379 research outputs found
Abundance Anomalies in the X-ray Spectra of the Planetary Nebulae NGC 7027 and BD +30 363
We revisit Chandra observations of the planetary nebulae NGC 7027 and BD +30 3639 in order to address the question of abundance anomalies in the X-ray emitting gas. Enhanced abundances relative to solar of magnesium (Mg) for NGC 7027 and neon (Ne) for BD +30 3639 are required to fit their X-ray spectra, whereas observations at optical and infrared wavelengths show depleted Mg and Ne in these systems. We attribute the enhancement of Mg in NGC 7027 in the X-ray, relative to the optical, to the depletion of Mg onto dust grains within the optical nebula. For BD +30 3639, we speculate that the highly enhanced Ne comes from a WD companion, which accreted a fraction of the wind blown by the asymptotic giant branch progenitor, and went through a nova-like outburst which enriched the X-ray emitting gas with Ne
GCIRS16SW: a massive eclipsing binary in the Galactic Center
We report on the spectroscopic monitoring of GCIRS16SW, an Ofpe/WN9 star and
LBV candidate in the central parsec of the Galaxy. SINFONI observations show
strong daily spectroscopic changes in the K band. Radial velocities are derived
from the HeI 2.112 um line complex and vary regularly with a period of 19.45
days, indicating that the star is most likely an eclipsing binary. Under
various assumptions, we are able to derive a mass of ~ 50 Msun for each
component.Comment: 4 pages, 4 figures, ApJ Letters accepte
The unfriendly ISM in the radio galaxy 4C12.50 (PKS 1345+12)
The radio source 4C12.50 has often been suggested to be a prime candidate for
the link between ultraluminous infrared galaxies and young radio galaxies. A
VLBI study of the neutral hydrogen in the nuclear regions of this object shows
that most of the gas detected close to the systemic velocity is associated with
an off-nuclear cloud (~50 to 100 pc from the radio core) with a column density
of ~10^22 T_spin/100 K) cm^(-2) and an HI mass of a few times 10^5 to 10^6
M_sun. We consider a number of possibilities to explain the results. In
particular, we discus the possibility that this cloud indicates the presence of
a rich and clumpy interstellar medium in the centre, likely left over from the
merger that triggered the activity and that this medium influences the growth
of the radio source. The location of the cloud -- at the edge of the northern
radio jet/lobe -- suggests that the radio jet might be interacting with a gas
cloud. This interaction could be responsible for bending the young radio jet.
The velocity profile of the gas is relatively broad (~150$ km/s) and we
interpret this as kinematical evidence for interaction of the radio plasma with
the cloud. We also consider the model where the cloud is part of a broader
circumnuclear structure. Only a limited region of this structure would have
sufficient background radio brightness and large enough column depth in neutral
gas to obtain detectable HI absorption against the counterjet. The VLBI study
of the neutral hydrogen in 4C12.50 suggests that HI detected near the systemic
velocity (as it is often the case in radio galaxies) may not necessarily be
connected with a circumnuclear disk or torus (as is very often assumed) but
instead could be a tracer of the large-scale medium that surrounds the active
nucleus and that may influence the growth of the young radio source.Comment: 7 pages, 2 figures. Accepted for publication in A&
Interior structure models of GJ 436b
GJ 436b is the first extrasolar planet discovered that resembles Neptune in
mass and radius. The particularly interesting property of Neptune-sized planets
is that their mass Mp and radius Rp are close to theoretical M-R relations of
water planets. Given Mp, Rp, and equilibrium temperature, however, various
internal compositions are possible. A broad set of interior structure models is
presented here that illustrates the dependence of internal composition and
possible phases of water occurring in presumably water-rich planets, such as GJ
436b on the uncertainty in atmospheric temperature profile and mean density. We
show how the set of solutions can be narrowed down if theoretical constraints
from formation and model atmospheres are applied or potentially observational
constraints for the atmospheric metallicity Z1 and the tidal Love number k2. We
model the interior by assuming either three layers (hydrogen-helium envelope,
water layer, rock core) or two layers (H/He/H2O envelope, rocky core). For
water, we use the equation of state H2O-REOS based on FT-DFT-MD simulations.
Some admixture of H/He appears mandatory for explaining the measured radius.
For the warmest considered models, the H/He mass fraction can reduce to 10^-3,
still extending over ~0.7 REarth. If water occurs, it will be essentially in
the plasma phase or in the superionic phase, but not in an ice phase.
