234 research outputs found
Computationally efficient methods for modelling laser wakefield acceleration in the blowout regime
Electron self-injection and acceleration until dephasing in the blowout
regime is studied for a set of initial conditions typical of recent experiments
with 100 terawatt-class lasers. Two different approaches to computationally
efficient, fully explicit, three-dimensional particle-in-cell modelling are
examined. First, the Cartesian code VORPAL using a perfect-dispersion
electromagnetic solver precisely describes the laser pulse and bubble dynamics,
taking advantage of coarser resolution in the propagation direction, with a
proportionally larger time step. Using third-order splines for macroparticles
helps suppress the sampling noise while keeping the usage of computational
resources modest. The second way to reduce the simulation load is using
reduced-geometry codes. In our case, the quasi-cylindrical code CALDER-CIRC
uses decomposition of fields and currents into a set of poloidal modes, while
the macroparticles move in the Cartesian 3D space. Cylindrical symmetry of the
interaction allows using just two modes, reducing the computational load to
roughly that of a planar Cartesian simulation while preserving the 3D nature of
the interaction. This significant economy of resources allows using fine
resolution in the direction of propagation and a small time step, making
numerical dispersion vanishingly small, together with a large number of
particles per cell, enabling good particle statistics. Quantitative agreement
of the two simulations indicates that they are free of numerical artefacts.
Both approaches thus retrieve physically correct evolution of the plasma
bubble, recovering the intrinsic connection of electron self-injection to the
nonlinear optical evolution of the driver
The experimental cascade curves of EAS at E sub 0 10(17) eV obtained by the method of detection of Cherenkov pulse shape
The individual cascade curves of EAS with E sub 0 10 to the 17th power eV/I to 3/ were studied by detection of EAS Cherenkov light pulses. The scintillators located at the center of the Yakutsk EAS array within a 500-m radius circle were used to select the showers and to determine the main EAS parameters. The individual cascade curves N(t) were obtained using the EAS Cherenkov light pulses satisfying the following requirements: (1) the signal-to-noise ratio fm/delta sub n 15, (2) the EAS axis-detector distance tau sub 350 m, (3) the zenith angle theta 30 deg, (4) the probability for EAS to be detected by scintillators W 0.8. Condition (1) arises from the desire to reduce the amplitude distortion of Cherenkov pulses due to noise and determines the range of EAS sizes, N(t). The resolution times of the Cherenkov pulse shape detectors are tau sub 0 approx. 23 ns which results in distortion of a pulse during the process of the detection. The distortion of pulses due to the finiteness of tau sub 0 value was estimated. It is shown that the rise time of pulse becomes greater as tau sub 0.5/tau sub 0 ratio decreases
Possibility of Using a Satellite-Based Detector for Recording Cherenkov Light from Ultrahigh-Energy Extensive Air Showers Penetrating into the Ocean Water
We have estimated the reflected component of Cherenkov radiation, which
arises in developing of an extensive air shower with primary energy of 10^20 eV
over the ocean surface. It has been shown that, under conditions of the TUS
experiment, a flash of the reflected Cherenkov photons at the end of the
fluorescence track can be identified in showers with zenith angles up to 20
degrees.Comment: 5 pages, 3 figures. This preprint corrects errors which appeared in
the English version of the article published in Bull. Rus. Acad. Sci. Phys.,
2011, Vol. 75, No. 3, p. 381. The original russian text was published in Izv.
RAN. Ser. Fiz., 2011, Vol. 75, No. 3, p. 41
The Affine-Metric Quantum Gravity with Extra Local Symmetries
We discuss the role of additional local symmetries related to the
transformations of connection fields in the affine-metric theory of gravity.
The corresponding BRST transformations connected with all symmetries (general
coordinate, local Lorentz and extra) are constructed. It is shown, that extra
symmetries give the additional contribution to effective action which is
proportional to the corresponding Nielsen-Kallosh ghost one. Some arguments are
given, that there is no anomaly associated with extra local symmetries.Comment: 14 pages in LATEX (The version of paper accepted for publication in
Class. Quant. Grav.
