622 research outputs found
Silver Photodiffusion into Ge-Rich Amorphous Germanium Sulfide—Neutron Reflectivity Study
Silver diffuses into chalcogenide films upon light exposure, and the kinetics of photodiffusion has been a subject of various investigations because of the difficulties in the in situ determination of the time-dependent Ag reaction and diffusion development in the chalcogenide layers. In this paper, we report the results of time-resolved neutron reflectivity measurement of Ag/Ge40S60/Si substrates under light exposure to clarify the kinetics of Ag photodiffusion into Ge-rich Ge chalcogenides. It reveals that Ag ions diffuse all over the Ge chalcogenide host layer once Ag dissolves into the layer without forming a metastable reaction layer unlike the case of S-rich Ge chalcogenide such as Ge20S80. The decay curve suggests that the Ag dissolution is determined by two types of Ag capturing chalcogen sites. Also, the observed relaxation time showed anomalous chalcogenide layer thickness dependence. This is attributed to an additional diffusion-driven accelerating factor, which is unique to the silver photodiffusion. Furthermore, we observed indicative changes in the formation of an inhomogeneous in-plane structure at the Ag/chalcogenide interface. This would be related to the nucleation and growth of the Ag-dissolved reaction product
Theoretical study of kinks on screw dislocation in silicon
Theoretical calculations of the structure, formation and migration of kinks
on a non-dissociated screw dislocation in silicon have been carried out using
density functional theory calculations as well as calculations based on
interatomic potential functions. The results show that the structure of a
single kink is characterized by a narrow core and highly stretched bonds
between some of the atoms. The formation energy of a single kink ranges from
0.9 to 1.36 eV, and is of the same order as that for kinks on partial
dislocations. However, the kinks migrate almost freely along the line of an
undissociated dislocation unlike what is found for partial dislocations. The
effect of stress has also been investigated in order to compare with previous
silicon deformation experiments which have been carried out at low temperature
and high stress. The energy barrier associated with the formation of a stable
kink pair becomes as low as 0.65 eV for an applied stress on the order of 1
GPa, indicating that displacements of screw dislocations likely occur via
thermally activated formation of kink pairs at room temperature
Operational Experience Of The Distributed Control System For synchrotron radiation Beam Lines At The Photon Factory
Measurements of Atmospheric Antiprotons
We measured atmospheric antiproton spectra in the energy range 0.2 to 3.4
GeV, at sea level and at balloon altitude in the atmospheric depth range 4.5 to
26 g/cm^2. The observed energy spectra, including our previous measurements at
mountain altitude, were compared with estimated spectra calculated on various
assumptions regarding the energy distribution of antiprotons that interacted
with air nuclei.Comment: Accepted for publication in PL
Observation of Galactic Sources of Very High Energy Gamma-Rays with the MAGIC Telescope
The MAGIC telescope with its 17m diameter mirror is today the largest
operating single-dish Imaging Air Cherenkov Telescope (IACT). It is located on
the Canary Island La Palma, at an altitude of 2200m above sea level, as part of
the Roque de los Muchachos European Northern Observatory. The MAGIC telescope
detects celestial very high energy gamma-radiation in the energy band between
about 50 GeV and 10 TeV. Since the autumn of 2004 MAGIC has been taking data
routinely, observing various objects, like supernova remnants (SNRs), gamma-ray
binaries, Pulsars, Active Galactic Nuclei (AGN) and Gamma-ray Bursts (GRB). We
briefly describe the observational strategy, the procedure implemented for the
data analysis, and discuss the results of observations of Galactic Sources.Comment: Brief Review, to be pulished in: Mod. Phys. Lett.
Asymmetric Patterns of Visual Field Defect in Primary Open-Angle and Primary Angle-Closure Glaucoma
Purpose: To compare the hemifield asymmetry of visual field (VF) loss in primary open-angle glaucoma (POAG) and primary angle-closure glaucoma (PACG) across all severity levels.