Metal-free envelope models have 0.02<k2<0.2, and the core mass cannot be
determined from a measurement of k2. In contrast, models with 0.3<k2<0.82
require high metallicities Z1<0.89 in the outer envelope. The uncertainty in
core mass decreases to 0.4 Mp, if k2>0.3, and further to 0.2 Mp, if k2>0.5, and
core mass and Z1 become sensitive functions of k2. To further narrow the set of
solutions, a proper treatment of the atmosphere and the evolution is necessary.Comment: 9 pages, accepted to A&
A multifunctional cotton fabric using TiO2 and PCMs: introducing thermal comfort and self-cleaning properties
The development of materials with multiple functionalities is a market imperative that places new challenges on textile processing. Whatever the application, the goal is always to achieve the best performance with the simplest and most economically attractive process, without forgetting the sustainability issues. The purpose of this study is to establish the conditions to obtain by a simple method a cotton material with comfort, self-cleaning properties and antimicrobial activity. For that, microcapsules of phase change materials (PCMs) and TiO2 nanoparticles (NP) were applied conjugated and resulting fabrics were characterized by infrared spectroscopy (FTIR), differential scanning calorimetry (DSC), contact angle and scanning electron microscopy with X-ray microanalysis (SEM/EDS). The self-cleaning properties of treated fabrics were also analyzed based on the photocatalytic ability of coated fabrics capability to decomposition of methyl orange (MO) under solar simulator irradiation [1] [1]and assessment of degradation of coffee, red wine and curry stains [2]. The comfort properties were assessed according DSC and Alambeta analysis. Moreover, incorporating TiO2 NP in the finishing formulation also was assessment the bacterial inhibition on the treated fabrics.CNPq-Brazil (Conselho Nacional de Desenvolvimento Científico e Tecnológico – Brasil / National Council of Scientific and Technological Development – Brazil) for the doctoral scholarship (233550/2014-3). Programme - COMPETE and by national funds through FCT – Foundation for Science and Technology within the scope of the project POCI-01-0145-FEDER-007136 and Strategic Funding UID/Multi/04423/2013 by FCT and European Regional Development Fund (ERDF), in the framework of the programme PT2020.info:eu-repo/semantics/publishedVersio
The Centurion 18 telescope of the Wise Observatory
We describe the second telescope of the Wise Observatory, a 0.46-m Centurion
18 (C18) installed in 2005, which enhances significantly the observing
possibilities. The telescope operates from a small dome and is equipped with a
large-format CCD camera. In the last two years this telescope was intensively
used in a variety of monitoring projects.
The operation of the C18 is now automatic, requiring only start-up at the
beginning of a night and close-down at dawn. The observations are mostly
performed remotely from the Tel Aviv campus or even from the observer's home.
The entire facility was erected for a component cost of about 70k$ and a labor
investment of a total of one man-year.
We describe three types of projects undertaken with this new facility: the
measurement of asteroid light variability with the purpose of determining
physical parameters and binarity, the following-up of transiting extrasolar
planets, and the study of AGN variability. The successful implementation of the
C18 demonstrates the viability of small telescopes in an age of huge
light-collectors, provided the operation of such facilities is very efficient.Comment: 16 pages, 13 figures, some figures quality was degraded, accepted for
publication in Astrophysics and Space Scienc
Possible thermochemical disequilibrium in the atmosphere of the exoplanet GJ 436b
The nearby extrasolar planet GJ 436b--which has been labelled as a 'hot
Neptune'--reveals itself by the dimming of light as it crosses in front of and
behind its parent star as seen from Earth. Respectively known as the primary
transit and secondary eclipse, the former constrains the planet's radius and
mass, and the latter constrains the planet's temperature and, with measurements
at multiple wavelengths, its atmospheric composition. Previous work using
transmission spectroscopy failed to detect the 1.4-\mu m water vapour band,
leaving the planet's atmospheric composition poorly constrained. Here we report
the detection of planetary thermal emission from the dayside of GJ 436b at
multiple infrared wavelengths during the secondary eclipse. The best-fit
compositional models contain a high CO abundance and a substantial methane
(CH4) deficiency relative to thermochemical equilibrium models for the
predicted hydrogen-dominated atmosphere. Moreover, we report the presence of
some H2O and traces of CO2. Because CH4 is expected to be the dominant
carbon-bearing species, disequilibrium processes such as vertical mixing and
polymerization of methane into substances such as ethylene may be required to
explain the hot Neptune's small CH4-to-CO ratio, which is at least 10^5 times
smaller than predicted
The nuclear star cluster of the Milky Way
The nuclear star cluster of the Milky Way is a unique target in the Universe.
