6,415 research outputs found
Monte Carlo calculations of diatomic molecule gas flows including rotational mode excitation
The direct simulation Monte Carlo method was used to solve the Boltzmann equation for flows of an internally excited nonequilibrium gas, namely, of rotationally excited homonuclear diatomic nitrogen. The semi-classical transition probability model of Itikawa was investigated for its ability to simulate flow fields far from equilibrium. The behavior of diatomic nitrogen was examined for several different nonequilibrium initial states that are subjected to uniform mean flow without boundary interactions. A sample of 1000 model molecules was observed as the gas relaxed to a steady state starting from three specified initial states. The initial states considered are: (1) complete equilibrium, (2) nonequilibrium, equipartition (all rotational energy states are assigned the mean energy level obtained at equilibrium with a Boltzmann distribution at the translational temperature), and (3) nonequipartition (the mean rotational energy is different from the equilibrium mean value with respect to the translational energy states). In all cases investigated the present model satisfactorily simulated the principal features of the relaxation effects in nonequilibrium flow of diatomic molecules
Spatial and Dynamical Biases in Velocity Statistics of Galaxies
We present velocity statistics of galaxies and their biases inferred from the
statistics of the underlying dark matter using a cosmological hydrodynamic
simulation of galaxy formation in low-density and spatially flat cold dark
matter cosmogony. We find that the pairwise velocity dispersion (PVD) of all
galaxies is significantly lower than that of the dark matter particles, and
that the PVD of the young galaxies is lower than that of the old types, and
even of all galaxies together, especially at small separations. These results
are in reasonable agreement with the recent measurements of PVDs in the Las
Campanas redshift survey, the PSCz catalogue and the SDSS data. We also find
that the low PVD of young galaxies is due to the effects of dynamical friction
as well as the different spatial distribution. We also consider the mean infall
velocity and the POTENT density reconstruction that are often used to measure
the cosmological parameters, and investigate the effects of spatial bias and
dynamical friction. In our simulation, the mean infall velocity of young
galaxies is significantly lower than that of all the galaxies or of the old
galaxies, and the dynamical bias becomes important on scales less than 3Mpc/h.
The mass density field reconstructed from the velocity field of young galaxies
using the POTENT-style method suffers in accuracy both from the spatial bias
and the dynamical friction on the smoothing scale of R_s=8Mpc/h. On the other
hand, in the case of R_s=12Mpc/h, which is typically adopted in the actual
POTENT analysis, the density reconstruction based on various tracers of
galaxies is reasonably accurate.Comment: 29 pages, 11 figures, accepted for publication in the Ap
Confirming the Detection of an Intergalactic X-ray Absorber Toward PKS 2155-304
We present new observations on PKS 2155-304 with the Chandra Low Energy
Transmission Grating Spectrometer (LETG), using the Advanced CCD Imaging
Spectrometer (ACIS). We confirm the detection of an absorption line plausibly
identified as OVIII Ly-alpha from the warm-hot intergalactic medium associated
with a small group of galaxies along the line of sight, as originally reported
by Fang et al. 2002 (here after FANG02). Combining the previous observations in
FANG02 and five new, long observations on the same target, we increase the
total exposure time by a factor of three, and the total counts per resolution
element by a factor of five. The measured line equivalent width is smaller than
that observed in FANG02, but still consistent at 90% confidence. We also
analyze the XMM-Newton observations on the same target, as well as observations
using the Chandra LETG and the High Resolution Camera (HRC) combination. These
observations have been used to challenge our reported detection. While no line
is seen in either the XMM-Newton and the Chandra LETG+HRC data, we find that
our result is consistent with the upper limits from both data sets. We
attribute the non-detection to (1) higher quality of the Chandra LETG+ACIS
spectrum, and (2) the rather extended wings of the line spread functions of
both the XMM RGS and the Chandra LETG+HRC. We discuss the implication of our
observation on the temperature and density of the absorber. We also confirm the
detection of z ~ 0 OVII absorption and, comparing with previous Chandra
analysis, we obtain much tighter constraints on the line properties.Comment: 10 pages, 8 figures, accepted for publication in Ap
Systematic Investigation of Possibilities for New Physics Effects in b --> s Penguin Processes
Although recent experimental results in b-->s penguin process seem to be
roughly consistent with the standard model predictions, there may be still
large possibilities of new physics hiding in this processes. Therefore, here we
investigate systematically the potential new physics effects that may appear in
time-dependent CP asymmetries of B --> phi K^0, B--> eta^\prime K^0 and B-->
K^0 \pi^0 decay modes, by classifying the cases for the values of the
mixing-induced indirect CP asymmetries, S_{phi K^0}, S_{eta^\prime K^0}, S_{K^0
