148 research outputs found
Bacterial isolates from patients with preterm labor with and without preterm rupture of the fetal membranes.
OBJECTIVE: The aim of this study is to describe the bacterial flora of women in preterm labor with or without premature rupture of membranes. METHODS: Retrospective studies of 239 patients with preterm labor were performed. RESULTS: One hundred and twenty-three of 239 patients with preterm labor (51.5%) had bacterial vaginosis. Seventy of the 239 patients with preterm labor (29.3%) developed premature rupture of the membranes (preterm PROM). Of the 70 patients with preterm PROM, 51 (72.9%) had bacterial vaginosis. Therefore, 51 of the 123 patients with bacterial vaginosis (41.5%) developed preterm PROM. An increased number of organisms detected from the vaginal discharge in patients with preterm labor was associated with preterm PROM by Cochran-Armitage test. An increased number of organisms detected from the vaginal discharge in patients with preterm labor complicated with bacterial vaginosis was significantly associated with preterm PROM by Cochran-Armitage test. CONCLUSIONS: In preterm labor, the number of different species detected in the vagina provide sensitive and specific prediction of preterm PROM in patients with preterm labor
Circumbinary MHD Accretion into Inspiraling Binary Black Holes
As 2 black holes bound to each other in a close binary approach merger their
inspiral time becomes shorter than the characteristic inflow time of
surrounding orbiting matter. Using an innovative technique in which we
represent the changing spacetime in the region occupied by the orbiting matter
with a 2.5PN approximation and the binary orbital evolution with 3.5PN, we have
simulated the MHD evolution of a circumbinary disk surrounding an equal-mass
non-spinning binary. Prior to the beginning of the inspiral, the structure of
the circumbinary disk is predicted well by extrapolation from Newtonian
results. The binary opens a low-density gap whose radius is roughly two binary
separations, and matter piles up at the outer edge of this gap as inflow is
retarded by torques exerted by the binary; nonetheless, the accretion rate is
diminished relative to its value at larger radius by only about a factor of 2.
During inspiral, the inner edge of the disk at first moves inward in
coordination with the shrinking binary, but as the orbital evolution
accelerates, the rate at which the inner edge moves toward smaller radii falls
behind the rate of binary compression. In this stage, the rate of angular
momentum transfer from the binary to the disk slows substantially, but the net
accretion rate decreases by only 10-20%. When the binary separation is tens of
gravitational radii, the rest-mass efficiency of disk radiation is a few
percent, suggesting that supermassive binary black holes in galactic nuclei
could be very luminous at this stage of their evolution. If the luminosity were
optically thin, it would be modulated at a frequency that is a beat between the
orbital frequency of the disk's surface density maximum and the binary orbital
frequency. However, a disk with sufficient surface density to be luminous
should also be optically thick; as a result, the periodic modulation may be
suppressed.Comment: 54 pages, color figures, submitted to the Astrophysical Journal, a
high resolution version and movies can be found at
http://ccrg.rit.edu/~scn/cmhdaiibh
Properties of Accretion Flows Around Coalescing Supermassive Black Holes
What are the properties of accretion flows in the vicinity of coalescing
supermassive black holes (SBHs)? The answer to this question has direct
implications for the feasibility of coincident detections of electromagnetic
(EM) and gravitational wave (GW) signals from coalescences. Such detections are
considered to be the next observational grand challenge that will enable
testing general relativity in the strong, nonlinear regime and improve our
understanding of evolution and growth of these massive compact objects. In this
paper we review the properties of the environment of coalescing binaries in the
context of the circumbinary disk and hot, radiatively inefficient accretion
flow models and use them to mark the extent of the parameter space spanned by
this problem. We report the results from an ongoing, general relativistic,
hydrodynamical study of the inspiral and merger of black holes, motivated by
the latter scenario. We find that correlated EM+GW oscillations can arise
during the inspiral phase followed by the gradual rise and subsequent drop-off
in the light curve at the time of coalescence. While there are indications that
