676 research outputs found
Monte Carlo Study of Ordering and Domain Growth in a Class of fcc-Alloy Models
Ordering processes in fcc-alloys with composition A_3B (like Cu_3Au, Cu_3Pd,
CoPt_3 etc.) are investigated by Monte Carlo simulation within a class of
lattice models based on nearest-neighbor (NN) and second-neighbor (NNN)
interactions. Using an atom-vacancy exchange algorithm, we study the growth of
ordered domains following a temperature quench below the ordering spinodal. For
zero NNN-interactions we observe an anomalously slow growth of the domain size
L(t) \sim t^\alpha, where \alpha \sim 1/4 within our accessible timescales.
With increasing NNN-interactions domain growth becomes faster and \alpha
gradually approaches the value 1/2 as predicted by the conventional
Lifshitz-Allen-Cahn theory.Comment: 6 pages, 4 figure
Disappearance of Hard X-ray Emission in the Last BeppoSAX Observation of the Z Source GX 349+2
We report on the results from two BeppoSAX observations of the Z source GX
349+2 performed in February 2001 and covering the broad energy range 0.12-200
keV. The light curve obtained from these observations shows a large flaring
activity, the count rate varying from ~130 to ~260 counts/s, indicating that
the source was in the flaring branch during these observations. The average
spectrum is well described by a soft blackbody and a Comptonized component. To
well fit the energy spectrum three gaussian lines are needed at 1.2 keV, 2.6
keV, and 6.7 keV with corresponding equivalent widths of 13 eV, 10 eV, and 39
eV, probably associated to L-shell emission of Fe XXIV, Ly-alpha S XVI, and Fe
XXV, respectively. These lines may be produced at different distances from the
neutron star, which increase when the count rate of the source increases. An
absorption edge is also needed at 9 keV with an optical depth of ~3 10^{-2}.
From the Color-Color Diagram (CD) we selected five zones from which we
extracted the corresponding energy spectra. The temperatures of the blackbody
and of the Comptonized component tend to increase when the intensity of the
source increases. We discuss our results comparing them to those obtained from
a previous BeppoSAX observation, performed in March 2000, during which the
source was a similar position of its Z-track. In particular we find that,
although the source showed similar spectral states in the 2000 and the 2001
observations, a hard tail, that was significantly detected in March 2000, is
not observed in these recent observations.Comment: Accepted for publication on Ap
About the measurements of the hard X-ray background
We analyze uncertainties in the cosmic X-ray background measurements
performed by the INTEGRAL observatory. We find that the most important effect
limiting the accuracy of the measurements is related to the intrinsic
background variation in detectors. Taking into account all of the uncertainties
arising during the measurements we conclude that the X-ray background intensity
obtained in the INTEGRAL observations is compatible with the historic X-ray
background observations performed by the HEAO-1 satellite.Comment: 20 pages, 4 figures, accepted for publication in Astrophysics and
Space Scienc
Testing Comptonization as the origin of the continuum in nonmagnetic Cataclysmic Variables. The photon index of X-ray emission
X-ray spectra of nonmagnetic cataclysmic variables (nmCVs) in the ~ 0.315
keV energy band have been described either by one or several optically thin
thermal plasma components, or by cooling flow models. We tested if the spectral
continuum in nmCVs could be successfully described by Comptonization of soft
photons off hot electrons presented in a cloud surrounding the source [the
transition layer, (TL)]. We used publicly XMM-Newton Epic-pn, Chandra HETG/ACIS
and LETG/HRC, and RXTE PCA and HEXTE observations of four Dwarf Novae (U~Gem,
SS~Cyg, VW~Hyi and SS~Aur) observed in the quiescence and outburst states. In
total, we analyzed 18 observations, including a simultaneous 0.4150 keV
Chandra/RXTE spectrum of SS~Cyg in quiescence. We fitted the spectral continuum
with up to two thermal Comptonization components (compTT or compTB models in
XSPEC), using only one thermal plasma temperature and one optical depth. In
this framework the two seed photon components are coming presumably from the
innermost and outer parts of the TL (or innermost part of the disk). We
obtained that the thermal Comptonization can successfully describe the spectral
continuum of these nmCV in the ~ 0.4150 keV energy band. Moreover, we
present the first principal radiative transfer model which explains the
quasi-constancy of the spectral photon index observed around 1.8, which
strongly supports the Comptonization framework in nmCVs.Comment: 34 pages, 8 figure
Monte Carlo simulation of subsurface ordering kinetics in an fcc-alloy model
Within the atom-vacancy exchange mechanism in a nearest-neighbor interaction
model we investigate the kinetics of surface-induced ordering processes close
to the (001) surface of an fcc A_3B-alloy. After a sudden quench into the
ordered phase with a final temperature above the ordering spinodal, T_f > T_sp,
the early time kinetics is dominated by a segregation front which propagates
into the bulk with nearly constant velocity. Below the spinodal, T_f < T_sp,
motion of the segregation wave reflects a coarsening process which appears to
be slower than predicted by the Lifschitz-Allen-Cahn law. In addition, in the
front-penetrated region lateral growth differs distinctly from perpendicular
growth, as a result of the special structure of antiphase boundaries near the
surface. Our results are compared with recent experiments on the subsurface
ordering kinetics at Cu_3Au (001).Comment: 10 pages, 9 figures, submitted to Phys. Rev. B, in prin
A Hard X-ray View on Scorpius X-1 with INTEGRAL: non-Thermal Emission ?
