42,143 research outputs found
Atmospheric turbulence and superstatistics
Nonequilibrium systems with large-scale fluctuations of a suitable system
parameter are often effectively described by a superposition of two statistics,
a superstatistics. Here we illustrate this concept by analysing experimental
data of fluctuations in atmospheric wind velocity differences at Florence
airport.Comment: 9 pages, 4 figures. New version to appear in Europhysics News (2005
Transport in ultradilute solutions of He in superfluid He
We calculate the effect of a heat current on transporting He dissolved in
superfluid He at ultralow concentration, as will be utilized in a proposed
experimental search for the electric dipole moment of the neutron (nEDM). In
this experiment, a phonon wind will generated to drive (partly depolarized)
He down a long pipe. In the regime of He concentrations and temperatures K, the phonons comprising the heat current
are kept in a flowing local equilibrium by small angle phonon-phonon
scattering, while they transfer momentum to the walls via the He first
viscosity. On the other hand, the phonon wind drives the He out of local
equilibrium via phonon-He scattering. For temperatures below K, both
the phonon and He mean free paths can reach the centimeter scale, and we
calculate the effects on the transport coefficients. We derive the relevant
transport coefficients, the phonon thermal conductivity and the He
diffusion constants from the Boltzmann equation. We calculate the effect of
scattering from the walls of the pipe and show that it may be characterized by
the average distance from points inside the pipe to the walls. The temporal
evolution of the spatial distribution of the He atoms is determined by the
time dependent He diffusion equation, which describes the competition
between advection by the phonon wind and He diffusion. As a consequence of
the thermal diffusivity being small compared with the He diffusivity, the
scale height of the final He distribution is much smaller than that of the
temperature gradient. We present exact solutions of the time dependent
temperature and He distributions in terms of a complete set of normal
modes.Comment: NORDITA PREPRINT 2015-37, 9 pages, 6 figure
Transport in very dilute solutions of He in superfluid He
Motivated by a proposed experimental search for the electric dipole moment of
the neutron (nEDM) utilizing neutron-He capture in a dilute solution of
He in superfluid He, we derive the transport properties of dilute
solutions in the regime where the He are classically distributed and rapid
He-He scatterings keep the He in equilibrium. Our microscopic
framework takes into account phonon-phonon, phonon-He, and He-He
scatterings. We then apply these calculations to measurements by Rosenbaum et
al. [J.Low Temp.Phys. {\bf 16}, 131 (1974)] and by Lamoreaux et al.
[Europhys.Lett. {\bf 58}, 718 (2002)] of dilute solutions in the presence of a
heat flow. We find satisfactory agreement of theory with the data, serving to
confirm our understanding of the microscopics of the helium in the future nEDM
experiment.Comment: 10 pages, 5 figures, v
Low Temperature Transport Properties of Very Dilute Classical Solutions of He in Superfluid He
We report microscopic calculations of the thermal conductivity, diffusion
constant and thermal diffusion constant for classical solutions of He in
superfluid He at temperatures T \la 0.6~K, where phonons are the dominant
excitations of the He. We focus on solutions with He concentrations
\la \,10^{-3}, for which the main scattering mechanisms are phonon-phonon
scattering via 3-phonon Landau and Beliaev processes, which maintain the
phonons in a drifting equilibrium distribution, and the slower process of
He-phonon scattering, which is crucial for determining the He
distribution function in transport. We use the fact that the relative changes
in the energy and momentum of a He atom in a collision with a phonon are
small to derive a Fokker-Planck equation for the He distribution function,
which we show has an analytical solution in terms of Sonine polynomials. We
also calculate the corrections to the Fokker-Planck results for the transport
coefficients.Comment: 29 pages, 2 figure
Spectroscopy at the solar limb: II. Are spicules heated to coronal temperatures ?
