2,502 research outputs found
Topological persistence and dynamical heterogeneities near jamming
We introduce topological methods for quantifying spatially heterogeneous
dynamics, and use these tools to analyze particle-tracking data for a
quasi-two-dimensional granular system of air-fluidized beads on approach to
jamming. In particular we define two overlap order parameters, which quantify
the correlation between particle configurations at different times, based on a
Voronoi construction and the persistence in the resulting cells and nearest
neighbors. Temporal fluctuations in the decay of the persistent area and bond
order parameters define two alternative dynamic four-point susceptibilities,
XA(t) and XB(t), well-suited for characterizing spatially-heterogeneous
dynamics. These are analogous to the standard four-point dynamic susceptibility
X4(l,t), but where the space-dependence is fixed uniquely by topology rather
than by discretionary choice of cutoff function. While these three
susceptibilities yield characteristic time scales that are somewhat different,
they give domain sizes for the dynamical heterogeneities that are in good
agreement and that diverge on approach to jamming
The partition of energy for air-fluidized grains
The dynamics of one and two identical spheres rolling in a nearly-levitating
upflow of air obey the Langevin Equation and the Fluctuation-Dissipation
Relation [Ojha et al. Nature 427, 521 (2004) and Phys. Rev. E 71, 01631
(2005)]. To probe the range of validity of this statistical mechanical
description, we perturb the original experiments in four ways. First, we break
the circular symmetry of the confining potential by using a stadium-shaped
trap, and find that the velocity distributions remain circularly symmetric.
Second, we fluidize multiple spheres of different density, and find that all
have the same effective temperature. Third, we fluidize two spheres of
different size, and find that the thermal analogy progressively fails according
to the size ratio. Fourth, we fluidize individual grains of aspherical shape,
and find that the applicability of statistical mechanics depends on whether or
not the grain chatters along its length, in the direction of airflow.Comment: experimen
Carbon-enhanced metal-poor stars: a window on AGB nucleosynthesis and binary evolution. II. Statistical analysis of a sample of 67 CEMP- stars
Many observed CEMP stars are found in binary systems and show enhanced
abundances of -elements. The origin of the chemical abundances of these
CEMP- stars is believed to be accretion in the past of enriched material
from a primary star in the AGB phase. We investigate the mechanism of mass
transfer and the process of nucleosynthesis in low-metallicity AGB stars by
modelling the binary systems in which the observed CEMP- stars were formed.
For this purpose we compare a sample of CEMP- stars with a grid of
binary stars generated by our binary evolution and nucleosynthesis model. We
classify our sample CEMP- stars in three groups based on the observed
abundance of europium. In CEMP stars the europium-to-iron ratio is more
than ten times higher than in the Sun, whereas it is lower than this threshold
in CEMP stars. No measurement of europium is currently available for
CEMP- stars. On average our models reproduce well the abundances observed
in CEMP- stars, whereas in CEMP- stars and CEMP- stars the
abundances of the light- elements are systematically overpredicted by our
models and in CEMP- stars the abundances of the heavy- elements are
underestimated. In all stars our modelled abundances of sodium overestimate the
observations. This discrepancy is reduced only in models that underestimate the
abundances of most of the -elements. Furthermore, the abundance of lead is
underpredicted in most of our model stars. These results point to the
limitations of our AGB nucleosynthesis model, particularly in the predictions
of the element-to-element ratios. Finally, in our models CEMP- stars are
typically formed in wide systems with periods above 10000 days, while most of
the observed CEMP- stars are found in relatively close orbits with periods
below 5000 days.Comment: 23 pages, 8 figures, accepted for publication on Astronomy &
Astrophysic
Carbon-enhanced metal-poor stars: a window on AGB nucleosynthesis and binary evolution. I. Detailed analysis of 15 binary stars with known orbital periods
AGB stars are responsible for producing a variety of elements, including
carbon, nitrogen, and the heavy elements produced in the slow neutron-capture
process (-elements). There are many uncertainties involved in modelling the
evolution and nucleosynthesis of AGB stars, and this is especially the case at
low metallicity, where most of the stars with high enough masses to enter the
AGB have evolved to become white dwarfs and can no longer be observed. The
stellar population in the Galactic halo is of low mass () and only a few observed stars have evolved beyond the first
giant branch. However, we have evidence that low-metallicity AGB stars in
binary systems have interacted with their low-mass secondary companions in the
past. The aim of this work is to investigate AGB nucleosynthesis at low
metallicity by studying the surface abundances of chemically peculiar very
metal-poor stars of the halo observed in binary systems. To this end we select
a sample of 15 carbon- and -element-enhanced metal-poor (CEMP-) halo
stars that are found in binary systems with measured orbital periods. With our
model of binary evolution and AGB nucleosynthesis, we determine the binary
configuration that best reproduces, at the same time, the observed orbital
period and surface abundances of each star of the sample. The observed periods
provide tight constraints on our model of wind mass transfer in binary stars,
while the comparison with the observed abundances tests our model of AGB
nucleosynthesis.Comment: 18 pages, 20 figures, accepted for publication on A&
Baryonic acoustic oscillations simulations for the Large Synoptic Survey Telescope (LSST)
The baryonic acoustic oscillations are features in the spatial distribution
of the galaxies which, if observed at different epochs, probe the nature of the
dark energy. In order to be able to measure the parameters of the dark energy
equation of state to high precision, a huge sample of galaxies has to be used.
