1,996 research outputs found
Investigating the Structure of Paramagnetic Aggregates from Colloidal Emulsions - 2
Particle dynamics of magnetorheological fluids (fluids that change properties in response to magnetic fields) are studied to help understand adaptable new fluids for use in such applications as brake systems and robotics
Colloidal diffusion and hydrodynamic screening near boundaries
The hydrodynamic interactions between colloidal particles in small ensembles are measured at varying distances from a no-slip surface over a range of inter-particle separations. The diffusion tensor for motion parallel to the wall of each ensemble is calculated by analyzing thousands of particle trajectories generated by blinking holographic optical tweezers and by dynamic simulation. The Stokesian
Dynamics simulations predict similar particle dynamics. By separating the dynamics into three classes of modes: self, relative and collective diffusion, we observe qualitatively different behavior depending on the relative magnitudes of the distance of the ensemble from the wall and the inter-particle separation. A simple picture of the pair-hydrodynamic interactions is developed, while many-body-hydrodynamic interactions give rise to more complicated behavior. The results demonstrate that the
effect of many-body hydrodynamic interactions in the presence of a wall is much richer than the single
particle behavior and that the multiple-particle behavior cannot be simply predicted by a superposition of pair interactions
On Algorithmic Statistics for space-bounded algorithms
Algorithmic statistics studies explanations of observed data that are good in
the algorithmic sense: an explanation should be simple i.e. should have small
Kolmogorov complexity and capture all the algorithmically discoverable
regularities in the data. However this idea can not be used in practice because
Kolmogorov complexity is not computable.
In this paper we develop algorithmic statistics using space-bounded
Kolmogorov complexity. We prove an analogue of one of the main result of
`classic' algorithmic statistics (about the connection between optimality and
randomness deficiences). The main tool of our proof is the Nisan-Wigderson
generator.Comment: accepted to CSR 2017 conferenc
High resolution radio imaging of the two Particle-Accelerating Colliding-Wind Binaries HD167971 and HD168112
The colliding-wind region in binary systems made of massive stars allows us
to investigate various aspects of shock physics, including particle
acceleration. Particle accelerators of this kind are tagged as
Particle-Accelerating Colliding-Wind Binaries, and are mainly identified thanks
to their synchrotron radio emission. Our objective is first to validate the
idea that obtaining snapshot high-resolution radio images of massive binaries
constitutes a relevant approach to unambiguously identify particle
accelerators. Second, we intend to exploit these images to characterize the
synchrotron emission of two specific targets, HD167971 and HD168112, known as
particle accelerators. We traced the radio emission from the two targets at 1.6
GHz with the European Very Long Baseline Interferometry Network, with an
angular resolution of a few milli-arcseconds. Our measurements allowed us to
obtain images for both targets. For HD167971, our observation occurs close to
apastron, at an orbital phase where the synchrotron emission is minimum. For
HD168112, we resolved for the very first time the synchrotron emission region.
The emission region appears slightly elongated, in agreement with expectation
for a colliding-wind region. In both cases the measured emission is
significantly stronger than the expected thermal emission from the stellar
winds, lending strong support for a non-thermal nature. Our study brings a
significant contribution to the still poorly addressed question of high angular
resolution radio imaging of colliding-wind binaries. We show that snapshot Very
Long Baseline Interferometry measurements constitute an efficient approach to
investigate these objects, with promising results in terms of identification of
additional particle accelerators, on top of being promising as well to reveal
long period binaries.Comment: 8 pages, 1 figure, accepted for publication in A&
An upper limit on anomalous dust emission at 31 GHz in the diffuse cloud [LPH96]201.663+1.643
[LPH96]201.663+1.643, a diffuse H{\sc ii} region, has been reported to be a
candidate for emission from rapidly spinning dust grains. Here we present
Cosmic Background Imager (CBI) observations at 26-36 GHz that show no evidence
for significant anomalous emission. The spectral index within the CBI band, and
between CBI and Effelsberg data at 1.4/2.7 GHz, is consistent with optically
thin free-free emission. The best-fitting temperature spectral index from 2.7
to 31 GHz, , is close to the theoretical value,
for K. We place an upper limit of 24% ~ (2\sigma)
for excess emission at 31 GHz as seen in a 6\arcmin FWHM beam. Current
spinning dust models are not a good fit to the spectrum of LPH96. No polarized
emission is detected in the CBI data with an upper limit of 2% on the
polarization fraction.Comment: 5 pages, 3 figures, submitted to ApJ
On the Enhanced Interstellar Scattering Toward B1849+005
(Abridged) This paper reports new Very Large Array (VLA) and Very Long
Baseline Array (VLBA) observations of the extragalactic source B1849+005 at
frequencies between 0.33 and 15 GHz and the re-analysis of archival VLA
observations at 0.33, 1.5, and 4.9 GHz. The structure of this source is complex
but interstellar scattering dominates the structure of the central component at
least to 15 GHz. An analysis of the phase structure functions of the
interferometric visibilities shows the density fluctuations along this line of
sight to be anisotropic (axial ratio = 1.3) with a frequency-independent
position angle, and having an inner scale of roughly a few hundred kilometers.
The anisotropies occur on length scales of order 10^{15} cm (D/5 kpc), which
within the context of certain magnetohydrodynamic turbulence theories indicates
the length scale on which the kinetic and magnetic energy densities are
comparable. A conservative upper limit on the velocity of the scattering
material is 1800 km/s. In the 0.33 GHz field of view, there are a number of
other sources that might also be heavily scattered. Both B1849+005 and PSR
B1849+00 are highly scattered, and they are separated by only 13'. If the lines
of sight are affected by the same ``clump'' of scattering material, it must be
at least 2.3 kpc distant. However, a detailed attempt to account for the
scattering observables toward these sources does not produce a self-consistent
set of parameters for such a clump. A clump of H\alpha emission, possibly
associated with the H II region G33.418-0.004, lies between these two lines of
sight, but it seems unable to account for all of the required excess
scattering.Comment: 23 pages, LaTeX2e AASTeX, 13 figures in 14 PostScript files, accepted
for publication in Ap
- …