High-energy neutrinos could be emitted from the center of the Sun as annihilation products of heavy galactic dark-matter particles. We analyze neutrino events observed by the Kamiokande detector to ...search for such neutrinos. The observed upper limits on solar high-energy neutrinos from these data set limits on the mass and density of certain galactic dark matter. The particles analyzed are heavy Dirac neutrinos ({nu}{sub {ital D}}), heavy Majorana neutrinos ({nu}{sub {ital M}}), Higgsinos ({ital {tilde h}}), neutrinos ({tilde {nu}}) with three flavors, and photinos ({tilde {gamma}}) as the lightest supersymmetric particles. Excluded mass regions are obtained for each dark-matter candidate: 3 GeV{lt}{ital m}{sub {nu}{ital D}}{lt}100 GeV, 3 GeV{lt}{ital m}{sub n{tilde u}}{ital e}{lt}90 GeV, 3 GeV{lt}{ital m}{sub n}{tilde u}{mu}{lt}90 GeV, and 4 GeV{lt}{ital m}{sub n}{tilde u}{tau}{lt}90 GeV. No limits are obtained on the masses of {nu}{sub {ital M}}, {ital {tilde h}}, and {tilde {gamma}} yet.
Phys.Rev.D75:043006,2007 Using the ``modified DPMJET-III'' model explained in the previous paper, we
calculate the atmospheric neutrino flux. The calculation scheme is almost the
same as HKKM04 ...\cite{HKKM2004}, but the usage of the ``virtual detector'' is
improved to reduce the error due to it. Then we study the uncertainty of the
calculated atmospheric neutrino flux summarizing the uncertainties of
individual components of the simulation. The uncertainty of $K$-production in
the interaction model is estimated by modifying FLUKA'97 and Fritiof 7.02 so
that they also reproduce the atmospheric muon flux data correctly, and the
calculation of the atmospheric neutrino flux with those modified interaction
models. The uncertainties of the flux ratio and zenith angle dependence of the
atmospheric neutrino flux are also studied.
Phys.Rev.D75:043005,2007 We have studied the hadronic interaction for the calculation of the
atmospheric neutrino flux by summarizing the accurately measured atmospheric
muon flux data and comparing ...with simulations. We find the atmospheric muon and
neutrino fluxes respond to errors in the $\pi$-production of the hadronic
interaction similarly, and compare the atmospheric muon flux calculated using
the HKKM04 code with experimental measurements. The $\mu^++\mu^-$ data show
good agreement in the 1$\sim$30 GeV/c range, but a large disagreement above 30
GeV/c. The the $\mu^+/\mu^-$ ratio shows sizable differences at lower and
higher momenta for opposite directions. As the disagreements are considered to
be due to assumptions in the hadronic interaction model, we try to improve it
phenomenologically based on the quark parton model. The improved interaction
model reproduces the observed muon flux data well. The calculation of the
atmospheric neutrino flux will be reported in the following paper
The atmospheric neutrino-flux is calculated over the wide energy range from 1 GeV to 3,000 GeV for the study of neutrino-physics using the data from underground neutrino-detectors. The uncertainty of ...atmospheric neutrino-fluxes is also discussed. A brief comment is made to interpret the anomaly in terms of neutrino oscillations.
We present the calculation of the atmospheric neutrino fluxes for the neutrino experiments proposed at INO, South Pole and Pyh\"asalmi. Neutrino fluxes have been obtained using ATMNC, a simulation ...code for cosmic ray in the atmosphere. Even using the same primary flux model and the interaction model, the calculated atmospheric neutrino fluxes are different for the different sites due to the geomagnetic field. The prediction of these fluxes in the present paper would be quite useful in the experimental analysis.
PDF
