HADRONIC INTERACTIONS - NTNUweb.phys.ntnu.no/~mika/lipari.pdf · in the modeling of hadronic...
Transcript of HADRONIC INTERACTIONS - NTNUweb.phys.ntnu.no/~mika/lipari.pdf · in the modeling of hadronic...
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UHECR and
HADRONIC
INTERACTIONS
Paolo Lipari“Searching for the originof Cosmic Rays”Trondheim 18th June 2009
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Mass A
Energy
Hadronic interactionModeling
~60 years of UHECR
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Energy measurement problem “solved”. “Fly's Eye”
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1st Fly's Eye
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Observed Light
Emitted Photons
Shower Size
Geometry Atmospheric Absorption
FluorescenceYields
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SmallModeldependence
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Area Energy
Shape depends on :● Primary Identity● Interaction Model
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COMPOSITION of UHECR
Xmax
Fluctuations of Xmax
Other methods
Very high astrophysical importance
Controversial - inconsistent observations.
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AUGER ICRC 2007
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Elongation rate corrected for detector acceptance andcomparison with previous results
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The “theory curve” <Xmax(E)> is determinedby the parameters that describehadronic interactions.(and by their energy dependence).
Interaction Lengths Multiplicity Inclusive Spectra .......
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Xmax and the Composition of Cosmic Rays
Logarithmicgrowthof average Xmax with energy
Proton Showers
Mass dependence
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Xmax and the Composition of Cosmic Rays
Logarithmicgrowthof average Xmax with energy
Proton Showers
Mass dependence
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Obtain the average mass and its variation with energy
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The importance of “CORNERS”(when real)
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“METHODOLOGY”
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AstrophysicalInformation
HadronicInteractions
C.R. DATA
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AstrophysicalInformation
HadronicInteractions
C.R. DATA
From Accelerator Data + Theory Astrophysics
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AstrophysicalInformation
Data
HadronicInteractions
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Naive 2-component model
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Sibyll-Interpretation
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Sibyll-Interpretation
Compositionis Mixed
50% p50% Fe
Compositionbecome heavierwith increasing Energy
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QGSJet-Interpretation
Compositionis Mixed
60% p40% Fe
Composition:Indication (1.5 s)of moderate increaseof A with Energy
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How can we include systematic uncertaintiesin the modeling of hadronic interactionsin the estimate of propertiesof Cosmic Rays?
“Spread” of predictions for diferent model.
Overestimate ? Underestimate ?
Some models arelower quality.
Perhaps we are missingsomething important.
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HadronicInteractions
C.R. DATA
“Alternative Approach” to the problem.
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“CONSISTENCY”
Diferent Methods to measure same physical quantity must agree
Fluorescence versus Surface detection
Xmax versus “Muons”
.....
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AstrophysicalInformation
HadronicInteractions
C.R. DATA
From Cosmic Ray Data Hadronic Interactions
“Astrophysical Composition Methods”
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AstrophysicalInformation
HadronicInteractions
C.R. DATA
From Cosmic Ray Data Hadronic Interactions
“Astrophysical Composition Methods” 1 < A < 56 (very likely)
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“Astrophysical Composition Methods”
Energy Spectrum “imprints” of Energy Loss
“Cosmic Magnetic Spectrometer”
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Features in the Cosmic Ray Energy Spectrumcan in principle give informationon the nature of the particle
Interpreted as the efectof energy loss during propagationfrom their extragalactic sources.
Known target: 2.7 K CMBR radiation feld
Energy Thresholds for protons :
“GZK”Pair Production
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Berezinskyet al.
Inject Smooth power lawSpectrum.
Let propagationleave its“imprint”on the shapeof the spectrum.
“ANKLE” -->“DIP” e+e- production
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“COSMIC MAGNETIC SPECTROMETER”
Correlations of the Highest-EnergyCosmic Rays with Nearby Extragalactic Objects (AGN)
AUGER RESULTB, ZConstraint on :
Protons are preferred [....? ....]
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Deviation in GALACTIC Magnetic Field
Deviation in EXTRA-GLACTIC Magnetic Field
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IF one accepts (at least for the sake of discussion) the astrophysical hints of a proton dominated composition....
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ProtonLine!! (?)
IF one accepts (at least for the sake of discussion) the astrophysical hints of a proton dominated composition....
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Electromagnetic Showers
versus
Hadronic Showers
Toy modeldiscussion.
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Vertices : theoretically understood(and scaling)
Electromagnetic Showers
Radiation Length(Energy independent)
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Electromagnetic Showers
Logarithmicgrowth of thepenetration.
EnergyConservation
Elongation rate = 85 (g/cm2)/decade
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Heitler toy modelfor electromagnetic showerws
“Electron-photon”
particle
Splitting length λCritical energy ε
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Shower development in Heitler toy model:
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Proton Shower Vertices : theoretically not understood (and not exactly scaling)
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“Hadronic particle”
Hadronic vertex
1
1-f
f/mEnergy sharing1 → (1-f) + f/m + f/m + f/m + f/m + .......
Hadronic Interaction Length
“Hadron”
Interaction Length Λ“Inelasticity” f“multiplicity m
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Hadronic shower
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Λ, inelasticity, hardnessHadronic parameters
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Hadronic shower in toy model.
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[integer]
Hadronic interactionparameters
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IF Λ , and the other
hadronic interactions parametersare energy independent
“Elongation rate”is equal to theradiation length
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IF Λ , and the other
hadronic interactions parametersare energy independent
“Elongation rate”is equal to theradiation length
Energy dependent parameters: Elongation rate changes
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Scaling model : 85 (g/cm2)/decade
Increasing crosssections
Softerspectra
Elongation RateFor protons
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p
π
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Exactly Scaling Interactions
λπ=const.
