D. Seckel

Neutrinos from propagation of ultrahigh-energy protons

We present a calculation of the production of neutrinos during propagation of ultra-high energy cosmic rays from their astrophysical sources to us. Photoproduction interactions are modeled with the event generator SOPHIA that represents very well the experimentally measured particle production cross sections at accelerator energies. We give the fluxes expected from different assumptions on cosmic ray source distributions, cosmic ray injection spectra, cosmological evolution of the sources and different cosmologies, and compare them to the Waxman-Bahcall limit on source neutrinos. We estimate rates for detection of neutrino induced showers in a km3 water detector. The ratio of the local high energy neutrino flux to the ultra-high energy cosmic ray flux is a crucial parameter in distinguishing between astrophysical and cosmological (top-down) scenarios of the ultra-high energy cosmic ray origin.

RICE limits on the diffuse ultrahigh energy neutrino flux

We present new limits on ultrahigh energy neutrino fluxes above

The anthropic principle and the mass scale of the Standard Model

{10}^{17}\text{ }\text{ }\mathrm{eV}

Constraints on Cosmic Neutrino Fluxes from the Antarctic Impulsive Transient Antenna Experiment

based on data collected by the Radio Ice Cherenkov Experiment (RICE) at the South Pole from 1999\char21{}2005. We discuss estimation of backgrounds, calibration and data analysis algorithms (both online and offline), procedures used for the dedicated neutrino search, and refinements in our Monte Carlo (MC) simulation, including recent in situ measurements of the complex ice dielectric constant. An enlarged data set and a more detailed study of hadronic showers results in a sensitivity improvement of more than 1 order of magnitude compared to our previously published results. Examination of the full RICE data set yields zero acceptable neutrino candidates, resulting in 95% confidence-level model-dependent limits on the flux

Observations of the Askaryan Effect in Ice

{E}_{\ensuremath{\nu}}^{2}d\ensuremath{\phi}/d{E}_{\ensuremath{\nu}}l{10}^{\ensuremath{-}6}\text{ }\text{ }\mathrm{GeV}/(\mathrm{c}{\mathrm{m}}^{2}\text{ }\mathrm{s}\text{ }\mathrm{sr})

The Antarctic Impulsive Transient Antenna ultra-high energy neutrino detector: Design, performance, and sensitivity for the 2006–2007 balloon flight

in the energy range

New Limits on the Ultrahigh Energy Cosmic Neutrino Flux from the ANITA Experiment

{10}^{17}l{E}_{\ensuremath{\nu}}l{10}^{20}\text{ }\text{ }\mathrm{eV}

Observation of ultrahigh-energy cosmic rays with the ANITA balloon-borne radio interferometer

. The new RICE results rule out the most intense flux model projections at 95% confidence level.

Limits on the Ultra-High Energy Electron Neutrino Flux from the RICE Experiment

In theories in which different regions of the universe can have different values of the the physical parameters, we would naturally find ourselves in a region which has parameters favorable for life. We explore the range of anthropically allowed values of the mass parameter in the Higgs potential, µ 2 . For µ 2 0, baryon stability requires that |µ| << MP, the Planck Mass. Smaller values of � µ 2 � may or may not be allowed depending on issues of element synthesis and stellar evolution. We conclude that the observed value of µ 2 is reasonably typical of the anthropically allowed range, and that anthropic arguments provide a plausible explanation for the closeness of the QCD scale and the weak scale.

NUCLEON SPIN FLUCTUATIONS AND THE SUPERNOVA EMISSION OF NEUTRINOS AND AXIONS

P. F. Dowkontt, 4 M. A. DuVernois,5 P. A. Evenson, 6 D. Goldstein, 1 P. W. Gorham, 9 C. L. Hebert, 9 M. H. Israel,4 J. G. Learned, 9 K. M. Liewer,10 J. T. Link,9 S. Matsuno, 9 P. Miočinović,9 J. Nam, 1 C. J. Naudet, 10 R. Nichol,2 K. Palladino, 2 M. Rosen, 9 D. Saltzberg, 7 D. Seckel, 6 A. Silvestri,1 B. T. Stokes, 9 G. S. Varner, 9 and F. Wu1 1Department of Physics and Astronomy, University of California at Irvine, Irvine, California 2Department of Physics, Ohio State University, Columbus, Ohio 3Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 4Department of Physics, Washington University in St. Louis, St. Louis, Missouri 5School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 6Bartol Research Institute, University of Delaware, Newark, Delaware 7Department of Physics and Astronomy, University of California at Los Angeles, Los Angeles, California 8Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, Pennsylvania 9Department of Physics and Astronomy, University of Hawaii at Manoa, Honolulu, Hawaii 10Jet Propulsion Laboratory, Pasadena, California