We present here simultaneous INTEGRAL/RXTE observations of Sco X-1, and in
particular a study of the hard X-ray emission of the source and its correlation
with the position in the Z-track of the X-ray color-color diagram. We find that
the hard X-ray (above about 30 keV) emission of Sco X-1 is dominated by a
power-law component with a photon index of ~3. The flux in the power-law
component slightly decreases when the source moves in the color-color diagram
in the sense of increasing inferred mass accretion rate from the horizontal
branch to the normal branch/flaring branch vertex. It becomes not significantly
detectable in the flaring branch, where its flux has decreased by about an
order of magnitude. These results present close analogies to the behavior of GX
17+2, one of so-called Sco-like Z sources. Finally, the hard power law in the
spectrum of Sco X-1 does not show any evidence of a high energy cutoff up to
100 - 200 keV, strongly suggesting a non-thermal origin of this component.Comment: 5 pages including 3 figures. Accepted for publication by ApJ Letter
The BeppoSAX view of the X-ray active nucleus of NGC4258
BeppoSAX observed NGC4258 on December 1998, when its 2-10 keV luminosity was
\~1E41 erg/s. 100% variability is observed in the 3-10 keV band on timescales
of a half a day while 20% variability is observed on timescales of one hour.
The nuclear component is visible above 2 keV only, being obscured by a column
density of (9.5+/-1.2)E22 cm-2; this component is detected up to 70 keV with
S/N>=3 and with the steep power law energy index of 1.11+/-0.14. Bremsstrahlung
emission for the 2-70 keV X-ray luminosity, as expected in ADAF models with
strong winds, is ruled out by the data. The ratio between the nuclear radio and
the X-ray luminosities is <=1E-5, similar to that of radio quiet AGN. X-ray
variability and spectral shape, radio to X-ray and NIR to X-ray luminosity
ratios suggest that the nucleus of NGC4258 could be a scaled-down version of a
Seyfert nucleus. The soft (E<=2keV) X-ray emission is complex. There are at
least two thermal-like components, with T1=0.6+/-0.1 keV and T2>=1.3 keV. The
cooler (L(0.1-2.4keV)=1E40 erg/s) component is probably associated with the
jet, resolved in X-rays by the ROSAT HRI. The second component, which can be
modeled equally well by an unobscured power law model, has L(0.1-2.4keV)~7E39
erg/s, consistent with that expected from discrete X-ray sources in the host
galaxy. NGC4258 and other maser AGNs show strong nuclear X-ray absorption. We
propose that this large column of gas might be responsible for shielding the
regions of maser emission from X-ray illumination. So a large column density
gas may be a necessary property of masing AGNs.Comment: ApJ in pres
Selective Spin-State Switch and Metal-Insulator Transition in \boldmath
Ultra-high resolution synchrotron diffraction data for
throw new light on the metal-insulator transition of Co Ba-cobaltites.
An anomalous expansion of CoO octahedra is observed at the phase transition
on heating, while CoO pyramids show the normal shrinking at the closing of
the gap. The insulator-to-metal transition is attributed to a sudden excitation
of some electrons in the octahedra ( state) into the Co band
(final state). The state in the pyramids does
not change and the structural study also rules out a
orbital ordering at .Comment: Phys. Rev. B (to appear
The Interplanetary Network Supplement to the BeppoSAX Gamma-Ray Burst Catalogs
Between 1996 July and 2002 April, one or more spacecraft of the
interplanetary network detected 787 cosmic gamma-ray bursts that were also
detected by the Gamma-Ray Burst Monitor and/or Wide-Field X-Ray Camera
experiments aboard the BeppoSAX spacecraft. During this period, the network
consisted of up to six spacecraft, and using triangulation, the localizations
of 475 bursts were obtained. We present the localization data for these events.Comment: 89 pages, 3 figures. Submitted to the Astrophysical Journal
Supplement Serie
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