
Electrical signal produced at anode.
Anode
PhotonElectron
DynodesPhotocathode
γ + atom → ion + e-
Photomultiplier Tube
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Detecting cosmic rays
If a charged particle (e.g. a cosmic ray) passesthrough both scintillators, it will produce anelectrical pulse from each
If these signals occur almost exactly a thesame time, we assume that these “coincidences”have been produced by a charged particlepassing through both scintillators.
The electronics counts how many coincidenceshave been detected
This counter tells us directly how many cosmicrays have passed through the two scintillators ina given time.
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ConclusionsConclusions
Cosmic rays offer a natural laboratory
Real-science experiments can be donewith the detectors shown
Great way to start with particlephysics !