Methods: A total of 522 eyes of 327 patients with POAG (mean age ± SD, 54.1 ± 12.4 years) and 375 eyes of 204 patients with PACG (67.3 ± 8.9 years) were included. Subjects meeting the definitions of POAG or PACG were included. Means of the total deviation (TD) values (Humphrey 24-2 VF) in the Glaucoma Hemifield Test (GHT) regions were calculated in early (≥ −6 dB), moderate (< −6 dB and ≥ −12 dB), and advanced (< −12 dB) stages of POAG and PACG eyes. Then the differences of the TD values between superior and inferior hemifield GHT regions of POAG and PACG eyes were calculated. Also, the relationship between the values of pattern SD (PSD) and mean TD (mTD) was compared between POAG and PACG.
Results: In POAG eyes in the early stage, three regions (central, paracentral, and peripheral) in the superior hemifield had greater loss than their inferior counterparts; in moderate and advanced stages, all GHT regions in the superior hemifield had greater loss than their inferior counterparts. In PACG eyes, siginificantly fewer regions in the superior hemifield were significantly worse than their inferior counterpart, compared with POAG: one region (central) in early stage, two regions (central and peripheral) in moderate stage, and one region (central) in advanced stage. POAG eyes had greater PSD values than PACG eyes for given mean of TD values.
Conclusions: In both POAG and PACG eyes, VF damage was more pronounced in superior hemifield than inferior hemifield; however, this tendency was more obvious in POAG eyes than in PACG eyes
Measurements of 0.2 to 20 GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer
We measured low energy cosmic-ray proton and helium spectra in the kinetic
energy range 0.215 - 21.5 GeV/n at different solar activities during a period
from 1997 to 2002. The observations were carried out with the BESS spectrometer
launched on a balloon at Lynn Lake, Canada. A calculation for the correction of
secondary particle backgrounds from the overlying atmosphere was improved by
using the measured spectra at small atmospheric depths ranging from 5 through
37 g/cm^2. The uncertainties including statistical and systematic errors of the
obtained spectra at the top of atmosphere are 5-7 % for protons and 6-9 % for
helium nuclei in the energy range 0.5 - 5 GeV/n.Comment: 27 pages, 7 Tables, 9 figures, Submitted to Astroparticle Physic
Measurements of Proton, Helium and Muon Spectra at Small Atmospheric Depths with the BESS Spectrometer
The cosmic-ray proton, helium, and muon spectra at small atmospheric depths
of 4.5 -- 28 g/cm^2 were precisely measured during the slow descending period
of the BESS-2001 balloon flight. The variation of atmospheric secondary
particle fluxes as a function of atmospheric depth provides fundamental
information to study hadronic interactions of the primary cosmic rays with the
atmosphere.Comment: 21 pages, 11 figures, 4 table
Discovery of an Ultra-fast X-ray Pulsar in the Supernova Remnant N157B
We present the serendipitous discovery of 16 ms pulsed X-ray emission from
the Crab-like supernova remnant N157B in the Large Magellanic Cloud. This is
the fastest spinning pulsar associated with a supernova remnant (SNR).
Observations with the Rossi X-ray Timing Explorer (RXTE), centered on the field
containing SN1987A, reveal an X-ray pulsar with a narrow pulse profile.
Archival ASCA X-ray data confirm this detection and locate the pulsar within 1'
of the supernova remnant N157B, 14' from SN1987A. The pulsar manifests evidence
for glitch(es) between the RXTE and ASCA observations which span 3.5 years; the
mean linear spin-down rate is Pdot = 5.126 X 10E-14 s/s. The background
subtracted pulsed emission is similar to other Crab-like pulsars with a power
law of photon index of ~ 1.6. The characteristic spin-down age (~ 5000 years)
is consistent with the previous age estimate of the SNR. The inferred B-field
for a rotationally powered pulsar is ~ 1 X 10E12 Gauss. Our result confirms the
Crab-like nature of N157B; the pulsar is likely associated with a compact X-ray
source revealed by ROSAT HRI observations.Comment: 9 pages with 3 eps figure, LaTex (aas2pp2, psfig). Submitted to the
Astrophysical Journal Letter
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