25,894 research outputs found
A precessing jet model for the PN K 3-35: simulated radio-continuum emission
The bipolar morphology of the planetary nebula (PN) K 3-35 observed in
radio-continuum images was modelled with 3D hydrodynamic simulations with the
adaptive grid code yguazu-a. We find that the observed morphology of this PN
can be reproduced considering a precessing jet evolving in a dense AGB
circumstellar medium, given by a mass loss rate
\dot{M}_{csm}=5x10^{-5}M_{\odot}/yr and a terminal velocity v_{w}=10 km/s.
Synthetic thermal radio-continuum maps were generated from numerical results
for several frequencies. Comparing the maps and the total fluxes obtained from
the simulations with the observational results, we find that a model of
precessing dense jets, where each jet injects material into the surrounding CSM
at a rate \dot{M}_j=2.8x10^{-4} {M_{\odot}/yr (equivalent to a density of
8x10^{4} {cm}^{-3}, a velocity of 1500 km/s, a precession period of 100 yr, and
a semi-aperture precession angle of 20 degrees agrees well with the
observations.Comment: 6 pages, 4 figures, accepted to MNRA
3D MHD Modeling of the Gaseous Structure of the Galaxy: Synthetic Observations
We generated synthetic observations from the four-arm model presented in
Gomez & Cox (2004) for the Galactic ISM in the presence of a spiral
gravitational perturbation. We found that velocity crowding and diffusion have
a strong effect in the l-v diagram. The v-b diagram presents structures at the
expected spiral arm velocities, that can be explained by the off-the-plane
structure of the arms presented in previous papers of this series. Such
structures are observed in the Leiden/Dwingeloo HI survey. The rotation curve,
as measured from the inside of the modeled galaxy, shows similarities with the
observed one for the Milky Way Galaxy, although it has large deviations from
the smooth circular rotation corresponding to the background potential. The
magnetic field inferred from a synthetic synchrotron map shows a largely
circular structure, but with interesting deviations in the midplane due to
distortion of the field from circularity in the interarm regions.Comment: Accepted for publication in ApJ. Better quality figures in
http://www.astro.umd.edu/~gomez/publica/3d_galaxy-3.pd
Path integral approach to no-Coriolis approximation in heavy-ion collisions
We use the two time influence functional method of the path integral approach
in order to reduce the dimension of the coupled-channels equations for
heavy-ion reactions based on the no-Coriolis approximation. Our method is
superior to other methods in that it easily enables us to study the cases where
the initial spin of the colliding particle is not zero. It can also be easily
applied to the cases where the internal degrees of freedom are not necessarily
collective coordinates. We also clarify the underlying assumptions in our
approach.Comment: 11 pages, Latex, Phys. Rev. C in pres
An Early Universe Model with Stiff Matter and a Cosmological Constant
In the present work, we study the quantum cosmology description of a
Friedmann-Robertson-Walker model in the presence of a stiff matter perfect
fluid and a negative cosmological constant. We work in the Schutz's variational
formalism and the spatial sections have constant negative curvature. We
quantize the model and obtain the appropriate Wheeler-DeWitt equation. In this
model the states are bounded therefore we compute the discrete energy spectrum
and the corresponding eigenfunctions. In the present work, we consider only the
negative eigenvalues and their corresponding eigenfunctions. This choice
implies that the energy density of the perfect fluid is negative. A stiff
matter perfect fluid with this property produces a model with a bouncing
solution, at the classical level, free from an initial singularity. After that,
we use the eigenfunctions in order to construct wave packets and evaluate the
time-dependent expectation value of the scale factor. We find that it
oscillates between maximum and minimum values. Since the expectation value of
the scale factor never vanishes, we confirm that this model is free from an
initial singularity, also, at the quantum level.Comment: 12 Pages, 4 Figures. Final version. Accepted for publication in the
Proceedings of the 8th Friedmann Seminar, Rio de Janeiro, 2011. We restricted
our attention to treat the case where the stiff matter has negative energy
eigenvalues, following the referee's suggestio
From weak to strong coupling of localized surface plasmons to guided modes in a luminescent slab
We investigate a periodic array of aluminum nanoantennas embedded in a
light-emitting slab waveguide. By varying the waveguide thickness we
demonstrate the transition from weak to strong coupling between localized
surface plasmons in the nanoantennas and refractive index guided modes in the
waveguide. We experimentally observe a non-trivial relationship between
extinction and emission dispersion diagrams across the weak to strong coupling
transition. These results have implications for a broad class of photonic
structures where sources are embedded within coupled resonators. For
nanoantenna arrays, strong vs. weak coupling leads to drastic modifications of
radiation patterns without modifying the nanoantennas themselves, thereby
representing an unprecedented design strategy for nanoscale light sources
Resolving parameter degeneracies in long-baseline experiments by atmospheric neutrino data
In this work we show that the physics reach of a long-baseline (LBL) neutrino
oscillation experiment based on a superbeam and a megaton water Cherenkov
detector can be significantly increased if the LBL data are combined with data
from atmospheric neutrinos (ATM) provided by the same detector. ATM data are
sensitive to the octant of and to the type of the neutrino mass
hierarchy, mainly through three-flavor effects in e-like events. This allows to
resolve the so-called - and sign()-parameter
degeneracies in LBL data. As a consequence it becomes possible to distinguish
the normal from the inverted neutrino mass ordering at CL from a
combined LBL+ATM analysis if . The potential
to identify the true values of and the CP-phase
is significantly increased through the lifting of the
degeneracies. These claims are supported by a detailed simulation of the T2K
(phase II) LBL experiment combined with a full three-flavor analysis of ATM
data in the HyperKamiokande detector.Comment: 25 pages, 10 figure
H2O Maser Observations of Candidate Post-AGB Stars and Discovery of Three High-velocity Water Sources
We present the results of 22 GHz H_2O maser observations of a sample of 85
post-Asymptotic Giant Branch (post-AGB) candidate stars, selected on the basis
of their OH 1612 MHz maser and far-infrared properties. All sources were
observed with the Tidbinbilla 70-m radio telescope and 21 detections were made.