pi^0} which are compared to S_{J/psi K^0}. We also show that several B_s decay
modes may help to resolve the ambiguities in such an analysis. Through
combining analysis with the time-dependent CP asymmetries of B_s decay modes
such as B_s --> phi eta^\prime, B_s--> eta^\prime pi^0 and B_s --> K^0
bar{K}^0, we can determine where the new CP phases precisely come from.Comment: 17 pages, version to be published in Prog.Theor.Phy
Why is the condensed phase of DNA preferred at higher temperature? DNA compaction in the presence of a multivalent cation
Upon the addition of multivalent cations, a giant DNA chain exhibits a large
discrete transition from an elongated coil into a folded compact state. We
performed single-chain observation of long DNAs in the presence of a
tetravalent cation (spermine), at various temperatures and monovalent salt
concentrations. We confirmed that the compact state is preferred at higher
temperatures and at lower monovalent salt concentrations. This result is
interpreted in terms of an increase in the net translational entropy of small
ions due to ionic exchange between higher and lower valence ions.Comment: 4pages,3figure
Modeling Intra-Cluster Gas in Triaxial Dark Halos : An Analytical Approach
We present the first physical model for the non-spherical intra-cluster gas
distribution in hydrostatic equilibrium under the gravity of triaxial dark
matter halos. Adopting the concentric triaxial density profiles of the dark
halos with constant axis ratios proposed by Jing & Suto (2002), we derive an
analytical expression for the triaxial halo potential on the basis of the
perturbation theory, and find the hydrostatic solutions for the gas density and
temperature profiles both in isothermal and polytropic equations of state. The
resulting iso-potential surfaces are well approximated by triaxial ellipsoids
with the eccentricities dependent on the radial distance. We also find a
formula for the eccentricity ratio between the intra-cluster gas and the
underlying dark halo. Our results allow one to determine the shapes of the
underlying dark halos from the observed intra-cluster gas through the X-ray
and/or the Sunyaev-Zel'dovich effects clusters.Comment: accepted by ApJ, LaTex file, 22 pages, 8 postscript figure
Locating the Warm-Hot Intergalactic Medium in the Simulated Local Universe
We present an analysis of mock spectral observation of warm-hot intergalactic
medium (WHIM) using a constrained simulation of the local universe. The
simulated map of oxygen emission lines from local WHIM reproduces well the
observed structures traced by galaxies in the real local universe. We further
attempt to perform mock observations of outer parts of simulated Coma cluster
and A3627 adopting the expected performance of DIOS (Diffuse Intergalactic
Oxygen Surveyor), which is proposed as a dedicated soft X-ray mission to search
for cosmic missing baryons. We find that WHIMs surrounding nearby clusters are
detectable with a typical exposure time of a day, and thus constitute realistic
and promising targets for DIOS. We also find that an X-ray emitting clump in
front of Coma cluster, recently reported in the XMM-Newton observation, has a
counterpart in the simulated local universe, and its observed spectrum can be
well reproduced in the simulated local universe if the gas temperature is set
to the observationally estimated value.Comment: 25 pages, 3 tables, 16 figures. Accepted for publication in PASJ.
High resolution PS/PDF files are available at
http://www-utap.phys.s.u-tokyo.ac.jp/~kohji/research/x-ray/index.htm
Properties of the cosmological filament between two clusters: A possible detection of a large-scale accretion shock by
We report on the results of a observation of the plasma in the
filament located between the two massive clusters of galaxies Abell 399 and
Abell 401. Abell 399 (=0.0724) and Abell 401 (=0.0737) are expected to be
in the initial phase of a cluster merger. In the region between the two
clusters, we find a clear enhancement in the temperature of the filament plasma
from 4 keV (expected value from a typical cluster temperature profile) to
6.5 keV. Our analysis also shows that filament plasma is present out to
a radial distance of 15' (1.3 Mpc) from a line connecting the two clusters. The
temperature profile is characterized by an almost flat radial shape with
6-7 keV within 10' or 0.8 Mpc. Across =8'~from the axis, the
temperature of the filament plasma shows a drop from 6.3 keV to 5.1 keV,
indicating the presence of a shock front. The Mach number based on the
temperature drop is estimated to be 1.3. We also successfully
determined the abundance profile up to 15' (1.3 Mpc), showing an almost
constant value (=0.3 solar) at the cluster outskirt. We estimated the
Compton -parameter to be 14.5, which is in
agreement with 's results (14-17 on the filament). The
line of sight depth of the filament is 1.1 Mpc, indicating that the
geometry of filament is likely a pancake shape rather than cylindrical. The
total mass of the filamentary structure is 7.7. We discuss a possible interpretation of the drop of X-ray emission
at the rim of the filament, which was pushed out by the merging activity and
formed by the accretion flow induced by the gravitational force of the
filament.Comment: 8 pages, 8 figures, accepted for publication in A&
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