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Lecture 1: Introduction. Cosmic-ray spectrum and measurements. Spectrometers ( D A = 1 resolution, good E resolution). Air showers. Calorimeters (less good resolution) + TRACER. Air-shower arrays on the ground to overcome low flux. Don’t see primaries directly.
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Lecture 1: Introduction Cosmic-ray spectrum and measurements PS638 T. Gaisser
Spectrometers (DA = 1 resolution, good E resolution) Air showers Calorimeters (less good resolution) + TRACER Air-shower arrays on the ground to overcome low flux. Don’t see primaries directly. Primary spectrum Knee Ankle Current questions PS638 T. Gaisser
Spectral Energy Distribution (linear plot shows most E < 100 GeV) (4p/c) Ef(E) = local differential CR energy density Energetics of cosmic rays • Total local energy density: • (4p/c) ∫ Ef(E) dE ~ 10-12 erg/cm3 ~ B2 / 8p • Power needed: (4p/c) ∫ Ef(E) /tesc(E) dE galactic tesc ~ 107 E-0.6 yrs Power ~ 10-26 erg/cm3s • Supernova power: 1051 erg per SN ~3 SN per century in disk ~ 10-25 erg/cm3s • SN model of galactic CR Power spectrum from shock acceleration, propagation PS638 T. Gaisser
Solar flare shock acceleration Coronal mass ejection 09 Mar 2000 PS638 T. Gaisser
SOHO/ LASCO CME of 06-Nov 1997 PS638 T. Gaisser
Particle with E1 u1 ~ 4/3 V Forward shock Contact discontinuity, V Shocked ISM SN ejecta u1 ~ 4/3 V E2 = x E1 Supernova blast wave acceleration Unshocked ISM Supernova progenitor SNR expands into ISM with velocity V~ 104 km/s. Drives forward shock at 4/3 V TSN ~ 1000 yrs before slowdown Emax ~ Z x 100 TeV PS638 T. Gaisser
Composition PS638 T. Gaisser
Four ways to plot spectra • Particles per GeV / nucleon • for propagation/fragmentation in gas • Particles per GV / nucleon • for propagation/acceleration in magnetic fields • Nucleons per GeV / nucleon • for production of secondaries in the atmosphere • Particles per GeV / nucleus • for air shower experiments PS638 T. Gaisser
Two kinds of measurements Hodoscope: e.g. EAS Inclusive: e.g. muon flux PS638 T. Gaisser
Two kinds of measurement at accelerators • Spectrometer measures inclusive cross section • for example, the HARP experiment • 4π detector • Goal is to detect all particles produced in an interaction • for example, a collider detector like Atlas PS638 T. Gaisser
Definition of energy spectrum • Number of particles per m2 sr s • i.e. Rate per unit area per solid angle • Differential: dN / d ln(E) = E x dN / dE • Preferable to dN / dE for power-law spectrum • δE / E ~ constant, so binning of data is logarithmic • Integral: N(>E) per m2 sr s • If dN / d ln(E) ~ K (E)-gthen • dN / d ln(E) = g x N(>E) PS638 T. Gaisser
Acceptance • Detector acceptance = area x solid angle • Example: • 2 parallel planes of area A1, A2 • Separation d >> sqrt (A1) and d >> sqrt(A2) • Approx acceptance = A1 x A2 / d2 • In general • A x Ω = ∫∫dx1dy1 x ∫ dφ∫ sin(θ) dθ • For each point inside A1 constraints on the solid angle integral depend on (x1,y1) and require the vector in the (θ,φ) direction to pass inside A2 • Evaluate integral by Monte Carlo PS638 T. Gaisser
CAPRICE spectrometer AΩ ~ 0.3 m2 x 0.3 m2 / 10 m2 ~ 0.01 m2 sr CAPRICE 1998 PS638 T. Gaisser
BESS spectrometer AΩ ~ 0.085 m2 sr PS638 T. Gaisser
Magnetic spectrometer • Momentum measurement • Gyroradius: rL = Pc / (zeB) ≡ R / B • Rigidity: R = Pc / ze (units = GV) • Measure z with dE / dX in scintillator ~ z2 • P = A x pN; pN = momentum / nucleon • Example: 100 GeV/c proton in B = 104 Gauss • rL = 333 m • Maximum Detectable Momentum (MDM) • δp ~ eB┴ δt from Lorentz force equation; δt ~ L / c • δx / L ~ δp / p ~ eB┴L / (pc) (pc)max ~ eB┴L2 / δxmin • Example: for B┴L2 = 0.8 Tm2, (pc)max~ 240 GeV for protons in a detector with 1 mm spatial resolution PS638 T. Gaisser
Time of Flight (TOF) • Two scintillators separated by L • β = L / (cΔt) • δβ = -(L/cΔt) x (δt/Δt) = β x (δt/Δt) • δβ / β ~ δt / Δt • Need sub-nanosecond time resolution to measure velocity of a relativistic particle over a scale of 1 m PS638 T. Gaisser
Cherenkov radiation Cherenkov angle: cos(θc) = 1 / (βn) Threshold: β > 1 / n Intensity: ~ z2 x sin2(θc) = z2 x [1 – 1 / (βn)2] • Uses: • Threshold detector, e.g. separate e+ from p • Use gas or other material with small n ~ 1.003 • Measure energy near threshold • Use plastic or clear material with n ~ 1.5 PS638 T. Gaisser
TRACER uses transition radiation PS638 T. Gaisser
Compilation from RPP Note TRACER measurements in 3 energy ranges PS638 T. Gaisser
Balloon-borne calorimeters • RUNJOB emulsion chamber • Russian-Japanese collaboration • Detector material interleaved • with sheets of photographic emulsion • Primary ID (pink) • Interaction in Target (yellow) • Secondaries separate (blue) • Photons make cascades in • calorimeter (violet) • Calibrate at accelerator • Important for overlap with EAS PS638 T. Gaisser