Spicules of the so-called type II were suggested to be relevant for coronal
heating because of their ubiquity on the solar surface and their eventual
extension into the corona. We investigate whether solar spicules are heated to
transition-region or coronal temperatures and reach coronal heights (>6 Mm)
using multi-wavelength observations of limb spicules in different chromospheric
spectral lines (Ca II H, Hepsilon, Halpha, Ca II IR at 854.2 nm, He I at 1083
nm). We determine the line width of individual spicules and throughout the
field of view and estimate the maximal height that different types of off-limb
features reach. We derive estimates of the kinetic temperature and the
non-thermal velocity from the line width of spectral lines from different
chemical elements. We find that most regular spicules reach a maximal height of
about 6 Mm above the solar limb. The majority of features found at larger
heights are irregularly shaped with a significantly larger lateral extension
than spicules. Both individual and average line profiles in all spectral lines
show a decrease in their line width with height above the limb with very few
exceptions. Both the kinetic temperature and the non-thermal velocity decrease
with height above the limb. We find no indications that the spicules in our
data reach coronal heights or transition-region or coronal temperatures.Comment: Accepted for publication in Solar Physics, 52 pages, 32 figure
The Infrared Nucleus of the Wolf-Rayet Galaxy Henize 2-10
We have obtained near-infrared images and mid-infrared spectra of the
starburst core of the dwarf Wolf-Rayet galaxy He 2-10. We find that the
infrared continuum and emission lines are concentrated in a flattened ellipse
3-4'' or 150 pc across which may show where a recent accretion event has
triggered intense star formation. The ionizing radiation from this cluster has
an effective temperature of 40,000 K, corresponding to stars, and
the starburst is years old.Comment: 17 pages Latex, 7 postscript figures, 1 postscript table, accepted to
A
The polarization signature of photospheric magnetic fields in 3D MHD simulations and observations at disk center
Before using 3D MHD simulations of the solar photosphere in the determination
of elemental abundances, one has to ensure that the correct amount of magnetic
flux is present in the simulations. The presence of magnetic flux modifies the
thermal structure of the solar photosphere, which affects abundance
determinations and the solar spectral irradiance. We compare the polarization
signals in disk-center observations of the solar photosphere in quiet-Sun
regions with those in Stokes spectra computed on the basis of 3D MHD
simulations having average magnetic flux densities of about 20, 56, 112 and 224
G. This approach allows us to find the simulation run that best matches the
observations. The observations were taken with the Hinode SP, TIP, POLIS and
the GFPI, respectively. We determine characteristic quantities of full Stokes
profiles in a few photospheric spectral lines in the visible (630 nm) and
near-infrared (1083 and 1565 nm). We find that the appearance of abnormal
granulation in intensity maps of degraded simulations can be traced back to an
initially regular granulation pattern with numerous bright points in the
intergranular lanes before the spatial degradation. The linear polarization
signals in the simulations are almost exclusively related to canopies of strong
magnetic flux concentrations and not to transient events of magnetic flux
emergence. We find that the average vertical magnetic flux density in the
simulation should be less than 50 G to reproduce the observed polarization
signals in the quiet Sun internetwork. A value of about 35 G gives the best
match across the SP, TIP, POLIS and GFPI observations.Comment: 12 pages, 11 figures; accepted for publication in Ap
Aphidophagous Coccinellids in Alfalfa, Small Grains, and Maize in Eastern South Dakota
In a 13-year study of aphidophagous coccinellids associated with alfalfa (Medicago sativa), maize (Zea mays), and small grain crops in eastern South Dakota, the following species were consistently associated with the crops: Hippodamia convergens, H. tredecimpunctata tibialis, H. parenthesis, Coleomegilla maculata lengi, Coccinella transversoguttata richardsoni, Cycloneda munda, and Adalia bipunctata. All species except A. bipunctata were associated with each of the three crops, while A. bipunctata occurred only in maize. Relative abundances of each species varied among crops and among years. Although only seven species were associated with the crops, additional species were captured on sticky traps stationed adjacent to sampled fields. The species diversity of immature coccinellids did not differ among crops but did differ among years. The diversity of adults differed among crops and years. The site from which samples were taken had no influence on the diversity of immatures or adults. Species relative abundances in alfalfa and small grains were more similar to each other than they were to relative abundances in maize
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