602 research outputs found
Rhomboid prism pair for rotating the plane of parallel light beams
An optical system is described for rotating the plane defined by a pair of parallel light beams. In one embodiment a single pair of rhomboid prisms have their respective input faces disposed to receive the respective input beams. Each prism is rotated about an axis of revolution coaxial with each of the respective input beams by means of a suitable motor and gear arrangement to cause the plane of the parallel output beams to be rotated relative to the plane of the input beams. In a second embodiment, two pairs of rhomboid prisms are provided. In a first angular orientation of the output beams, the prisms merely decrease the lateral displacement of the output beams in order to keep in the same plane as the input beams. In a second angular orientation of the prisms, the input faces of the second pair of prisms are brought into coincidence with the input beams for rotating the plane of the output beams by a substantial angle such as 90 deg
Slow relaxation to equipartition in spring-chain systems
In this study, one-dimensional systems of masses connected by springs, i.e.,
spring-chain systems, are investigated numerically. The average kinetic energy
of chain-end particles of these systems is larger than that of other particles,
which is similar to the behavior observed for systems made of masses connected
by rigid links. The energetic motion of the end particles is, however,
transient, and the system relaxes to thermal equilibrium after a while, where
the average kinetic energy of each particle is the same, that is, equipartition
of energy is achieved. This is in contrast to the case of systems made of
masses connected by rigid links, where the energetic motion of the end
particles is observed in equilibrium. The timescale of relaxation estimated by
simulation increases rapidly with increasing spring constant. The timescale is
also estimated using the Boltzmann-Jeans theory and is found to be in quite
good agreement with that obtained by the simulation
A stochastic simulation of the propagation of Galactic cosmic rays reflecting the discreteness of cosmic ray sources. Age and path length distribution
The path length distribution of Galactic cosmic rays (GCRs) is the
fundamental ingredient for modeling the propagation process of GCRs based on
the so-called weighted slab method. We try to derive this distribution
numerically by taking into account the discreteness in both space and time of
occurrences of supernova explosions where GCRs are suspected to be born. We
solve numerically the stochastic differential equations equivalent to the
Parker diffusion-convection equation which describes the propagation process of
GCR in the Galaxy. We assume the three-dimensional diffusion is an isotropic
one without any free escape boundaries. We ignore any energy change of GCRs and
the existence of the Galactic wind for simplicity. We also assume axisymmetric
configurations for the density distributions of the interstellar matter and for
the surface density of supernovae. We have calculated age and path length of
GCR protons arriving at the solar system with this stochastic method. The
obtained age is not the escape time of GCRs from the Galaxy as usually assumed,
but the time spent by GCRs during their journey to the solar system from the
supernova remnants where they were born. The derived age and path length show a
distribution spread in a wide range even for GCR protons arriving at the solar
system with the same energy. The distributions show a cut-off at a lower range
in age or path length depending on the energy of GCRs. These cut-offs clearly
come from the discreteness of occurrence of supernovae. The mean age of GeV
particles obtained from the distributions is consistent with the age obtained
by direct observation of radioactive secondary nuclei. The energy dependence of
the B/C ratio estimated with the path length distribution reproduces reliably
the energy dependence of B/C obtained by recent observations in space.Comment: 5 pages, 5 figures. Accepted for publication in A&
Constraints on Cold Dark Matter in the Gamma-ray Halo of NGC 253
A gamma-ray halo in a nearby starburst galaxy NGC 253 was found by the
CANGAROO-II Imaging Atmospheric Cherenkov Telescope (IACT). By fitting the
energy spectrum with expected curves from Cold Dark Matter (CDM) annihilations,
we constrain the CDM-annihilation rate in the halo of NGC 253. Upper limits for
the CDM density were obtained in the wide mass range between 0.5 and 50 TeV.
