20,012 research outputs found
Covariance Properties of Reflection Equation Algebras
The reflection equations (RE) are a consistent extension of the Yang-Baxter
equations (YBE) with an addition of one element, the so-called reflection
matrix or -matrix. For example, they describe the conditions for
factorizable scattering on a half line just like the YBE give the conditions
for factorizable scattering on an entire line. The YBE were generalized to
define quadratic algebras, \lq Yang-Baxter algebras\rq\ (YBA), which were used
intensively for the discussion of quantum groups. Similarly, the RE define
quadratic algebras, \lq the reflection equation algebras\rq\ (REA), which enjoy
various remarkable properties both new and inherited from the YBA. Here we
focus on the various properties of the REA, in particular, the quantum group
comodule properties, generation of a series of new solutions by composing known
solutions, the extended REA and the central elements, etc.Comment: 31 pages, 8 figures (not included
Comment on "Memory Effects in an Interacting Magnetic Nanoparticle System"
In Phys. Rev. Lett. 91 167206 (2003), Sun et al. study memory effects in an
interacting nanoparticle system with specific temperature and field protocols.
The authors claim that the observed memory effects originate from spin-glass
dynamics and that the results are consistent with the hierarchical picture of
the spin-glass phase. In this comment, we argue their claims premature by
demonstrating that all their experimental curves can be reproduced
qualitatively using only a simplified model of isolated nanoparticles with a
temperature dependent distribution of relaxation times.Comment: 1 page, 2 figures, slightly changed content, the parameters involved
in Figs. 1 and 2 are changed a little for a semi-quantitative comparision
with experimental result
Realization of a collective decoding of codeword states
This was also extended from the previous article quant-ph/9705043, especially
in a realization of the decoding process.Comment: 6 pages, RevTeX, 4 figures(EPS
XMM-Newton observation of the interacting galaxies NGC1512 and NGC1510
The galaxy NGC1512 is interacting with the smaller galaxy NGC1510 and shows a
peculiar morphology, characterised by two extended arms immersed in an HI disc
whose size is about four times larger than the optical diameter of NGC1512. For
the first time we performed a deep X-ray observation of the galaxies NGC1512
and NGC1510 with XMM-Newton to gain information on the population of X-ray
sources and diffuse emission in a system of interacting galaxies. We identified
and classified the sources detected in the XMM-Newton field of view by means of
spectral analysis, hardness-ratios calculated with a Bayesian method, X-ray
variability, and cross-correlations with catalogues in optical, infrared, and
radio wavelengths. We also made use of archival Swift (X-ray) and Australia
Telescope Compact Array (radio) data to better constrain the nature of the
sources detected with XMM-Newton. We detected 106 sources in the energy range
of 0.2-12 keV, out of which 15 are located within the D_25 regions of NGC1512
and NGC1510 and at least six sources coincide with the extended arms. We
identified and classified six background objects and six foreground stars. We
discussed the nature of a source within the D_25 ellipse of NGC1512, whose
properties indicate a quasi-stellar object or an intermediate ultra-luminous
X-ray source. Taking into account the contribution of low-mass X-ray binaries
and active galactic nuclei, the number of high-mass X-ray binaries detected
within the D_25 region of NGC1512 is consistent with the star formation rate
obtained in previous works based on radio, infrared optical, and UV
wavelengths. We detected diffuse X-ray emission from the interior region of
NGC1512 with a plasma temperature of kT=0.68(0.31-0.87) keV and a 0.3-10 keV
X-ray luminosity of 1.3E38 erg/s, after correcting for unresolved discrete
sources.Comment: Accepted for publication in Astronomy and Astrophysics. 20 pages.
Appendix B will be published electronically onl
Temperature Chaos and Bond Chaos in the Edwards-Anderson Ising Spin Glass : Domain-Wall Free-Energy Measurements
Domain-wall free-energy , entropy , and the correlation
function, , of are measured independently in the
four-dimensional Edwards-Anderson (EA) Ising spin glass. The stiffness
exponent , the fractal dimension of domain walls and the
chaos exponent are extracted from the finite-size scaling analysis of
, and respectively well inside the
spin-glass phase. The three exponents are confirmed to satisfy the scaling
relation derived by the droplet theory within our
numerical accuracy. We also study bond chaos induced by random variation of
bonds, and find that the bond and temperature perturbations yield the universal
chaos effects described by a common scaling function and the chaos exponent.
