2,328 research outputs found
Ni-impurity effects on the superconducting gap of LaSrCuO studied from the magnetic field and temperature dependence of the electronic specific heat
The magnetic field and temperature dependence of the electronic specific heat
have been systematically investigated in (LSCNO) in order to study Ni-impurity
effects on the superconducting (SC) gap. In LSCNO with =0.15 and =0.015,
the value of () at =0 K, , is
enhanced under the magnetic field applied along the -axis. The
increment of , , follows the Volovik relation
=, characteristic of the SC gap with line nodes,
with prefactor similar to that of a pure sample. The vs.
curve under =0 shows a d-wave-like SC anomaly with an abrupt increase at
and -linear dependence at , although the
-value in the vs. curve increases with increasing
Ni concentrations. Interestingly, as the SC part of , , decreases in LSCNO, is
reduced in proportion to the decrease of . These findings can
be explained phenomenologically by a simple model in which Ni impurities bring
about strong pair breaking at the edges of the coherent nodal part of the Fermi
surface but in the vicinity of the nodes of the SC gap. The reduction of the SC
condensation energy in LSCNO, evaluated from at
{0.3em}\raisebox{0.4ex}{} {-0.75em}\raisebox{-.7ex}{} {0.3em}, is also understood by the same model.Comment: 7 pages, 6 figures, accepted in Phys. Rev.
Differences in bird communities on the forest edge and in the forest interior: Are there forest-interior specialists in Japan?
Most North American bird species that are less successful in small forests than in large forests, are forest-interior specialists that winter in the tropics. These species have declined in small forests because of high rates of nest predation and brood parasitism near the forest edge. To determine whether migratory forest-interior specialists are also important components of bird communities in Japan, we surveyed bird populations on plots at the edge and in the interior of deciduous forests in Hokkaido and Kyoto. Surveys were conducted during the breeding season in forest fragments using the point count method. We calculated edge indices for the most abundant species in Hokkaido and Kyoto (38 and 18 species, respectively). Among the nine species that were more abundant in interior than in edge plots in Hokkaido were the following tropical migrants: Turdus cardis, Phylloscopus coronatus, and Cuculus saturatus. In Kyoto, the abundance of particular species of tropical migrants was too low to permit statistical analysis. We therefore analyzed the rare species as a group and this group was more abundant in the forest interior than on the forest edge. Three resident species, Garrulus glandrius, Picus awokera, and Bambusicola thoracica, were also more abundant in the forest interior. The most frequent potential nest predator, Corvus macrorhynchos, was more abundant at the edge than in the interior in Hokkaido, but showed the reverse pattern in Kyoto. The abundance of the most frequent brood parasite in Hokkaido, Cuculus saturatus, had a weak positive relation with the abundance of its host species, but was not significantly related to the distance from the forest edge. Therefore, the major negative edge effects in Japan may be due to nest predation by corvids. The impact of negative edge effects, as well as the effect of forest structure, on forest-interior birds in Japan should be the focus of future research
Dynamics of Rotating Accretion Flows Irradiated by a Quasar
We study the axisymmetric, time-dependent hydrodynamics of rotating flows
that are under the influence of supermassive black hole gravity and radiation
from an accretion disk surrounding the black hole. This work is an extension of
the earlier work presented by Proga, where nonrotating flows were studied.
Here, we consider effects of rotation, a position-dependent radiation
temperature, density at large radii, and uniform X-ray background radiation. As
in the non-rotating case, the rotating flow settles into a configuration with
two components (1) an equatorial inflow and (2) a bipolar inflow/outflow with
the outflow leaving the system along the pole. However, with rotation the flow
does not always reach a steady state. In addition, rotation reduces the outflow
collimation and the outward flux of mass and kinetic energy. Moreover rotation
increases the outward flux of the thermal energy and can lead to fragmentation
and time-variability of the outflow. We also show that a position-dependent
radiation temperature can significantly change the flow solution. In
particular, the inflow in the equatorial region can be replaced by a thermally
driven outflow. Generally, as it have been discussed and shown in the past, we
find that self-consistently determined preheating/cooling from the quasar
radiation can significantly reduce the rate at which the central BH is fed with
matter. However, our results emphasize also a little appreciated feature.
