The hadronic models for cosmic ray physics: the FLUKA code solutions

FLUKA is a general purpose Monte Carlo transport and interaction code used for fundamental physics and for a wide range of applications. These include Cosmic Ray Physics (muons, neutrinos, EAS, underground physics), both for basic research and applied studies in space and atmospheric flight dosimetry and radiation damage. A review of the hadronic models available in FLUKA and relevant for the description of cosmic ray air showers is presented in this paper. Recent updates concerning these models are discussed. The FLUKA capabilities in the simulation of the formation and propagation of EM and hadronic showers in the Earth's atmosphere are shown.Comment: 8 pages, 9 figures. Invited talk presented by M.V. Garzelli at ISVHECRI2006, International Symposium on Very High Energy Cosmic Rays, Weihai, China, August 15 - 22 200

FORCE ANALYSIS OF THE UNDERWATER STATIONARY RUNNIG

It aimed to analyze the vertical component of the ground reaction force in the underwater stationary running. The sample was composed by 6 subjects divided in two groups (Male Group and Female Group). The underwater stationary running was performed in two immersion levels: in the hip level and in the xiphoid process level. An underwater force plate was used. For data analysis descriptive statistics was used. The mean values of vertical GRF were 2,08BW for the MG and 1,69BW for the FG in the hip level; 1,15BW for the MG and 1,12BW for the FG in the xiphoid process level. The results showed the vertical component of the GRF is affected by the immersion level and by the frequency of the activity. Both factors should be considered by professionals who work with therapeutic or physical conditioning programs using the underwater stationary running

The physics models of FLUKA: status and recent development

A description of the intermediate and high energy hadronic interaction models used in the FLUKA code is given. Benchmarking against experimental data is also reported in order to validate the model performances. Finally the most recent developments and perspectives for nucleus-nucleus interactions are described together with some comparisons with experimental data.Comment: talk from the 2003 Computing in High Energy and Nuclear Physics (CHEP03), La Jolla, Ca, USA, March 2003, 10 pages, p

c-axis magnetotransport in CeCoIn5_{5}

We present the results of out-of-plane electrical transport measurements on the heavy fermion superconductor CeCoIn$_{5}$ at temperatures from 40 mK to 400 K and in magnetic field up to 9 T. For $T <$ 10 K transport measurements show that the zero-field resistivity $\rho_{c}$ changes linearly with temperature and extrapolates nearly to zero at 0 K, indicative of non-Fermi-liquid (nFL) behavior associated with a quantum critical point (QCP). The longitudinal magnetoresistance (LMR) of CeCoIn$_{5}$ for fields applied parallel to the c-axis is negative and scales as $B/(T+T^{*})$ between 50 and 100 K, revealing the presence of a single-impurity Kondo energy scale $T^{*} \sim 2$ K. Beginning at 16 K a small positive LMR feature is evident for fields less than 3 tesla that grows in magnitude with decreasing temperature. For higher fields the LMR is negative and increases in magnitude with decreasing temperature. This sizable negative magnetoresistance scales as $B{^2}/T$ from 2.6 K to roughly 8 K, and it arises from an extrapolated residual resistivity that becomes negative and grows quadratically with field in the nFL temperature regime. Applying a magnetic field along the c-axis with B $>$ B$_{c2}$ restores Fermi-liquid behavior in $\rho_{c}(T)$ at $T$ less than 130 mK. Analysis of the $T{^2}$ resistivity coefficient's field-dependence suggests that the QCP in CeCoIn$_{5}$ is located \emph{below} the upper critical field, inside the superconducting phase. These data indicate that while high-$T$ c-axis transport of CeCoIn$_{5}$ exhibits features typical for a heavy fermion system, low-$T$ transport is governed both by spin fluctuations associated with the QCP and Kondo interactions that are influenced by the underlying complex electronic structure intrinsic to the anisotropic CeCoIn$_{5}$ crystal structure

An updated Monte Carlo calculation of the CNGS neutrino beam

The new release of the CNGS neutrino beam simulation, which describes the beam-line features according to its final design, and its main results are presented and discussed. Storage of neutrino identity, energy and history in n-tuple format is also described, so that the experiments at the Gran Sasso can fully exploit all the informations from beam simulations

Calculation Of Secondary Particles In Atmosphere And Hadronic Interactions

Calculation of secondary particles produced by the interaction of cosmic rays with the nuclei of Earth's atmosphere pose important requirements to particle production models. Here we summarize the important features of hadronic simulations, stressing the importance of the so called ``microscopic'' approach, making explicit reference to the case of the FLUKA code. Some benchmarks are also presented.Comment: 10 pages, 4 figures. Extended version of report given at the IInd Workshop on Matter and anti-Matter, Trento, Oct. 200

Hard diffraction in hadron--hadron interactions and in photoproduction

Hard single diffractive processes are studied within the framework of the triple--Pomeron approximation. Using a Pomeron structure function motivated by Regge--theory we obtain parton distribution functions which do not obey momentum sum rule. Based on Regge-- factorization cross sections for hard diffraction are calculated. Furthermore, the model is applied to hard diffractive particle production in photoproduction and in $p\bar{p}$ interactions.Comment: 13 pages, Latex, 13 uuencoded figure

The Wisconsin Plasma Astrophysics Laboratory

The Wisconsin Plasma Astrophysics Laboratory (WiPAL) is a flexible user facility designed to study a range of astrophysically relevant plasma processes as well as novel geometries that mimic astrophysical systems. A multi-cusp magnetic bucket constructed from strong samarium cobalt permanent magnets now confines a 10 m$^3$, fully ionized, magnetic-field free plasma in a spherical geometry. Plasma parameters of $T_{e}\approx5$ to $20$ eV and $n_{e}\approx10^{11}$ to $5\times10^{12}$ cm$^{-3}$ provide an ideal testbed for a range of astrophysical experiments including self-exciting dynamos, collisionless magnetic reconnection, jet stability, stellar winds, and more. This article describes the capabilities of WiPAL along with several experiments, in both operating and planning stages, that illustrate the range of possibilities for future users.Comment: 21 pages, 12 figures, 2 table