2,394 research outputs found
The solubility of rhenium in silicate melts: Implications for the geochemical properties of rhenium at high temperatures
The solubility of rhenium (Re) in a haplobasaltic melt (anorthite-diopside eutectic composition) has been experimentally determined using the mechanically assisted equilibration technique at 1400°C as a function of oxygen fugacity (10â12 < fO2 †10â7 bar), imposed by CO-CO2 gas mixtures. Samples were analysed by laser ablation-inductively coupled plasma-mass spectrometry (LA-ICP-MS). This is a true microanalytical technique, which allows small-scale sample heterogeneity to be detected, while providing a limit of detection of 2 ppb Re. Time-resolved LA-ICP-MS spectra revealed the presence of suboptically sized micronuggets of Re in all samples, which, because they are present at the 0.5 to 10 ppm level, dominate the true solubilities of Re (<1 ppm at the conditions of the experiment) in bulk analyses of the samples. Nevertheless, the micronuggets could be filtered out from the time-resolved spectra to reveal accurate values of the true Re solubility. A number of time series of samples were taken at constant fO2 to demonstrate that the solubilities converge to a constant value. In addition, solubilities were measured after increasing and decreasing the imposed fO2. The results show that Re dissolves in the silicate melt as ReO2 (Re4+) and ReO3 (Re6+) species, with the latter predominating at typical terrestrial upper-mantle oxygen fugacities. The total solubility of Re is described by the following expression (fO2 in bars): [Re/ppb] = 9.7(±1.9) Ă 109 (fO2) + 4.2 (±0.3) Ă 1014 (fO2)1.5Assuming an activity coefficient for Re in Fe-rich metal of 1, this gives a value of DRemet/sil of 5 Ă 1010 at log fO2 = IW-2, appropriate for metal-silicate partitioning in an homogenously accreting Earth. Thus, Re is indeed very highly siderophile, and the mantleâs abundance cannot be explained by homogenous accretion
Quasi-conservation laws for compressible 3D Navier-Stokes flow
We formulate the quasi-Lagrangian fluid transport dynamics of mass density
and the projection q=\bom\cdot\nabla\rho of the vorticity \bom onto
the density gradient, as determined by the 3D compressible Navier-Stokes
equations for an ideal gas, although the results apply for an arbitrary
equation of state. It turns out that the quasi-Lagrangian transport of
cannot cross a level set of . That is, in this formulation, level sets of
(isopychnals) are impermeable to the transport of the projection .Comment: 2 page note, to appear in Phys Rev
Delayed kinetics of poliovirus RNA synthesis in a human cell line with reduced levels of hnRNP C proteins.
The hnRNP C heterotetramer [(C1(3))C2] binds RNA polymerase II transcripts in the nucleus, along with other proteins of the core hnRNP complex, and plays an important role in mRNA biogenesis and transport. Infection of HeLa cells with poliovirus causes hnRNP C to re-localize from the nucleus, where it is normally retained during interphase, to the cytoplasm. We have proposed that in the cytoplasm, the protein isoforms of hnRNP C participate in the recognition of viral specific RNAs by the poliovirus replication proteins and/or in the assembly of membrane-bound RNA replication complexes. In SK-OV-3 cells, which express reduced levels of hnRNP C compared to HeLa cells or 293 cells, the kinetics of poliovirus replication are delayed. hnRNP C is also re-localized from the nucleus to the cytoplasm in SK-OV-3 cells infected with poliovirus. Increased expression of hnRNP C in SK-OV-3 cells by transient transfection increases the rate of virus production and overall yield over that seen in mock-transfected cells. We propose that hnRNP C interacts with poliovirus RNA and replication proteins to increase the efficiency of viral genomic RNA synthesis
An Extreme-AO Search for Giant Planets around a White Dwarf --VLT/SPHERE performance on a faint target GD 50
CONTEXT. Little is known about the planetary systems around single white
dwarfs although there is strong evidence that they do exist.
AIMS. We performed a pilot study with the extreme-AO system on the
Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) on the Very
Large Telescopes (VLT) to look for giant planets around a young white dwarf, GD
50.
METHODS. We were awarded science verification time on the new ESO instrument
SPHERE. Observations were made with the InfraRed Dual-band Imager and
Spectrograph in classical imaging mode in H band.
