4,083 research outputs found
Non-invasive estimation of left atrial dominant frequency in atrial fibrillation from different electrode sites: Insight from body surface potential mapping
© 2014, CardioFront LLC. All rights reserved. The dominant driving sources of atrial fibrillation are often found in the left atrium, but the expression of left atrial activation on the body surface is poorly understood. Using body surface potential mapping and simultaneous invasive measurements of left atrial activation our aim was to describe the expression of the left atrial dominant fibrillation frequency across the body surface. 20 patients in atrial fibrillation were studied. The spatial distributions of the dominant atrial fibrillation frequency across anterior and posterior sites on the body surface were quantified. Their relationship with invasive left atrial dominant fibrillation frequency was assessed by linear regression analysis, and the coefficient of determination was calculated for each body surface site. The correlation between intracardiac and body surface dominant frequency was significantly higher with posterior compared with anterior sites (coefficient of determination 67±8% vs 48±2%,
A high resolution mid-infrared survey of water emission from protoplanetary disks
We present the largest survey of spectrally resolved mid-infrared water
emission to date, with spectra for 11 disks obtained with the Michelle and
TEXES spectrographs on Gemini North. Water emission is detected in 6 of 8 disks
around classical T Tauri stars. Water emission is not detected in the
transitional disks SR 24 N and SR 24 S, in spite of SR 24 S having
pre-transitional disk properties like DoAr 44, which does show water emission
(Salyk et al. 2015). With R~100,000, the TEXES water spectra have the highest
spectral resolution possible at this time, and allow for detailed lineshape
analysis. We find that the mid-IR water emission lines are similar to the
"narrow component" in CO rovibrational emission (Banzatti & Pontoppidan 2015),
consistent with disk radii of a few AU. The emission lines are either single
peaked, or consistent with a double peak. Single-peaked emission lines cannot
be produced with a Keplerian disk model, and may suggest that water
participates in the disk winds proposed to explain single-peaked CO emission
lines (Bast et al. 2011, Pontoppidan et al. 2011). Double-peaked emission lines
can be used to determine the radius at which the line emission luminosity drops
off. For HL Tau, the lower limit on this measured dropoff radius is consistent
with the 13 AU dark ring (ALMA partnership et al. 2015). We also report
variable line/continuum ratios from the disks around DR Tau and RW Aur, which
we attribute to continuum changes and line flux changes, respectively. The
reduction in RW Aur line flux corresponds with an observed dimming at visible
wavelengths (Rodriguez et al. 2013).Comment: To appear in the Astrophysical Journa
Modelling the Fluid Mechanics of Cilia and Flagella in Reproduction and Development
Cilia and flagella are actively bending slender organelles, performing
functions such as motility, feeding and embryonic symmetry breaking. We review
the mechanics of viscous-dominated microscale flow, including time-reversal
symmetry, drag anisotropy of slender bodies, and wall effects. We focus on the
fundamental force singularity, higher order multipoles, and the method of
images, providing physical insight and forming a basis for computational
approaches. Two biological problems are then considered in more detail: (1)
left-right symmetry breaking flow in the node, a microscopic structure in
developing vertebrate embryos, and (2) motility of microswimmers through
non-Newtonian fluids. Our model of the embryonic node reveals how particle
transport associated with morphogenesis is modulated by the gradual emergence
of cilium posterior tilt. Our model of swimming makes use of force
distributions within a body-conforming finite element framework, allowing the
solution of nonlinear inertialess Carreau flow. We find that a three-sphere
model swimmer and a model sperm are similarly affected by shear-thinning; in
both cases swimming due to a prescribed beat is enhanced by shear-thinning,
with optimal Deborah number around 0.8. The sperm exhibits an almost perfect
linear relationship between velocity and the logarithm of the ratio of zero to
infinite shear viscosity, with shear-thickening hindering cell progress.Comment: 20 pages, 24 figure
Detection of Water Vapor in the Thermal Spectrum of the Non-Transiting Hot Jupiter upsilon Andromedae b
The upsilon Andromedae system was the first multi-planet system discovered
orbiting a main sequence star. We describe the detection of water vapor in the
atmosphere of the innermost non-transiting gas giant ups~And~b by treating the
star-planet system as a spectroscopic binary with high-resolution, ground-based
spectroscopy. We resolve the signal of the planet's motion and break the
mass-inclination degeneracy for this non-transiting planet via deep combined
flux observations of the star and the planet. In total, seven epochs of Keck
NIRSPEC band observations, three epochs of Keck NIRSPEC short wavelength
band observations, and three epochs of Keck NIRSPEC long wavelength
band observations of the ups~And~system were obtained. We perform a multi-epoch
cross correlation of the full data set with an atmospheric model. We measure
the radial projection of the Keplerian velocity ( = 55 9 km/s), true
mass ( = 1.7 ), and orbital inclination \big(
= 24 4\big), and determine that the planet's opacity structure
is dominated by water vapor at the probed wavelengths. Dynamical simulations of
the planets in the ups~And~system with these orbital elements for ups~And~b
show that stable, long-term (100 Myr) orbital configurations exist. These
measurements will inform future studies of the stability and evolution of the
ups~And~system, as well as the atmospheric structure and composition of the hot
Jupiter.Comment: Accepted to A
Granulicatella adiacens, an unusual causative agent in chronic dacryocystitis
West Virginia Universit
Neural Field Models: A mathematical overview and unifying framework
Rhythmic electrical activity in the brain emerges from regular non-trivial
interactions between millions of neurons. Neurons are intricate cellular
structures that transmit excitatory (or inhibitory) signals to other neurons,
often non-locally, depending on the graded input from other neurons. Often this
requires extensive detail to model mathematically, which poses several issues
in modelling large systems beyond clusters of neurons, such as the whole brain.
