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Search Results: 1 - 10 of 593417 matches for " J. M. LoSecco "
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Problems with Atmospheric Neutrino Oscillations
J. M. LoSecco
Physics , 1998,
Abstract: The neutrino oscillation hypothesis does a poor job of representing the atmospheric neutrino anomaly. The anomaly is observed over 4 decades in path length and at least a factor of 30 in energy. This restricts the potential oscillation solutions to those with large amplitudes and mixing mass differences that are ruled out by other observations. The $\Delta m^{2}$ region in the range $10^{-4} - 10^{-2}$ leads to inconsistencies within the atmospheric neutrino data itself. The observed value of $R$ seems to be incompatible with the $\Delta m^{2}$ implied by recent results
$Δm^{2}$ Limits from $R(E_ν)$
J. M. LoSecco
Physics , 1998,
Abstract: A lower bound on $\Delta m^{2}$ for atmospheric neutrino oscillations can be obtained from the global value of $R$ at a given energy. This bound may be more reliable than one based on the observed isotropy. Some global values of $R$ imply an anisotropy in the neutrino flux that may, or may not be manifest in the observed neutrino interactions. A limit of $\Delta m^{2}>0.0077$ eV$^{2}$ is easily obtained. Much higher mass scales are implied by the reported energy independence and magnitude of $R$
Studying the Quark Antiquark Force with Inelastic Pion Electron Scattering
J. M. LoSecco
Physics , 1994, DOI: 10.1103/PhysRevD.51.6572
Abstract: The concept of studying the internal structure of mesons is explored. Mesons, which are in principle two body quark antiquark interactions, may be much easier to understand than the nucleon. Measurements of the inelastic form factors to specific final states may permit careful direct studies of various components of the strong force. For example by looking at vector meson final states the spin flip amplitude can be isolated. Technical difficulties involved in a realistic experiment are examined. Experiments to some final states such as $\rho$, $K^*$ and $a_{0}$ are practical today.
(Mis)Understanding the Atmospheric Neutrino Anomaly
J. M. LoSecco
Physics , 2000, DOI: 10.1016/S0920-5632(01)01221-X
Abstract: The apparent attenuation of muon neutrinos relative to electron neutrinos is a bit too low to be compatible with the most popular values of $\Delta m^{2}$. Fits to $R(E_{\nu})$ favor values of $\Delta m^{2}>0.1$ eV$^{2}$. The fit minimized by the Super Kamioka group in estimating neutrino oscillation parameters neglects systematic errors. The fit is dominated by systematic effects. The data being combined in recent fits may not be compatible since there appear to be significant variations in the properties of the data with time. A simple two component neutrino oscillation with $\Delta m^{2}$ in the range of 10$^{-3}$ to 10$^{-2}$ eV$^{2}$ seems unable to account for the observations.
Bounds on $ν_μ$ Oscillations from Atmospheric Neutrinos
J. M. LoSecco
Physics , 1998,
Abstract: A reanalysis of identified muon neutrino interactions from IMB 3 yields bounds on $\sin^{2}(2 \theta)$ and $\Delta m^{2}$. The limit $\sin^{2}(2 \theta) < 0.72$ is in conflict with the recent announcement of a neutrino mass.
Bounds on Dark Matter from the ``Atmospheric Neutrino Anomaly''
J. M. LoSecco
Physics , 1997, DOI: 10.1103/PhysRevD.56.4416
Abstract: Bounds are derived on the cross section, flux and energy density of new particles that may be responsible for the atmospheric neutrino anomaly. $4.6 \times 10^{-45} cm^2 < \sigma <2.4 \times 10^{-34} cm^2$ Decay of primordial homogeneous dark matter can be excluded.
Measuring the $ν_μ$ to $\bar{ν_μ}$ Ratio in a High Statistics Atmospheric Neutrino Experiment
J. M. LoSecco
Physics , 1998, DOI: 10.1103/PhysRevD.59.117302
Abstract: By exploiting differences in muon lifetimes it is possible to distinguish $\nu_{\mu}$ from $\bar{\nu_{\mu}}$ charged current interactions in underground neutrino detectors. Such observations would be a useful tool in understanding the source of the atmospheric neutrino anomaly.
What the Atmospheric Neutrino Anomaly is Not
J. M. LoSecco
Physics , 1998,
Abstract: The atmospheric neutrino anomaly is the apparent reduction of the $\nu_{\mu}/\nu_{e}$ ratio observed in underground detectors. It represents either a reduction in the muon neutrino interaction rate or an excess of the electron neutrino interaction rate, or both. Unable to answer the question of ``What else could it be?'' this paper explores a number of alternatives which do not seem to be viable. Various methods to reduce the apparent muon rate or to increase the apparent electron rate are discussed. Perhaps our bias that the interactions are due to neutrinos of atmospheric origin is incorrect. Both of these assumptions need to be confirmed. Efforts to reduce uncertainties in the estimated atmospheric neutrino flux would also help to narrow the possibilities further.
Bounds on Extra Dimensions from Binary Pulsars
J. M. LoSecco
Physics , 2000,
Abstract: Evidence for gravitational radiation from binary pulsars places constraints on properties of ``large'' extra dimensions. The size of these extra dimensions must exceed about 37 AU for gravitational radiation to be emitted.
Possible Sources of a Transient Natural Neutrino Flux
J. M. LoSecco
Physics , 1999,
Abstract: Recent observations of variability in the ``atmospheric neutrino'' rate place constraints on possible explanations of the atmospheric neutrino anomaly. Many proposed solutions to the problem are static and can not be adapted to the temporal dependence observed. Nonatmospheric sources may be needed to explain the variations.
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