the latter EM signature is a more robust one, a detection of either signal
coincidentally with GWs would be a convincing evidence for an impending SBH
binary coalescence. The observability of an EM counterpart in the hot accretion
flow scenario depends on the details of a model. In the case of the most
massive binaries observable by the Laser Interferometer Space Antenna, upper
limits on luminosity imply that they may be identified by EM searches out to
z~0.1-1. However, given the radiatively inefficient nature of the gas flow, we
speculate that a majority of massive binaries may appear as low luminosity AGN
in the local universe.Comment: Revised version accepted to Class. Quantum Grav. for proceedings of
8th LISA Symposium. 15 pages, 3 figures, includes changes suggested in
referee report
Observable Signatures of EMRI Black Hole Binaries Embedded in Thin Accretion Disks
We examine the electromagnetic (EM) and gravitational wave (GW) signatures of
stellar-mass compact objects (COs) spiraling into a supermassive black hole
(extreme mass-ratio inspirals or EMRIs), embedded in a thin, radiation-pressure
dominated, accretion disk. At large separations, the tidal effect of the
secondary CO clears a gap. We show that the gap refills during the late
GW-driven phase of the inspiral, leading to a sudden EM brightening of the
source. The accretion disk leaves an imprint on the GW through its angular
momentum exchange with the binary, the mass increase of the binary members due
to accretion, and its gravity. We compute the disk-modified GWs both in an
analytical Newtonian approximation and in a numerical effective-one-body
approach. We find that disk-induced migration provides the dominant
perturbation to the inspiral, with weaker effects from the mass accretion onto
the CO and hydrodynamic drag. Depending on whether a gap is present, the
perturbation of the GW phase is between 10 and 1000 radians per year,
detectable with the future Laser Interferometer Space Antenna (LISA) at high
significance. The Fourier transform of the disk-modified GW in the stationary
phase approximation is sensitive to disk parameters with a frequency trend
different from post-Newtonian vacuum corrections. Our results suggest that
observations of EMRIs may place new sensitive constraints on the physics of
accretion disks.Comment: 42 pages, 8 figures, 3 tables, submitted to Phys. Rev.
Modeling high-energy light curves of the PSR B1259-63/LS 2883 binary based on 3-D SPH simulations
Temporal changes of X-ray to very-high-energy gamma-ray emissions from the
pulsar-Be star binary PSR B1259-63/LS 2883 are studied based on 3-D SPH
simulations of pulsar wind interaction with Be-disk and wind. We focus on the
periastron passage of the binary and calculate the variation of the synchrotron
and inverse-Compton emissions using the simulated shock geometry and pressure
distribution of the pulsar wind. The characteristic double-peaked X-ray light
curve from observations is reproduced by our simulation under a dense Be disk
condition (base density ~10^{-9} g cm^{-3}). We interpret the pre- and
post-periastron peaks as being due to a significant increase in the conversion
efficiency from pulsar spin down power to the shock-accelerated particle energy
at orbital phases when the pulsar crosses the disk before periastron passage,
and when the pulsar wind creates a cavity in the disk gas after periastron
passage, respectively. On the contrary, in the model TeV light curve, which
also shows a double peak feature, the first peak appears around the periastron
phase. The possible effects of cooling processes on the TeV light curve are
briefly discussed.Comment: 32 pages, 6 figues. Accepted for publication in Ap
Three Dimensional MHD Simulation of Circumbinary Accretion Disks: Disk Structures and Angular Momentum Transport
We present the first three-dimensional magnetohydrodynamic (MHD) simulations
of a circumbinary disk surrounding an equal mass binary. The binary maintains a
fixed circular orbit of separation . As in previous hydrodynamical
simulations, strong torques by the binary can maintain a gap of radius . Streams curve inward from toward the binary; some of their
mass passes through the inner boundary, while the remainder swings back out to
the disk. However, we also find that near its inner edge the disk develops both
a strong asymmetry and growing orbital eccentricity. Because the MHD
stresses introduce more matter into the gap, the total torque per unit disk
mass is times larger than found previously. The inner boundary
accretion rate per unit disk mass is times greater than found from
