830 research outputs found
Evidence of grain growth in the disk of the bipolar proto-planetary nebula M 1--92
We investigate the dust size and dust shell structure of the bipolar
proto-planetary nebula M 1--92 by means of radiative transfer modeling. Our
models consists of a disk and bipolar lobes that are surrounded by an AGB
shell, each component having different dust characteristics. The upper limit of
the grain size in the lobes is estimated to be m from
the polarization value in the bipolar lobe. The value of the
disk is constrained with the disk mass (0.2 M_{\sun}), which was estimated
from a previous CO emission line observation. We find a good model with
m, which provides an approximated disk mass of 0.15
M_{\sun}. Even taking into account uncertainties such as the gas-to-dust mass
ratio, a significantly larger dust of m, comparing to
the dust in the lobe, is expected.
We also estimated the disk inner radius, the disk outer radius, and the
envelope mass to be 30 (=9 AU), 4500 AU, and 4 M_{\sun},
respectively, where is the expansion velocity. If the dust
existing in the lobes in large separations from the central star undergoes
little dust processing, the dust sizes preserves the ones in the dust
formation. Submicron-sized grains are found in many objects besides M 1--92,
suggesting that the size does not depend much on the object properties, such as
initial mass of the central star and chemical composition of the stellar
system. On the other hand, the grain sizes in the disk do. Evidence of large
grains has been reported in many bipolar PPNs, including M 1--92. This result
suggests that disks play an important role in grain growth.Comment: 8 pages with 3 figures. Accepted for publication in A&
Assembling strategies in extrinsic evolvable hardware with bi-directional incremental evolution
Bidirectional incremental evolution (BIE) has been proposed as a technique to overcome the ”stalling” effect in evolvable hardware applications. However preliminary results show perceptible dependence of performance of BIE and quality of evaluated circuit on assembling strategy applied during reverse stage of incremental evolution. The purpose of this paper is to develop assembling strategy that will assist BIE to produce relatively optimal solution with minimal computational effort (e.g. the minimal number of generations)
Mechanisms of enhanced orbital dia- and paramagnetism: Application to the Rashba semiconductor BiTeI
We study the magnetic susceptibility of a layered semiconductor BiTeI with
giant Rashba spin splitting both theoretically and experimentally to explore
its orbital magnetism. Apart from the core contributions, a large
temperature-dependent diamagnetic susceptibility is observed when the Fermi
energy E_F is near the crossing point of the conduction bands, while the
susceptibility turns to be paramagnetic when E_F is away from it. These
features are consistent with first-principles calculations, which also predict
an enhanced orbital magnetic susceptibility with both positive and negative
signs as a function of E_F due to band (anti)crossings. Based on these
observations, we propose two mechanisms for an enhanced paramagnetic orbital
susceptibility.Comment: 4 figures; added reference
Near-infrared integral field spectroscopy of Massive Young Stellar Objects
We present medium resolution () -band integral field
spectroscopy of six MYSOs. The targets are selected from the RMS survey, and we
used the NIFS on the Gemini North telescope. The data show various spectral
line features including Br, CO, H, and \mbox{He\,{\sc i}}. The
Br line is detected in emission in all objects with
-- 200 kms. V645 Cyg shows a high-velocity
P-Cygni profile between -800 kms and -300 kms. We performed
three-dimensional spectroastrometry to diagnose the circumstellar environment
in the vicinity of the central stars using the Br line. We measured the
centroids of the velocity components with sub-mas precision. The centroids
allow us to discriminate the blueshifted and redshifted components in a roughly
east--west direction in both IRAS 18151--1208 and S106 in Br. This lies
almost perpendicular to observed larger scale outflows. We conclude, given the
widths of the lines and the orientation of the spectroastrometric signature,
that our results trace a disc wind in both IRAS 18151--1208 and S106. The CO
absorption lines at low transitions are detected in IRAS
18151--1208 and AFGL 2136. We analysed the velocity structure of the neutral
gas discs. In IRAS 18151--1208, the absorption centroids of the blueshifted and
redshifted components are separated in a direction of north-east to south-west,
nearly perpendicular to that of the larger scale jet. The
position-velocity relations of these objects can be reproduced with central
masses of 30 M_{\sun} for IRAS 18151--1208 and 20 M_{\sun} for AFGL 2136.
We also detect CO bandhead emission in IRAS 18151--1208, S106 and
V645 Cyg. The results can be fitted reasonably with a Keplerian rotation model,
with masses of 15, 20 and 20 M_{\sun} respectively.Comment: 17 pages, 10 figures, accepted by MNRA
Dynamics of Multiferroic Domain Wall in Spin-Cycloidal Ferroelectric DyMnO
We report the dielectric dispersion of the giant magnetocapacitance (GMC) in
multiferroic DyMnO over a wide frequency range. The GMC is found to be
attributable not to the softened electromagnon but to the electric-field-driven
motion of multiferroic domain wall (DW). In contrast to conventional
ferroelectric DWs, the present multiferroic DW motion holds extremely high
relaxation rate of s even at low temperatures. This
mobile nature as well as the model simulation suggests that the multiferroic DW
is not atomically thin as in ferroelectrics but thick, reflecting its magnetic
origin.Comment: 4 pages, 4 figure
The Water-ice Feature in Near-infrared Disk-scattered Light around HD 142527:Micron-sized Icy Grains Lifted up to the Disk Surface?
We study the m scattering feature of water ice detected in the outer
disk of HD 142527 by performing radiative transfer simulations. We show that an
ice mass abundance at the outer disk surface of HD 142527 is much lower than
estimated in a previous study. It is even lower than inferred from far-infrared
ice observations, implying ice disruption at the disk surface. Next, we
demonstrate that a polarization fraction of disk-scattered light varies across
the ice-band wavelengths depending on ice grain properties; hence, polarimetric
spectra would be another tool for characterizing water-ice properties. Finally,
we argue that the observed reddish disk-scattered light is due to grains with a
few microns in size. To explain the presence of such grains at the disk
surface, we need a mechanism that can efficiently oppose dust settling. If we
assume turbulent mixing, our estimate requires ,
where is a non-dimensional parameter describing the vertical diffusion
coefficient of grains. Future observations probing gas kinematics would be
helpful to elucidate vertical grain dynamics in the outer disk of HD 142527.Comment: 21 pages, 14 figures, 1 table; Accepted for publication in Ap
Interplay of Spin-Orbit Interaction and Electron Correlation on the Van Vleck Susceptibility in Transition Metal Compounds
We have studied the effects of electron correlation on Van Vleck
susceptibility () in transition metal compounds. A typical
crossover behavior is found for the correlation effect on as
sweeping spin-orbit interaction, . For a small , orbital
fluctuation plays a dominant role in the correlation enhancement of
; however, the enhancement rate is rather small. In contrast,
for an intermediate , shows a substantial increase,
accompanied by the development of spin fluctuation. We will discuss the
behavior of in association with the results of Knight-shift
experiments on SrRuO and an anomalously large magnetic susceptibility
observed for Ir compounds.Comment: 5 pages, 3 figures, to appear in J. Phys. Soc. Jp
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