RESULTS. Despite the faintness of the target (14.2 mag in R band), the AO
loop was closed and a strehl of 37\% was reached in H band. No objects were
detected around GD 50. We achieved a 5-sigma contrast of 6.2, 8.0 and 8.25 mags
at 0{\farcs}2, 0{\farcs}4 and 0{\farcs}6 and beyond, respectively. We exclude
any substellar objects more massive than 4.0 M at 6.2 AU, 2.9
M at 12.4 AU and 2.8 M at 18.6 AU and beyond. This
rivals the previous upper limit set by Spitzer. We further show that SPHERE is
the most promising instrument available to search for close-in substellar
objects around nearby white dwarfs.Comment: A&A letters, accepte
Collisional modelling of the debris disc around HIP 17439
We present an analysis of the debris disc around the nearby K2 V star HIP
17439. In the context of the Herschel DUNES key programme the disc was observed
and spatially resolved in the far-IR with the Herschel PACS and SPIRE
instruments. In a first model, Ertel et al. (2014) assumed the size and radial
distribution of the circumstellar dust to be independent power laws. There, by
exploring a very broad range of possible model parameters several scenarios
capable of explaining the observations were suggested. In this paper, we
perform a follow-up in-depth collisional modelling of these scenarios trying to
further distinguish between them. In our models we consider collisions, direct
radiation pressure, and drag forces, i.e. the actual physical processes
operating in debris discs. We find that all scenarios discussed in Ertel et al.
are physically sensible and can reproduce the observed SED along with the PACS
surface brightness profiles reasonably well. In one model, the dust is produced
beyond 120au in a narrow planetesimal belt and is transported inwards by
Poynting-Robertson and stellar wind drag. A good agreement with the observed
radial profiles would require stellar winds by about an order of magnitude
stronger than the solar value, which is not supported, although not ruled out,
by observations. Another model consists of two spatially separated planetesimal
belts, a warm inner and a cold outer one. This scenario would probably imply
the presence of planets clearing the gap between the two components. Finally,
we show qualitatively that the observations can be explained by assuming the
dust is produced in a single, but broad planetesimal disc with a surface
density of solids rising outwards, as expected for an extended disc that
experiences a natural inside-out collisional depletion. Prospects of
discriminating between the competing scenarios by future observations are
discussed.Comment: Astronomy and Astrophysics (accepted for publication). 11 pages, 8
figure
Social Determinants of Health and HIV/AIDS in Florida
As of 2016, there were reported to be 135,986 people living with HIV/AIDS (PLWH) in Florida alone, and its cities lead the nationâs incidence rates at around 5,000 new HIV diagnoses annually. Using a few social determinants of health (SDH) associated with deaths of despair (DOD), this paper aims to connect HIV rates to SDH to gain more understanding of how SDH can aid in the alleviation of HIV through public health policy and social change. Methods: This analysis evaluated the predictive ability of the SDH: Education, Insurance, Race, and RaceXEducation for HIV incidence in Florida using regression analysis. Results: A backwards regression analysis using the four variables a) Race, b) Insurance, c) Education, and d) RaceXEducation was statistically significant, F(4,51) = 11.10, p \u3c .001, and accounted for 42% of the variance in HIV incidence. Higher rates of white residents and insured residents was associated with a significant decrease in HIV rate (ps \u3c .05), while higher levels of education were associated with a significant increase in HIV rate (p \u3c .001). The RaceXEducation interaction was significant in the negative direction (p = .001). Conclusion: Social Determinants of Health, particularly education and race, have a significant effect on HIV/AIDS prevalence and incidence and are great predictors of HIV status in Florida
An independent determination of Fomalhaut b's orbit and the dynamical effects on the outer dust belt
The nearby star Fomalhaut harbours a cold, moderately eccentric dust belt
with a sharp inner edge near 133 au. A low-mass, common proper motion companion
(Fom b), was discovered near the inner edge and was identified as a planet
candidate that could account for the belt morphology. However, the most recent
orbit determination based on four epochs of astrometry over eight years reveals
a highly eccentric orbit that appears to cross the belt in the sky plane
projection. We perform here a full orbital determination based on the available
astrometric data to independently validate the orbit estimates previously
presented. Adopting our values for the orbital elements and their associated
uncertainties, we then study the dynamical interaction between the planet and
the dust ring, to check whether the proposed disk sculpting scenario by Fom b
is plausible. We used a dedicated MCMC code to derive the statistical
distributions of the orbital elements of Fom b. Then we used symplectic N-body
integration to investigate the dynamics of the dust belt, as perturbed by a
single planet. Different attempts were made assuming different masses for Fom
b. We also performed a semi-analytical study to explain our results. Our