previous hydrodynamical calculations. The implied binary shrinkage rate is
determined by a balance between the rate at which the binary gains angular
momentum by accretion and loses it by gravitational torque. The large accretion
rate brings these two rates nearly into balance, but in net, we find that , and its magnitude is about 2.7 times larger than predicted by the
earlier hydrodynamic simulations. If the binary comprises two massive black
holes, the accretion rate may be great enough for one or both to be AGN, with
consequences for the physical state of the gas both in the disk body and in its
inner gap.Comment: 69 pages,19 figures, ApJ accepted version (add one more appendix
discussing the binary's eccentricity growth
The pre-outburst flare of the A 0535+26 August/September 2005 outburst
We study the spectral and temporal behavior of the High Mass X-ray Binary A
0535+26 during a `pre-outburst flare' which took place ~5 d before the peak of
a normal (type I) outburst in August/September 2005. We compare the studied
behavior with that observed during the outburst. We analyse RXTE observations
that monitored A 0535+26 during the outburst. We complete spectral and timing
analyses of the data. We study the evolution of the pulse period, present
energy-dependent pulse profiles both at the initial pre-outburst flare and
close to outburst maximum, and measure how the cyclotron resonance-scattering
feature (hereafter CRSF) evolves. We present three main results: a constant
period P=103.3960(5)s is measured until periastron passage, followed by a
spin-up with a decreasing period derivative of Pdot=(-1.69+/-0.04)x10^(-8)s/s
at MJD 53618, and P remains constant again at the end of the main outburst. The
spin-up provides evidence for the existence of an accretion disk during the
normal outburst. We measure a CRSF energy of Ecyc~50kev during the pre-outburst
flare, and Ecyc~46kev during the main outburst. The pulse shape, which varies
significantly during both pre-outburst flare and main outburst, evolves
strongly with photon energy.Comment: 4 pages, 4 figures, accepted for publication in A&A Letters. To be
published in parallel to Postnov et al. 200
Modelling Circumbinary Gas Flows in Close T Tauri Binaries
Young close binaries open central gaps in the surrounding circumbinary
accretion disc, but the stellar components may still gain mass from gas
crossing through the gap. It is not well understood how this process operates
and how the stellar components are affected by such inflows. Our main goal is
to investigate how gas accretion takes place and evolves in close T Tauri
binary systems. In particular, we model the accretion flows around two close T
Tauri binaries, V4046 Sgr and DQ Tau, both showing periodic changes in emission
lines, although their orbital characteristics are very different. In order to
derive the density and velocity maps of the circumbinary material, we employ
two-dimensional hydrodynamic simulations with a locally isothermal equation of
state. The flow patterns become quasi-stable after a few orbits in the frame
co-rotating with the system. Gas flows across the circumbinary gap through the
co-rotating Lagrangian points, and local circumstellar discs develop around
both components. Spiral density patterns develop in the circumbinary disc that
transport angular momentum efficiently. Mass is preferentially channelled
towards the primary and its circumstellar disc is more massive than the disc
around the secondary. We also compare the derived density distribution to
observed line profile variability. The line profile variability tracing the gas
flows in the central cavity shows clear similarities with the corresponding
observed line profile variability in V4046 Sgr, but only when the local
circumstellar disc emission was excluded. Closer to the stars normal
magnetospheric accretion may dominate while further out the dynamic accretion
process outlined here dominates. Periodic changes in the accretion rates onto
the stars can explain the outbursts of line emission observed in eccentric
systems such as DQ Tau.Comment: Accepted for publication in MNRA
Massive binary black holes in galactic nuclei and their path to coalescence
Massive binary black holes form at the centre of galaxies that experience a
merger episode. They are expected to coalesce into a larger black hole,
following the emission of gravitational waves. Coalescing massive binary black
holes are among the loudest sources of gravitational waves in the Universe, and
the detection of these events is at the frontier of contemporary astrophysics.
