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QuarkNet Oregon

QuarkNet Oregon. Ray Frey, Dept of Physics, UO. What is QuarkNet? National program, funded by NSF and DoE High-energy physics and the public (and our government) SSC  LHC Getting the public (schools) involved in (HEP) inquiry Demystification of basic science research

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QuarkNet Oregon

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  1. QuarkNet Oregon Ray Frey, Dept of Physics, UO • What is QuarkNet? • National program, funded by NSF and DoE • High-energy physics and the public (and our government) • SSC  LHC • Getting the public (schools) involved in (HEP) inquiry • Demystification of basic science research • Familiarity with the forefront research questions being studied • QuarkNet Oregon • HEP at UO  HS teachers  students • Research questions and methodologies • Activities surround annual 1 week workshops • Lectures and tours • Cosmic ray detectors for each involved teacher • Participation in national QuarkNet events • Looking for new teachers to get involved ! QuarkNet Oregon 2008, R Frey

  2. Supports learning by inquiry. • Provides teachers and students with real research opportunities in particle physics. • Encourages national and international collaboration among students, teachers and scientists. QuarkNet Oregon 2008, R Frey

  3. The Large Hadron Collider (LHC) • CERN, Geneva; startup 2008 • collisions of 7 TeV protons and 7 TeV protons • a billion collisions/second • The Standard Model of HEP appears to break down at E1 TeV • We anticipate New Physics but don’t know in what form it will appear • The Oregon HEP group collaborates on the Atlas experiment at the LHC • A goal of QuarkNet is to help bring the excitement of the LHC to the classroom QuarkNet Oregon 2008, R Frey

  4. Cosmic Rays • Outside earth’s atmosphere, these are charged particles, 86% protons • These primary cosmic ray particles interact with air high in the atmosphere (15 km), creating showers of secondary particles • By time the secondaries reach sea level, muons dominate the flux • The detectable (vertical) rate at sea level is 1/cm2/min (e.g. in CRDs) • Throughout our galaxy, CRs have an energy density of 1 eV/cm3 • Starlight: 0.6 eV/cm3 • CMB: 0.26 eV/cm3 • 30% of natural radiation (sea level) • Provide charge and seeds for lightning from QuarkNet CRD manual QuarkNet Oregon 2008, R Frey

  5. energy and origin of primaries • Steeply falling, power law energy spectrum • For E1014 eV, spectrum and flux are consistent with acceleration by shock waves from supernovae (“Fermi acceleration”) • For larger energy, mechanism is unknown (black hole at galactic center??) • For E1019 eV, protons would not be captured by galactic magnetic field (310-10 T) • pt [GeV] = (0.3q/e)B[T] R[m] • So higher energy CRs must be extra-galactic... but GZK cutoff... QuarkNet Oregon 2008, R Frey

  6. Auger CR observatorywww.auger.org • Sites in Mexico and Argentina • Array of detectors: (40x1.5 km)x(40x1.5 km) • GZK: extragalactic CRs attenuated: p +  (CMB)  +  p + , n + + • 411 CMB photons/ cm3 ; E=k2.7K=2.410-4 eV • No protons >1020 eV from further than 5 Mpc • Summer 2007: No excess above GZK cutoff • Fall 2007: UHE CRs associated with AGNs QuarkNet Oregon 2008, R Frey

  7. The cosmic ray showers • Primaries interact in the atmosphere – the maximum production of pions and muons is at z15 km, making showers of (mostly) short-lived particles.(e.g. pion () lifetime is 2.610-8 s) • Characteristic shower angle:   pt / pL  0.2 GeV/E • The long-lived secondaries are: • e, photons: mostly absorbed • neutrinos (): practically invisible • muons (): =lifetime is 2.210-6 s • Without time dilation, muons would travel dc=660 m, with a survival fraction e-0.66/15 10-10 • Instead, for a 10 GeV muon, 10/0.1=100, then mean distance is 66 km. (OK) QuarkNet Oregon 2008, R Frey

  8. cosmic rays at earth’s surface • Predominantly muons • Detectable (vertical) flux is 1/ cm2/ min • Mean energy  4 GeV • Originate at altitude of 15 km, on average • The very low energy muons (1-3 GeV) mostly decay • 15 km decay length corresponds to a 2.4 GeV muon • The higher energy muons lose about 2 GeV (on average) due to ionization in the atmosphere • and about 4 MeV / cm in concrete QuarkNet Oregon 2008, R Frey

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  11. QuarkNet cosmic ray detectors • 4 scintillator paddles and photomultiplier tubes • requires only wall plug power • GPS receiver • electronics card and computer interface • measure cosmic ray rates in various configurations • datasets written to computer • combine with other setups • muon lifetime experiment QuarkNet Oregon 2008, R Frey

  12. a community of cosmic experimenters • A “minimum ionizing particle” (MIP), e.g. a typical cosmic ray muon, passes through a plastic scintillator, depositing (on average) about 2 MeV / cm (ionization of the plastic) • Typically, the scintillation yield is 1 photon per 100 eV of ionization  2104 photons/ cm for each muon • Some fraction of the photons are collected at the photomultiplier tube (PMT) – depends on geometry and indices of refraction • The photocathode of the PMT converts a blue photon to an electron with efficiency of 10% • The PMT multiplies an electron by a factor 106 • depends on high voltage setting, number of stages N (N=10 to 12 typically), and geometry • Gain  (few)N QuarkNet Oregon 2008, R Frey

  13. a community of cosmic experimenters QuarkNet Oregon 2008, R Frey

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