results are in good agreement with others regarding the orbit of Fom b. We find
that the orbit is highly eccentric, is close to apsidally aligned with the
belt, and has a moderate mutual inclination relative to the belt plane of. If
coplanar, this orbit crosses the disk. Our dynamical study then reveals that
the observed planet could sculpt a transient belt configuration with a similar
eccentricity to what is observed, but it would not be simultaneously apsidally
aligned with the planet. This transient configuration only occurs a short time
after the planet is placed on such an orbit (assuming an initially circular
disk), a time that is inversely proportional to the planet's mass, and that is
in any case much less than the 440 Myr age of the star. We constrain how long
the observed dust belt could have survived with Fom b on its current orbit, as
a function of its possible mass. This analysis leads us to conclude that Fom b
is likely to have low mass, that it is unlikely to be responsible for the
sculpting of the belt, and that it supports the hypothesis of a more massive,
less eccentric planet companion Fom c.Comment: 17 pages, 15 figures, accepted for publication in Astronomy \&
Astrophysic
Collisional modelling of the AU Microscopii debris disc
The spatially resolved AU Mic debris disc is among the most famous and
best-studied debris discs. We aim at a comprehensive understanding of the dust
production and the dynamics of the disc objects with in depth collisional
modelling including stellar radiative and corpuscular forces. Our models are
compared to a suite of observational data for thermal and scattered light
emission, ranging from the ALMA radial surface brightness profile at 1.3mm to
polarisation measurements in the visible. Most of the data can be reproduced
with a planetesimal belt having an outer edge at around 40au and subsequent
inward transport of dust by stellar winds. A low dynamical excitation of the
planetesimals with eccentricities up to 0.03 is preferred. The radial width of
the planetesimal belt cannot be constrained tightly. Belts that are 5au and
17au wide, as well as a broad 44au-wide belt are consistent with observations.
All models show surface density profiles increasing with distance from the star
as inferred from observations. The best model is achieved by assuming a stellar
mass loss rate that exceeds the solar one by a factor of 50. While the SED and
the shape of the ALMA profile are well reproduced, the models deviate from the
scattered light data more strongly. The observations show a bluer disc colour
and a lower degree of polarisation for projected distances <40au than predicted
by the models. The problem may be mitigated by irregularly-shaped dust grains
which have scattering properties different from the Mie spheres used. From
tests with a handful of selected dust materials, we derive a preference for
mixtures of silicate, carbon, and ice of moderate porosity. We address the
origin of the unresolved central excess emission detected by ALMA and show that
it cannot stem from an additional inner belt alone. Instead, it should derive,
at least partly, from the chromosphere of the central star.Comment: Astronomy and Astrophysics (accepted for publication), 18 pages, 11
figure
Interpreting the extended emission around three nearby debris disc host stars
Cool debris discs are a relic of the planetesimal formation process around
their host star, analogous to the solar system's Edgeworth-Kuiper belt. As
such, they can be used as a proxy to probe the origin and formation of
planetary systems like our own. The Herschel Open Time Key Programmes "DUst
around NEarby Stars" (DUNES) and "Disc Emission via a Bias-free Reconnaissance
in the Infrared/Submillimetre" (DEBRIS) observed many nearby, sun-like stars at
far-infrared wavelengths seeking to detect and characterize the emission from
their circumstellar dust. Excess emission attributable to the presence of dust
was identified from around 20% of stars. Herschel's high angular
resolution ( 7" FWHM at 100 m) provided the capacity for resolving
debris belts around nearby stars with radial extents comparable to the solar
system (50 to 100 au). As part of the DUNES and DEBRIS surveys, we obtained
observations of three debris disc stars, HIP 22263 (HD 30495), HIP 62207 (HD
110897), and HIP 72848 (HD 131511), at far-infrared wavelengths with the
Herschel PACS instrument. Combining these new images and photometry with
ancilliary data from the literature, we undertook simultaneous multi-wavelength
modelling of the discs' radial profiles and spectral energy distributions using
three different methodologies: single annulus, modified black body, and a
radiative transfer code. We present the first far-infrared spatially resolved
images of these discs and new single-component debris disc models. We
characterize the capacity of the models to reproduce the disc parameters based
on marginally resolved emission through analysis of two sets of simulated
systems (based on the HIP 22263 and HIP 62207 data) with the noise levels
typical of the Herschel images. We find that the input parameter values are
recovered well at noise levels attained in the observations presented here.Comment: 13 pages, 5 figures, 5 tables, accepted for publication in A&
MYCOPLASMA STUDIES OF HUMAN LEUKEMIA *
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/72000/1/j.1749-6632.1967.tb27701.x.pd
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