Understanding the black hole binary formation path and dynamics in galaxy
mergers is therefore mandatory. A key question poses: during a merger, will the
black holes descend over time on closer orbits, form a Keplerian binary and
coalesce shortly after? Here we review progress on the fate of black holes in
both major and minor mergers of galaxies, either gas-free or gas-rich, in
smooth and clumpy circum-nuclear discs after a galactic merger, and in
circum-binary discs present on the smallest scales inside the relic nucleus.Comment: Accepted for publication in Space Science Reviews. To appear in hard
cover in the Space Sciences Series of ISSI "The Physics of Accretion onto
Black Holes" (Springer Publisher
Aging-associated renal disease in mice is fructokinase dependent
Aging-associated kidney disease is usually considered a degenerative process associated with aging. Recently, it has been shown that animals can produce fructose endogenously, and that this can be a mechanism for causing kidney damage in diabetic nephropathy and in association with recurrent dehydration. We therefore hypothesized that low-level metabolism of endogenous fructose might play a role in aging-associated kidney disease. Wild-type and fructokinase knockout mice were fed a normal diet for 2 yr that had minimal (<5%) fructose content. At the end of 2 yr, wild-type mice showed elevations in systolic blood pressure, mild albuminuria, and glomerular changes with mesangial matrix expansion, variable mesangiolysis, and segmental thrombi. The renal injury was amplified by provision of high-salt diet for 3 wk, as noted by the presence of glomerular hypertrophy, mesangial matrix expansion, and alpha smooth muscle actin expression, and with segmental thrombi. Fructokinase knockout mice were protected from renal injury both at baseline and after high salt intake (3 wk) compared with wild-type mice. This was associated with higher levels of active (phosphorylated serine 1177) endothelial nitric oxide synthase in their kidneys. These studies suggest that aging-associated renal disease might be due to activation of specific metabolic pathways that could theoretically be targeted therapeutically, and raise the hypothesis that aging-associated renal injury may represent a disease process as opposed to normal age-related degeneration.
aging is associated with the development of glomerulosclerosis and tubulointerstitial disease in humans and rodents (12, 23, 35). Interestingly, aging-associated renal injury can vary greatly, and some individuals may show minimal reduction in kidney function and relatively preserved kidney histology with age. This raises the possibility that some of the “normal” deterioration in renal function during the aging process observed in Western cultures may be subtle renal injury driven by diet or other mechanisms.
The ingestion of sugar has been associated with albuminuria in humans (3, 4, 31). Sugar contains fructose and glucose, and evidence suggests that the fructose component may be responsible for the renal injury. Specifically, fructose is metabolized in the proximal tubule by fructokinase, and this results in transient ATP depletion with the generation of oxidative stress and inflammatory mediators such as monocyte chemoattractant protein-1 (MCP-1) (5). The administration of fructose to rats results in modest proximal tubular injury, and has also been shown to accelerate preexistent kidney disease (9, 26). Fructose metabolism also results in the generation of uric acid, and this is associated with the development of afferent arteriolar disease with loss of autoregulation, resulting in glomerular hypertension (29, 30). While most studies have focused on dietary fructose, fructose can also be generated in the kidney and liver by the aldose reductase-sorbitol dehydrogenase polyol pathway, and modest fructose levels can be detected even in fasting animals (13, 21). Indeed, fructose can be generated in the kidney in diabetes or with dehydration, and in both situations may lead to local renal damage (20, 28).
We hypothesized that some of the renal damage associated with aging could be due to fructose-dependent renal injury, even in the absence of dietary fructose. To investigate this hypothesis, we studied aging wild-type mice and aging mice that could not metabolize fructose via the fructokinase-dependent pathway [fructokinase knockout, also known as ketohexokinase knockout (KHK-A/C KO mice)]. KHK-A/C KO mice have a normal phenotype when young (6), but have not been examined in the aging state
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