Contrary to extragalactic nuclear star clusters, using current technology it
can be resolved into tens of thousands of individual stars. This allows us to
study in detail its spatial and velocity structure as well as the different
stellar populations that make up the cluster. Moreover, the Milky Way is one of
the very few cases where we have firm evidence for the co-existence of a
nuclear star cluster with a central supermassive black hole, Sagittarius A*.
The number density of stars in the Galactic center nuclear star cluster can be
well described, at distances pc from Sagittarius A*, by a power-law
of the form with an index of .
In the central parsec the index of the power-law becomes much flatter and
decreases to . We present proper motions for more than 6000
stars within 1 pc in projection from the central black hole. The cluster
appears isotropic at projected distances pc from Sagittarius A*.
Outside of 0.5 pc and out to 1.0 pc the velocity dispersion appears to stay
constant. A robust result of our Jeans modeling of the data is the required
presence of of extended (stellar) mass in the
central parsec of the Galaxy.Comment: To appear in the proceedings of "The Universe under the Microscope -
Astrophysics at High Angular Resolution", Journal of Physics:Conference
Series (IOP; http://www.iop.org/EJ/conf) This version has been slightly
modified (e.g. double-log plot in right hand panel of Figure 5
Recommended from our members
Teaching in Contemporary Forest Resources Curricula: Applications to Courses in Forest Measurements and Biometrics
Foresters face new and evolving challenges as society reconsiders the balance of its interests between wood production and the provision of ecosystem services in the management of forests. Whatever paths this process may take, sound and broad-based decisions will continue to require accurate and relevant measurements of current forest conditions and projections of future conditions under alternative management programs. Forest measurements and biometrics (FMB) will remain a key component of future forest management and a critical element in the education of future forest managers. As professors who both teach and do research in FMB, we offer teaching goals that we believe will improve FMB education in forestry schools to meet future needs.
In the following sections, we outline teaching goals for university-level instruction in forest resources curricula and the roles of FMB in modern forestry. We then identify what we feel are the most critical challenges in teaching and learning FMB and discuss selected strategies to meet teaching objectives for FMB. A fourth section presents an overview of how selected strategies can be integrated into FMB classes, including examples and comments on the role that new technology might play in meeting the above-described challenges. The final section summarizes our main points and provides concluding remarks.This is the author's peer-reviewed final manuscript, as accepted by the publisher. The published article is copyrighted by the Society of American Foresters and can be found at: http://www.safnet.org/publications/jof/index.cfm.Keywords: forest inventory and monitoring, teaching applied statistics, Pacific Northwest, forest analysis, forest pedagog
A homogeneous spectroscopic analysis of host stars of transiting planets
The analysis of transiting extra-solar planets provides an enormous amount of
information about the formation and evolution of planetary systems. A precise
knowledge of the host stars is necessary to derive the planetary properties
accurately. The properties of the host stars, especially their chemical
composition, are also of interest in their own right. Information about planet
formation is inferred by, among others, correlations between different
parameters such as the orbital period and the metallicity of the host stars.
The stellar properties studied should be derived as homogeneously as possible.
The present work provides new, uniformly derived parameters for 13 host stars
of transiting planets. Effective temperature, surface gravity, microturbulence
parameter, and iron abundance were derived from spectra of both high
signal-to-noise ratio and high resolution by assuming iron excitation and
ionization equilibria. For some stars, the new parameters differ from previous
determinations, which is indicative of changes in the planetary radii. A
systematic offset in the abundance scale with respect to previous assessments
is found for the TrES and HAT objects. Our abundance measurements are
remarkably robust in terms of the uncertainties in surface gravities. The iron
abundances measured in the present work are supplemented by all previous
determinations using the same analysis technique. The distribution of iron
abundance then agrees well with the known metal-rich distribution of planet
host stars. To facilitate future studies, the spectroscopic results of the
current work are supplemented by the findings for other host stars of
transiting planets, for a total dataset of 50 objects.Comment: accepted for publication in A&A, 7 pages, 6 figure
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