Approaching large populations of neurons with interconnected constituent
single-neuron models results in an accumulation of exponentially many
complexities, rendering a realistic simulation that does not permit
mathematical tractability and obfuscates the primary interactions required for
emergent electrodynamical patterns in brain rhythms. A statistical mechanics
approach with non-local interactions may circumvent these issues while
maintaining mathematically tractability. Neural field theory is a
population-level approach to modelling large sections of neural tissue based on
these principles. Herein we provide a review of key stages of the history and
development of neural field theory and contemporary uses of this branch of
mathematical neuroscience. We elucidate a mathematical framework in which
neural field models can be derived, highlighting the many significant inherited
assumptions that exist in the current literature, so that their validity may be
considered in light of further developments in both mathematical and
experimental neuroscience.Comment: 55 pages, 10 figures, 2 table
Ground- and Space-based Detection of the Thermal Emission Spectrum of the Transiting Hot Jupiter KELT-2Ab
We describe the detection of water vapor in the atmosphere of the transiting
hot Jupiter KELT-2Ab by treating the star-planet system as a spectroscopic
binary with high-resolution, ground-based spectroscopy. We resolve the signal
of the planet's motion with deep combined flux observations of the star and the
planet. In total, six epochs of Keck NIRSPEC -band observations were
obtained, and the full data set was subjected to a cross correlation analysis
with a grid of self-consistent atmospheric models. We measure a radial
projection of the Keplerian velocity, , of 148 7 km s,
consistent with transit measurements, and detect water vapor at 3.8. We
combine NIRSPEC -band data with IRAC secondary eclipse data to
further probe the metallicity and carbon-to-oxygen ratio of KELT-2Ab's
atmosphere. While the NIRSPEC analysis provides few extra constraints on the
data, it does provide roughly the same constraints on metallicity and
carbon-to-oxygen ratio. This bodes well for future investigations of the
atmospheres of non-transiting hot Jupiters.Comment: accepted to A
Evidence for the Direct Detection of the Thermal Spectrum of the Non-Transiting Hot Gas Giant HD 88133 b
We target the thermal emission spectrum of the non-transiting gas giant HD
88133 b with high-resolution near-infrared spectroscopy, by treating the planet
and its host star as a spectroscopic binary. For sufficiently deep summed flux
observations of the star and planet across multiple epochs, it is possible to
resolve the signal of the hot gas giant's atmosphere compared to the brighter
stellar spectrum, at a level consistent with the aggregate shot noise of the
full data set. To do this, we first perform a principal component analysis to
remove the contribution of the Earth's atmosphere to the observed spectra.
Then, we use a cross-correlation analysis to tease out the spectra of the host
star and HD 88133 b to determine its orbit and identify key sources of
atmospheric opacity. In total, six epochs of Keck NIRSPEC L band observations
and three epochs of Keck NIRSPEC K band observations of the HD 88133 system
were obtained. Based on an analysis of the maximum likelihood curves calculated
from the multi-epoch cross correlation of the full data set with two
atmospheric models, we report the direct detection of the emission spectrum of
the non-transiting exoplanet HD 88133 b and measure a radial projection of the
Keplerian orbital velocity of 40 15 km/s, a true mass of
1.02, a nearly face-on orbital inclination of
15, and an atmosphere opacity structure at high
dispersion dominated by water vapor. This, combined with eleven years of radial
velocity measurements of the system, provides the most up-to-date ephemeris for
HD 88133.Comment: 9 pages, 6 figures; accepted for publication in Ap
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