Spin-transfer torque effects in the dynamic forced response of the magnetization of nanoscale ferromagnets in superimposed ac and dc bias fields in the presence of thermal agitation
Spin-transfer torque (STT) effects on the stationary forced response of
nanoscale ferromagnets subject to thermal fluctuations and driven by an ac
magnetic field of arbitrary strength and direction are investigated via a
generic nanopillar model of a spin-torque device comprising two ferromagnetic
strata representing the free and fixed layers and a nonmagnetic conducting
spacer all sandwiched between two ohmic contacts. The STT effects are treated
via the Brown magnetic Langevin equation generalized to include the Slonczewski
STT term thereby extending the statistical moment method [Y. P. Kalmykov et
al., Phys. Rev. B 88, 144406 (2013)] to the forced response of the most general
version of the nanopillar model. The dynamic susceptibility, nonlinear
frequency-dependent dc magnetization, dynamic magnetic hysteresis loops, etc.
are then evaluated highlighting STT effects on both the low-frequency thermal
relaxation processes and the high-frequency ferromagnetic resonance, etc.,
demonstrating a pronounced dependence of these on the spin polarization current
and facilitating interpretation of STT experiments
Cosmic Ray Air Shower Characteristics in the Framework of the Parton-Based Gribov-Regge Model NEXUS
The purpose of this paper is twofold: first we want to introduce a new type
of hadronic interaction model (NEXUS), which has a much more solid theoretical
basis as, for example, presently used models like QGSJET and VENUS, and ensures
therefore a much more reliable extrapolation towards high energies. Secondly,
we want to promote an extensive air shower (EAS) calculation scheme, based on
cascade equations rather than explicit Monte Carlo simulations, which is very
accurate in calculations of main EAS characteristics and extremely fast
concerning computing time. We employ the NEXUS model to provide the necessary
data on particle production in hadron-air collisions and present the average
EAS characteristics for energies 10^14 - 10^17 eV. The experimental data of the
casa-blanka group are analyzed in the framework of the new model.Comment: 15 pages, 8 figure
Influence of hadronic interaction models and the cosmic ray spectrum on the high energy atmospheric muon and neutrino flux
The recent observations of muon charge ratio up to about 10 TeV and of
atmospheric neutrinos up to energies of about 400 TeV has triggered a renewed
interest into the high-energy interaction models and cosmic ray primary
composition. A reviewed calculation of lepton spectra produced in cosmic-ray
induced extensive air showers is carried out with a primary cosmic-ray spectrum
that fits the latest direct measurements below the knee. In order to achieve
this, we used a full Monte Carlo method to derive the inclusive differential
spectra (yields) of muons, muon neutrinos and electron neutrinos at the surface
for energies between 80 GeV and hundreds of PeV. The air shower simulator {\sc
corsika} 6.990 was used for showering and propagation of the secondary
particles through the atmosphere, employing the established high-energy
hadronic interaction models {\sc sibyll} 2.1, {\sc qgsjet-01} and {\sc
qgsjet-ii 03}. We show that the performance of the interaction models allows
makes it possible to predict the spectra within experimental uncertainties,
while {\sc sibyll} generally yields a higher flux at the surface than the
qgsjet models. The calculation of the flavor and charge ratios has lead to
inconsistent results, mainly influenced by the different representations of the
K/ ratio within the models. Furthermore, we could quantify systematic
uncertainties of atmospheric muon- and neutrino fluxes, associated to the
models of the primary cosmic-ray spectrum and the interaction models. For most
recent parametrizations of the cosmic-ray primary spectrum, atmospheric muons
can be determined with an uncertainty smaller than % of the
average flux. Uncertainties of the muon- and electron neutrino fluxes can be
calculated within an average error of % and %,
respectively.Comment: 16 pages, 10 figures, version 2 includes analytic approximatio
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