λp, λπ=const.
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Exactly scaling models Diferent elongation rate
λπ=const.
Best ft
λp, λπ=const.
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Introduce Energy dependent softening of the spectra
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It is possible to “reproduce” A “desired” composition with (in this example) an appropriate gradual softening of secondary meson spectra.
Possible also to introduce A faster rise of the cross section
Ambiguities ! May possibilities.... How can we distinguish among them ?
Predictions for LHC !!?
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It is possible to “reproduce” A “desired” composition with (in this example) an appropriate gradual softening of secondary meson spectra.
Possible also to introduce A faster rise of the cross section
Ambiguities ! May possibilities.... How can we distinguish among them ?
WARNING !!Perhaps : this approach is completely incorrect the mass composition is indeed mixed .... We have to rely on [accelerator data + theory]
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Fluctuations on Xmax
Very Interesting an puzzling piece of information !
Not confrmed by HIRES
Potentially very important
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Comparison of data and p-QGSJET02 fuctuation widthsUse 2-sigma truncated gaussian width to ft Xmax distr.Detector resolution is NOT deconvoluted!
HIRESP.Sokolski
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Overall comparison of Xmax data with QGSJET02 p and FE
HIRES
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Overall comparison of Xmax data with QGSJET02 p and FE
HIRES
AUGER PeopleKeeping this distribution for themselves At the moment.
Good work to you !
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RMS [Xmax] decreasing with energy !
Need robust confrmation.
What does it imply ?
Composition getting heavier !
Proton shower fuctuationsbecoming smaller. Much larger cross sections (shorter interaction length) Particle production properties. (seems unlikely to me....) [but ....]
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THEORY
Construction of Hadronic Models
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Leading nucleon∼ 50% of energy
π ο → γ γElectromagnetic Shower
Interaction
Decay
HADRONIC INTERACTIONS
Inclusive spectra of secondary particles
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Ebeam
= 175 GeV FERMILAB SAS pp Brenner et al (1982)
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Phenomenological Evidence forFEYNMAN SCALING
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NUCLEAR efects: pp vs p-12C
NA49
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Hadronic Interactions
Composite (complex) ObjectsMultiple interaction structure QCD
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Deep Inelastic Scattering
Develop quarkfragmentation Modelfrom e+ e- Scattering
Data consistentwith QCD
1st Slide from R.Feynman seminar in 1976.
From R.Field
ISR high pTPion production
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Parton Distribution Functions
HARD scattering
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Field -Feynman : Quark - Fragmentation
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PartonDistributionFunction
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Where does the approximateFeynman scaling comes from ?The (iterative) Fragmentation of oneCOLOR STRING produces a SCALING SPECTRUM of HADRONS
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Basic Structure ofa NON difractive PP interactionsis made of TWO STRINGS
hard/semihard interactionsresult in additional strings
Diquark
Quark
Color Structure
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Most particles inFragmentation RegionsDescribed by the “beam remnants strings”
PythiaMC
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EXTRAPOLATION to HIGH ENERGY (Pythia pp)
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EXTRAPOLATION to HIGH ENERGY (Pythia pp)
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PROTON Spectra (elasticity spectra)
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PYTHIA PROTON Spectra
Antiprotons
protons
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PROTON Spectra (elasticity spectra)
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Estimate of the average number of Elementary interactions per pp scattering
“Spatial Distribution” (Transverse coordinates) of the partonic constituents.
Fluctuations of the “parton confguration” of an interactighadron.
MULTIPLE INTERACTIONS
[proton spin]
Beyond PDF'sParton Distribution Functions
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Hadrons crossing time short
“Snapshot” of the Parton Confguration.
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Very Important potential of LHC
7 + 7 TeV PP collider
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Problems at theBeginning of Commissioning
19th september 2008
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Jorg Wenninger : june 2008 Hadron Collider summer school
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FNAL June 4, 2009 97
LHC Physics in 2009/2010
First beams: First beams: very early physics - rediscover SM physicsrediscover SM physics Detector synchronization, in-situ alignment and calibration
10 pb10 pb-1-1: Standard Model processes measure jet and lepton rates, observe W, Z bosons frst lookfrst look at possible extraordinary signaturesextraordinary signatures…
Measure Standard Model ProcessesMeasure Standard Model Processes (at 10TeV need ~ 30pb-1):~ 104 Z → e+e- (golden Z’s for detector studies (1%))
~ 105 W → eν~ 103 ttbar (measure σ to 10%)
Initial Higgs searches and searches for physics beyond the SM
Background for new physics
Need to understand very well
30 pb30 pb-1-1
> 200 pb> 200 pb-1-1Entering Higgs discovery era and explore large part of SUSY and new resonances at ~ few TeV
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Event rate
On tape
Level-1
Higgs discoverygolden channel
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Cross sectionMeasurements
Prediction for LHC at sqrt[s] = 14 TeV
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CROSS SECTION MEASUREMENT
Optical Theorem
[Luminosity Determination]
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PROBLEM of PHASE SPACE COVERING
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LHCF Calorimeterfor neutral particlesin the very forward region
Two non-identical Detectors
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We are studying at the same time
“Gigantic Astrophysical Beasts” Millions of light years away
Length scale 10+24 cm
Microscopic
Partonic constituents of matterLength scale 10-13 cm
Exciting Difcult
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e+
π ±
Κ ±
ParticlePhysics
Cosmic RayPhysics
Andersondiscoveryof positron
Occhialini , Powell
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Galactic/ExtragalacticCosmic Rays