Namely, quasar radiation drives a non-spherical, multi-temperature and very
dynamic flow. These effects become dominant for luminosities in excess of 0.01
of the Eddington luminosity.Comment: accepted for publication in Ap
Accretion dynamics in the classical T Tauri star V2129 Oph
We analyze the photometric and spectroscopic variability of the classical T
Tauri star V2129 Oph over several rotational cycles to test the dynamical
predictions of magnetospheric accretion models. The photometric variability and
the radial velocity variations in the photospheric lines can be explained by
rotational modulation due to cold spots, while the radial velocity variations
of the He I (5876 \AA) line and the veiling variability are due to hot spot
rotational modulation. The hot and cold spots are located at high latitudes and
about the same phase, but the hot spot is expected to sit at the chromospheric
level, while the cold spot is at the photospheric level. Using the
dipole+octupole magnetic-field configuration previously proposed in the
literature for the system, we compute 3D MHD magnetospheric simulations of the
star-disk system. We use the simulation's density, velocity and scaled
temperature structures as input to a radiative transfer code, from which we
calculate theoretical line profiles at all rotational phases. The theoretical
profiles tend to be narrower than the observed ones, but the qualitative
behavior and the observed rotational modulation of the H\alpha and H\beta
emission lines are well reproduced by the theoretical profiles. The
spectroscopic and photometric variability observed in V2129 Oph support the
general predictions of complex magnetospheric accretion models with
non-axisymmetric, multipolar fields.Comment: Accepted by Astronomy and Astrophysic
MHD Simulations of Magnetospheric Accretion, Ejection and Plasma-field Interaction
We review recent axisymmetric and three-dimensional (3D) magnetohydrodynamic
(MHD) numerical simulations of magnetospheric accretion, plasma-field
interaction and outflows from the disk-magnetosphere boundary.Comment: 11 pages, 8 figures, conference proceedings: "Physics at the
Magnetospheric Boundary", Geneva, Switzerland, 25-28 June, 201
Modelling circumstellar discs with 3D radiation hydrodynamics
We present results from combining a grid-based radiative transfer code with a
Smoothed Particle Hydrodynamics code to produce a flexible system for modelling
radiation hydrodynamics. We use a benchmark model of a circumstellar disc to
determine a robust method for constructing a gridded density distribution from
SPH particles. The benchmark disc is then used to determine the accuracy of the
radiative transfer results. We find that the SED and the temperature
distribution within the disc are sensitive to the representation of the disc
inner edge, which depends critically on both the grid and SPH resolution. The
code is then used to model a circumstellar disc around a T-Tauri star. As the
disc adjusts towards equilibrium vertical motions in the disc are induced
resulting in scale height enhancements which intercept radiation from the
central star. Vertical transport of radiation enables these perturbations to
influence the mid-plane temperature of the disc. The vertical motions decay
over time and the disc ultimately reaches a state of simultaneous hydrostatic
and radiative equilibrium.Comment: MNRAS accepted; 15 pages; 17 figures, 4 in colou
Facing the wind of the pre-FUor V1331 Cyg
The mass outflows in T Tauri stars (TTS) are thought to be an effective
mechanism to remove angular momentum during the pre-main-sequence contraction
of a low-mass star. The most powerful winds are observed at the FUor stage of
stellar evolution. V1331 Cyg has been considered as a TTS at the pre-FUor
stage. We analyse high-resolution spectra of V1331 Cyg collected in 1998-2007
and 20-d series of spectra taken in 2012. For the first time the photospheric
spectrum of the star is detected and stellar parameters are derived: spectral
type G7-K0 IV, mass 2.8 Msun, radius 5 Rsun, vsini < 6 km/s. The photospheric
spectrum is highly veiled, but the amount of veiling is not the same in
different spectral lines, being lower in weak transitions and much higher in
strong transitions. The Fe II 5018, Mg I 5183, K I 7699 and some other lines of
metals are accompanied by a `shell' absorption at radial velocity of about -240
km/s. We show that these absorptions form in the post-shock gas in the jet,
i.e. the star is seen though its jet. The P Cyg profiles of H-alpha and H-beta
indicate the terminal wind velocity of about 500 km/s, which vary on
time-scales from several days to years. A model of the stellar wind is
developed to interpret the observations. The model is based on calculation of
hydrogen spectral lines using the radiative transfer code TORUS. The observed
H-alpha and H-beta line profiles and their variability can be well reproduced
with a stellar wind model, where the mass-loss rate and collimation (opening
angle) of the wind are variable. The changes of the opening angle may be
induced by small variability in magetization of the inner disc wind. The
mass-loss rate is found to vary within (6-11)x10^{-8} Msun/yr, with the
accretion rate of 2.0x10^{-6} Msun/yr.Comment: 11 pages, 12 figures; accepted for publication in MNRAS.
Typographical errors have been corrected after the proof stag
Ambulatory electrocardiographic evaluation of the occurrence of arrhythmias in healthy Salukis
Phylogenetic relationships of three hymenolepidid species inferred from nuclear ribosomal and mitochondrial DNA sequences
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