Although these limits are higher than the expected values, it is complementary
important to the other experimental techniques, especially considering the
energy coverage. We also investigate the next astronomical targets to improve
these limits.Comment: 13 pages, 5 figures, aastex.cls, natbib.sty, To appear in ApJ v596n1,
Oct. 10, 200
Simulating Cherenkov Telescope Array observation of RX J1713.7-3946
We perform simulations of Cherenkov Telescope Array (CTA) observations of a
young supernova remnant RX J1713.7-3946. This target is not only one of the
brightest sources ever discovered in very high-energy gamma rays but also well
observed in other wavebands. In X-rays, the emission is dominated by
synchrotron radiation, which links directly to the existence of high-energy
electrons. Radio observations of CO and HI gas have revealed a highly
inhomogeneous medium surrounding the SNR, such as clumpy molecular clouds.
Therefore gamma rays from hadronic interactions are naturally expected.
However, the spectrum in GeV energy range measured by Fermi/LAT indicates more
typical of leptonic emission from accelerated electrons. Despite lots of
multi-wavelength information, the competing interpretations have led to much
uncertainty in the quest of unraveling the true origin of the gamma-ray
emission from RX~J1713.7--3946. CTA will achieve highest performance ever in
sensitivity, angular resolution, and energy resolution. We estimate CTA
capability to examine the emission mechanisms of the gamma rays through
simulated spatial distribution, spectra, and their time variation.Comment: 8 pages, 3 figures. In Proceedings of the 34th International Cosmic
Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions
at arXiv:1508.0589
Size Segregation and Convection of Granular Mixtures Almost Completely Packed in the Rotating Thin Box
Size segregation of granular mixtures which are almost completely packed in a
rotating drum is discussed with an effective simulation and a brief analysis.
Instead of a 3D drum, we simulate 2D rotating thin box which is almost
completely packed with granular mixtures. The phase inversion of radially
segregated pattern which was found in a 3D experiment are qualitatively
reproduced with this simulation, and a brief analysis is followed. Moreover in
our simulation, a global convection appears after radial segregation pattern is
formed, and this convection induces axially segregated pattern.Comment: 9 pages, 5 figures, PACS number(s): 45.70.-n, 45.70.M
Evidence for TeV gamma-ray emission from the shell type SNR RXJ1713.7-3946
We report the results of TeV gamma-ray observations of the shell type SNR
RXJ1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission
from the northwest part of the remnant strongly suggests the existence of
electrons with energies up to 100 TeV in the remnant, making the SNR a good
candidate TeV gamma-ray source. We observed RXJ1713.7-3946 from May to August
1998 with the CANGAROO 3.8m atmospheric imaging Cerenkov telescope and obtained
evidence for TeV gamma-ray emission from the NW rim of the remnant with the
significance of 5.6 sigma. The observed TeV gamma-ray flux from the NW rim
region was estimated to be (5.3 +/- 0.9[statistical] +/- 1.6[systematic]) *
10^{-12} photons cm^{-2} s^{-1} at energies >= 1.8 +/- 0.9 TeV. The data
indicate that the emitting region is much broader than the point spread
function of our telescope. The extent of the emission is consistent with that
of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed
to the Inverse Compton scattering of the Cosmic Microwave Background Radiation
by shock accelerated ultra-relativistic electrons. Under this assumption, a
rather low magnetic field of 11 micro gauss is deduced for the remnant from our
observation.Comment: Accepted for publication by Astronomy and Astrophysics (5 pages, 2
figures
Galactic Gamma-Ray Halo of the Nearby Starburst Galaxy NGC 253
Recently, the CANGAROO-II telescope detected diffuse TeV gamma-ray emission
from a nearby edge-on starburst galaxy, NGC 253. The emission mechanism is
discussed in this report. We review the emissions of radio-to-TeV gamma-rays
from NGC 253, and present a model of the non-thermal emissions due to
synchrotron radiations and inverse Compton scatterings. A halo model
successfully explains the multiband spectrum of NGC 253.Comment: 11 pages, 1 figure. submitted to ApJ
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