The Large Synoptic Survey Telescope will survey the optical sky with 6 filters
from 300nm and 1100nm, such that a catalog of galaxies with photometric
redshifts will be available for dark energy studies. In this article, we will
give a rough estimate of the impact of the photometric redshift uncertainties
on the computation of the dark energy parameter through the reconstruction of
the BAO scale from a simulated photometric catalog.Comment: 4 pages, 2 figures, 10th Rencontres de Blois proceedin
Spatially Heterogeneous Dynamics in a Granular System Near Jamming
In supercooled liquids and dense colloidal suspensions, strings of correlated motion represent a dynamical correlation length that grows as the glass transition is approached. Here, we present a granular system driven close to the jamming transition that shares this hallmark dynamical feature. In analogy, it exhibits a dynamical length scale that grows as the jamming transition is approached
Effective temperatures and activated dynamics for a two-dimensional air-driven granular system on two approaches to jamming
We present experiments on several distinct effective temperatures in a
granular system at a sequence of increasing packing densities and at a sequence
of decreasing driving rates. This includes single-grain measurements based on
the mechanical energies of both the grains and an embedded oscillator, as well
as a collective measurement based on the Einstein relation between diffusivity
and mobility, which all probe different time scales. Remarkably, all effective
temperatures agree. Furthermore, mobility data along the two trajectories
collapse when plotted vs effective temperature and exhibit an Arrhenius form
with the same energy barrier as the microscopic relaxation time
Penetration depth for shallow impact cratering
We present data for the penetration of a variety of spheres, dropped from
rest, into a level non-cohesive granular medium. We improve upon our earlier
work [Uehara {\it et al.} Phys. Rev. Lett. {\bf 90}, 194301 (2003)] in three
regards. First, we explore the behavior vs sphere diameter and density more
systematically, by holding one of these parameters constant while varying the
other. Second, we prepare the granular medium more reproducibly and, third, we
measure the penetration depth more accurately. The new data support our
previous conclusion that the penetration depth is proportional to the 1/2 power
of sphere density, the 2/3 power of sphere diameter, and the 1/3 power of total
drop distance
Modelling the observed properties of carbon-enhanced metal-poor stars using binary population synthesis
The stellar population in the Galactic halo is characterised by a large
fraction of CEMP stars. Most CEMP stars are enriched in -elements (CEMP-
stars), and some of these are also enriched in -elements (CEMP- stars).
One formation scenario proposed for CEMP stars invokes wind mass transfer in
the past from a TP-AGB primary star to a less massive companion star which is
presently observed. We generate low-metallicity populations of binary stars to
reproduce the observed CEMP-star fraction. In addition, we aim to constrain our
wind mass-transfer model and investigate under which conditions our synthetic
populations reproduce observed abundance distributions. We compare the CEMP
fractions and the abundance distributions determined from our synthetic
populations with observations. Several physical parameters of the binary
stellar population of the halo are uncertain, e.g. the initial mass function,
the mass-ratio and orbital-period distributions, and the binary fraction. We
vary the assumptions in our model about these parameters, as well as the wind
mass-transfer process, and study the consequent variations of our synthetic
CEMP population. The CEMP fractions calculated in our synthetic populations
vary between 7% and 17%, a range consistent with the CEMP fractions among very
metal-poor stars recently derived from the SDSS/SEGUE data sample. The results
of our comparison between the modelled and observed abundance distributions are
different for CEMP- stars and for CEMP- stars. For the latter, our
simulations qualitatively reproduce the observed distributions of C, Na, Sr,
Ba, Eu, and Pb. Contrarily, for CEMP- stars our model cannot reproduce the
large abundances of neutron-rich elements such as Ba, Eu, and Pb. This result
is consistent with previous studies, and suggests that CEMP- stars
experienced a different nucleosynthesis history to CEMP- stars.Comment: 17 pages, 11 figures, accepted for publication on Astronomy and
Astrophysic
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Linked optical and gene expression profiling of single cells at high-throughput.
Single-cell RNA sequencing has emerged as a powerful tool for characterizing cells, but not all phenotypes of interest can be observed through changes in gene expression. Linking sequencing with optical analysis has provided insight into the molecular basis of cellular function, but current approaches have limited throughput. Here, we present a high-throughput platform for linked optical and gene expression profiling of single cells. We demonstrate accurate fluorescence and gene expression measurements on thousands of cells in a single experiment. We use the platform to characterize DNA and RNA changes through the cell cycle and correlate antibody fluorescence with gene expression. The platform's ability to isolate rare cell subsets and perform multiple measurements, including fluorescence and sequencing-based analysis, holds potential for scalable multi-modal single-cell analysis
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