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Relativistic Magnetic Monopole Flux Constraints from RICE

Relativistic Magnetic Monopole Flux Constraints from RICE. Daniel P. Hogan University of Kansas RICE Collaboration IGC Inaugural Conference 9 August 2007. Magnetic Monopole Overview. Dirac, 1931 Gut Scale Monopoles ~ 10 17 GeV Diluted by inflation “Intermediate Mass Monopoles” (IMM’s)

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Relativistic Magnetic Monopole Flux Constraints from RICE

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  1. Relativistic Magnetic MonopoleFlux Constraints from RICE Daniel P. Hogan University of Kansas RICE Collaboration IGC Inaugural Conference 9 August 2007

  2. Magnetic Monopole Overview • Dirac, 1931 • Gut Scale Monopoles ~ 1017 GeV • Diluted by inflation • “Intermediate Mass Monopoles” (IMM’s) • 108 GeV? (Frampton & Lee, 1990) • 105 GeV? (Frampton, 1999)

  3. Relativistic Magnetic Monopoles? • Wick et al. (’03): • Mass<1014 GeV  relativistic • Energy ~ 1016 GeV • Relativistic monopoles cause electro-magnetic cascades (showers) in ice.  Showers give off Cherenkov radiation.  Detection mechanism!

  4. Radio Ice Cherenkov Experiment • Martin A. Pomerantz Observatory (1km from S. Pole) • 16 buried radio receivers in 200m by 200m by 200m area • Detects Cherenkov radiation in 0.2GHz to 1GHz frequency range • 2001-2005: No high-energy neutrino detected in 58.3 Msec of livetime. Figure Credit: Kravchenko et al., 2003 Kravchenko et al., 2006

  5. A Muon Energy Loss Model Dutta, Reno, Sarcevic, & Seckel; hep-ph/0012350 βpair βbrem βphoto α = Ionization Energy Loss β = βbrem + βpair + βphoto βbrem = Fractional energy loss from bremsstrahlung βpair = Fractional energy loss from pair production βphoto = Fractional energy loss from photonuclear effect

  6. From Muon to Monopole Changes: • Muon mass → Monopole mass • Neglect Bremsstrahlung (dE/dx  1/M) • Multiply dE/dx by z2 = (68.5)2 • Hadronic interactions ignored

  7. Monte Carlo 1: Random Trajectory Generate random trajectory within 20km of RICE. Upgoing: • Propagate monopole through: • Distance: column thickness in g/cm2 from PREM • Medium: “standard rock” Dziewonski & Anderson, 1981

  8. Energy after Crossing Earth

  9. Monte Carlo 2: Passage through Ice Initially: 10m intervals θC-0.33 An antenna θC Data Stored 40cm intervals θC Another antenna θC+0.33 Max. error: 0.4ns Monopole Path

  10. Monte Carlo 3: Detector Response Treat each interval’s energy loss as separate shower. 40cm 40cm 40cm Monopole Path: Detector Response: Combined Detector Response:

  11. A Typical Voltage Profile E=10^16, γ=10^11, n=4011229

  12. Monte Carlo 4: Reconstruction • Send triggering monopoles through same reconstruction as RICE data. • Greatest obstacle: Time over threshold cut.

  13. Based on RadioMC, But No Ray Tracing Shift finished waveforms Ignore showers beyond visibility “horizon” (a function of antenna depth and shower depth) 20km maximum impact parameter unnecessary. Run code once to estimate actual distance distribution of triggering monopoles, then run it again with gamma-dependent maximum impact parameter. Monte Carlo Corrections

  14. Flux Upper Bounds

  15. Summary • “Light” monopoles become relativistic. • Monte Carlo shows RICE can detect these. • Flux upper bounds ~10-19 cm-2s-1sr-1

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