Cosmic Rays. Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon

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1 Cosmic Rays Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon Nobel Prize in 1936 Origin of high energy cosmic rays is still not completely understood but currently thought to be associated with shock waves of supernovae remnants (SNR) Cosmic ray physics continues to provide a window on the most energetic objects in the universe (supernovae, pulsars, AGN, black holes, etc.) 1

2 Cosmic Rays 2

3 Primary cosmic rays Cosmic Rays Accelerated at astrophysical sources Secondary cosmic rays Interaction of primaries with interstellar gas Interaction of primaries with earth s atmosphere The magnetic field of the interstellar medium (3μG) is sufficient to confine all but the most energetic (>10 15 GeV) cosmic rays within the galaxy Lower energy (MeV/GeV) cosmic rays are affected by the solar wind (e and p ejected from the sun) and the earth s geomagnetic field 3

4 Sources of Cosmic Rays Solar protons dominate < 100 MeV where the solar wind shields protons from outside the solar system For E < ev acceleration mechanism is thought to be shock wave of SNR 1st order Fermi 2nd order Fermi Shock front Magnetic clouds 4

5 Sources of Cosmic Rays The origins of cosmic rays above the knee region are less certain The origins of cosmic rays above ev must be from relatively nearby because of the GZK (Greisen-Zatsepin-Kuzmin) cutoff Above ~5x10 19 ev, interactions of cosmic ray protons with the cosmic microwave background can produce pions This can continue until their energy falls below the threshold We ll hear about the Pierre Auger experiment (3000 m 2!) later in the course One of the main objectives of this experiment is to probe the GZK region 5

6 Solar Wind Lower energy cosmic rays are affected by the solar wind and the earth s geomagnetic field 6

7 Earth s Magnetosphere 7

8 Differential intensity I N (E) ~ 1.8 x 10 4 E -2.7 Units are nucleons / m 2 s sr GeV Composition 79% protons 15% He Cosmic Rays 8

9 High Energy Cosmic Rays 9

10 High Energy Cosmic Rays 10

11 High Energy Cosmic Rays 11

12 High Energy Cosmic Rays 12

13 Cosmic Ray Showers 13

14 Cosmic Ray Showers 14

15 Cosmic Ray Muons Relevant particle decays (and CC) π K μ + μ ν e ν ν + μ + μ ν e μ ( -8 τ = s, Br = 1.0) ( -8 τ = s, Br = 0.63) ( -6 τ = s, Br = 1.0) μ Most muons are produced high in the atmosphere (15 km) and lose about 2 GeV in ionization loss before reaching the ground Mean energy at the ground is ~ 4 GeV The energy spectrum is ~flat below 1 GeV Follows primary spectrum between GeV Steeper slope at higher energies because of secondary pion interactions 15

16 Cosmic Ray Muons 16

17 Cosmic Ray Muons For muons with E > 1 GeV the integral intensity at sea level is 70 m -2 s -1 sr -1 This translates into a rule of thumb for a flux through horizontal detectors of 1 cm -2 min -1 For 15x15 cm 2 counter this is ~ 4 / s For muons with E ~ 3 GeV the angular distribution is ~ cos 2 θ 17

18 Cosmic Ray Neutrinos Considering π/k and μ decays, we expect by counting that v μ /v e ~2 Experiments observe v μ /v e data / v μ /v e predicted = 0.63 ± 0.3 ± 0.5 L up ~13,000 km L down ~15 km 18

19 Calculating the Cosmic Ray Flux Our setup for a 2x coincidence looks like 19

20 Calculating the Cosmic Ray Flux Then fraction f of muons through top counter T and area element A is area of T f = 2 4πd area of bottom counter B coincidence rate RTB = RA f area of A RA Runit area Runit area = and Flux F area of A 4π area of B area of T coincidence rate RTB = F ε 2 T ε B d this can be used to calculate F 20

21 21 Efficiency Error There are two common ways to do this neither is strictly correct A better calculation uses Bayes theorem but gives a difficult solution to implement Poisson Problems with k=0 and k=n i and / let + = = = = N k N k N k N k N k i i δ δ ε δ δ δ ε ε

22 Binomial Efficiency Error Can be considered because the efficiency is just the probability of the third counter successfully passing the coincidence condition Recall for the binomial distribution k σ δ = Nε k = ε σ k N ( 1 ε ) and taking ε = ε = N k N Problems with this when k=0 or k=n 22

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