These results strongly support the appropriateness of the droplet theory for
the description of chaos effect in the EA Ising spin glasses.Comment: 4 pages, 6 figures; The title, the abstract and the text are changed
slightl
Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0)
Context: We study the X-ray emission of the Galactic supernova remnant (SNR)
CTB 109 (G109.1-1.0), which is well-known for its enigmatic half-shell
morphology both in radio and in X-rays and is associated with the anomalous
X-ray pulsar (AXP) 1E2259+586. Aims: We want to understand the origin of the
X-ray bright feature inside the SNR called the Lobe and the details of the
interaction of the SNR shock wave with the ambient interstellar medium (ISM).
Methods: The Lobe and the northeastern part of the SNR were observed with
Chandra ACIS-I. We analysed the spectrum of the X-ray emission by dividing the
entire observed emission into small regions. The X-ray emission is best
reproduced with one-component or two-component non-equilibrium ionisation
models depending on the position. In the two-component model one emission
component represents the shocked ISM and the other the shocked ejecta. Results:
We detect enhanced element abundances, in particular for Si and Fe, in and
around the Lobe. There is one particular region next to the Lobe with a high Si
abundance of 3.3 (2.6 - 4.0) times the solar value. This is the first,
unequivocal detection of ejecta in CTB 109. Conclusions: The new Chandra data
confirm that the Lobe was created by the interaction of the SNR shock and the
supernova ejecta with dense and inhomogeneous medium in the environment of SNR
CTB 109. The newly calculated age of the SNR is t ~ 1.4 x 10^4 yr.Comment: Accepted for publication in A&A. 9 pages, 10 figure
Spectral and temporal properties of the supergiant fast X-ray transient IGR J18483-0311 observed by INTEGRAL
IGR J18483-0311 is a supergiant fast X-ray transient whose compact object is
located in a wide (18.5 d) and eccentric (e~0.4) orbit, which shows sporadic
outbursts that reach X-ray luminosities of ~1e36 erg/s. We investigated the
timing properties of IGR J18483-0311 and studied the spectra during bright
outbursts by fitting physical models based on thermal and bulk Comptonization
processes for accreting compact objects. We analysed archival INTEGRAL data
collected in the period 2003-2010, focusing on the observations with IGR
J18483-0311 in outburst. We searched for pulsations in the INTEGRAL light
curves of each outburst. We took advantage of the broadband observing
capability of INTEGRAL for the spectral analysis. We observed 15 outbursts,
seven of which we report here for the first time. This data analysis almost
doubles the statistics of flares of this binary system detected by INTEGRAL. A
refined timing analysis did not reveal a significant periodicity in the
INTEGRAL observation where a ~21s pulsation was previously detected. Neither
did we find evidence for pulsations in the X-ray light curve of an archival
XMM-Newton observation of IGR J18483-0311. In the light of these results the
nature of the compact object in IGR J18483-0311 is unclear. The broadband X-ray
spectrum of IGR J18483-0311 in outburst is well fitted by a thermal and bulk
Comptonization model of blackbody seed photons by the infalling material in the
accretion column of a neutron star. We also obtained a new measurement of the
orbital period using the Swift/BAT light curve.Comment: Accepted for publication in Astronomy and Astrophysics. 8 page
Analysis on Aging in the Generalized Random Energy Model
A new dynamics more natural than that proposed by Bouchaud and Dean is
introduced to the Generalized Random Energy Model, and the master equation for
the dynamics is solved exactly to calculate the time correlation function.
Although our results are very similar to those obtained by Bouchaud and Dean
qualitatively, the exponents for power law relaxation are different. The
Zero-Field-Cooled magnetization is also calculated with a relation between the
correlation function and the response function which holds even if the
relaxation is non-equilibrium. The validity of these analytic results are
confirmed by numerical simulations.Comment: 12 pages, 5 figures, submitted to J. Phys. Sci. Jp
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