86 GHz SiO Mopra observations of a subset of the sample are also presented. Of
the 21 H_2O detections, 15 are from sources that are likely to be massive AGB
stars and most of these show typical, regular H_2O maser profiles. In contrast,
nearly all the detections of more evolved stars exhibited high-velocity H_2O
maser emission. Of the five sources seen, v223 (W43A, IRAS 18450-0148) is a
well known `water-fountain' source which belongs to a small group of post-AGB
stars with highly collimated, high-velocity H_2O maser emission. A second
source in our sample, v270 (IRAS 18596+0315), is also known to have
high-velocity emission. We report the discovery of similar emission from a
further three sources, d46 (IRAS 15445-5449), d62 (IRAS 15544-5332) and b292
(IRAS 18043-2116). The source d46 is an evolved post-AGB star with highly
unusual maser properties. The H_2O maser emission from d62 is probably
associated with a massive star. The source b292 is a young post-AGB star that
is highly likely to be a water-fountain source, with masers detected over a
velocity range of 210 km s^{-1}.Comment: 47 pages, 9 figures, 4 tables, accepted by Ap
A survey for water maser emission towards planetary nebulae. New detection in IRAS 17347-3139
We report on a water maser survey towards a sample of 27 planetary nebulae
(PNe) using the Robledo de Chavela and Medicina single-dish antennas, as well
as the Very Large Array (VLA). Two detections have been obtained: the already
known water maser emission in K 3-35, and a new cluster of masers in IRAS
17347-3139. This low rate of detections is compatible with the short life-time
of water molecules in PNe (~100 yr). The water maser cluster at IRAS 17347-3139
are distributed on a ellipse of size ~ 0.2" x 0.1", spatially associated with
compact 1.3 cm continuum emission (simultaneously observed with the VLA). From
archive VLA continuum data at 4.9, 8.4, and 14.9 GHz, a spectral index alpha =
0.76 +- 0.03 is derived for this radio source, which is consistent with either
a partially optically thick ionized region or with an ionized wind. However,
the latter scenario can be ruled out on mass-loss considerations, thus
indicating that this source is probably a young PN. The spatial distribution
and the radial velocities of the water masers are suggestive of a rotating and
expanding maser ring, tracing the innermost regions of a torus formed at the
end of the AGB phase. Given that the 1.3 cm continuum emission peak is located
near one of the tips of the major axis of the ellipse of masers, we speculate
on a possible binary nature of IRAS 17347-3139, where the radio continuum
emission could belong to one of the components and the water masers would be
associated with a companion.Comment: Accepted by The Astrophysical Journal. 25 pages, 6 figure
OH 12.8-0.9: A New Water-Fountain Source
We present observational evidence that the OH/IR star OH 12.8-0.9 is the
fourth in a class of objects previously dubbed "water-fountain" sources. Using
the Very Long Baseline Array, we produced the first images of the water maser
emission associated with OH 12.8-0.9. We find that the masers are located in
two compact regions with an angular separation of ~109 mas on the sky. The axis
of separation between the two maser regions is at a position angle of 1.5 deg.
East of North with the blue-shifted (-80.5 to -85.5 km/s) masers located to the
North and the red-shifted (-32.0 to -35.5 km/s) masers to the South. In
addition, we find that the blue- and red-shifted masers are distributed along
arc-like structures ~10-12 mas across oriented roughly perpendicular to the
separation axis. The morphology exhibited by the water masers is suggestive of
an axisymmetric wind with the masers tracing bow shocks formed as the wind
impacts the ambient medium. This bipolar jet-like structure is typical of the
three other confirmed water-fountain sources. When combined with the previously
observed spectral characteristics of OH 12.8-0.9, the observed spatio-kinematic
structure of the water masers provides strong evidence that OH 12.8-0.9 is
indeed a member of the water-fountain class.Comment: 12 pages, 2 figures (1 color), accepted for publication in the Ap J
Letter
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