1,040 research outputs found
The shapes of light curves of Mira-type variables
Using a sample of 454 mira light curves from the ASAS survey we study the
shape of the light variations in this kind of variable stars. Opposite to
earlier studies, we choose a general approach to identify any deviation from a
sinusoidal light change. We find that about 30% of the studied light curves
show a significant deviation from the sinusoidal reference shape. Among these
stars two characteristic light curve shapes of comparable frequency could be
identified. Some hint for a connection between atmospheric chemistry and light
curve shape was found, but beside that no or only very weak relations between
light curve shape and other stellar parameters seem to exist.Comment: 7 pages, 7 figures, accepted for publication in A
Insight into the OH polarimetric structure of OH 26.5+0.6
We present the first view of the magnetic field structure in the OH shell of
the extreme OH/IR star OH 26.5+0.6. MERLIN interferometric observations of this
object were obtained in December 1993 in full polarisation, at 1612, 1665 and
1667 MHz. The maser spots show a spheroidal distribution both at 1612 and 1667
MHz, while at 1665 MHz emission from the blue-shifted maser peak is
concentrated on the stellar position, and the red-shifted peak emission
exhibits a filamentary structure oriented on a SE-NW axis. The linear
polarisation in both main lines is rather faint, ranging from 9 to 20% at 1665
MHz and from 0 to 30% at 1667 MHz. At 1612 MHz most maser spots exhibit a
similar range of linear polarisation although those in the outermost parts of
the envelope reach values as high as 66%. This is particularly apparent in the
southern part of the shell. The detailed distribution of the polarisation
vectors could only be obtained at 1612 MHz. The polarisation vectors show a
highly structured distribution indicative of a poloidal magnetic field inclined
by 40-60 to the line of sight. The velocity distribution of the maser
spots with respect to the radial distance is well explained by an isotropic
outflow at constant velocity in the case of a prolate shaped spheroid envelope,
also tilted about 45-65 to the line of sight.Comment: 20 pages, 16 figures, accepted for publication in MNRA
OH spectral evolution of oxygen-rich late-type stars
We investigated the main-line spectral evolution with shell thickness of
oxygen rich AGB stars. The study is based on a sample of 30 sources distributed
along the IRAS colour-colour diagram. The sources were chosen to trace the
Miras with thick shells and the whole range of OH/IR stars. The Miras exhibit a
1665 MHz emission strength comparable to that at 1667 MHz. Even though the
Miras of the study have quite thick shells, their spectral characteristics in
both main lines attest to a strong heterogeneity in their OH shell with, in
particular, the presence of significant turbulence and acceleration. The
expansion velocity has been found to be about the same at 1665 and 1667 MHz,
taking into account a possible velocity turbulence of 1-2km/s at the location
of the main-line maser emission. An increase in the intensity ratio 1667/1665
with shell thickness has been found. A plausible explanation for such a
phenomenon is that competitive gain in favour of the 1667 MHz line increases
when the shell is getting thicker. There is an evolution in the spectral
profile shape with the appearance of a substantial inter-peak signal when the
shell is getting thicker. Also, inter-peak components are found and can be as
strong as the external standard peaks when the shell is very thick. This trend
for an increase of the signal in between the two main peaks is thought to be
the result of an increase of the saturation with shell thickness. All sources
but two - a Mira and an OH/IR star from the lower part of the colour-colour
diagram - are weakly polarized. The strong polarization observed for those two
particular objects is thought to be the result of perturbations in their
shells.Comment: 19 pages, 12 figures, accepted for publication in A&
Cardiovascular risk profile and frailty in a population-based study of older British men.
BACKGROUND: Frailty in older age is known to be associated with cardiovascular disease (CVD) risk. However, the extent to which frailty is associated with the CVD risk profile has been little studied. Our aim was to examine the associations of a range of cardiovascular risk factors with frailty and to assess whether these are independent of established CVD.
METHODS: Cross-sectional study of a socially representative sample of 1622 surviving men aged 71-92 examined in 2010-2012 across 24 British towns, from a prospective study initiated in 1978-1980. Frailty was defined using the Fried phenotype, including weight loss, grip strength, exhaustion, slowness and low physical activity.
RESULTS: Among 1622 men, 303 (19%) were frail and 876 (54%) were pre-frail. Compared with non-frail, those with frailty had a higher odds of obesity (OR 2.03, 95% CI 1.38 to 2.99), high waist circumference (OR 2.30, 95% CI 1.67 to 3.17), low high-density lipoprotein-cholesterol (HDL-C) (OR 2.28, 95% CI 1.47 to 3.54) and hypertension (OR 1.79, 95% CI 1.27 to 2.54). Prevalence of these factors was also higher in those with frailty (prevalence in frail vs non-frail groups was 46% vs 31% for high waist circumference, 20% vs 11% for low HDL and 78% vs 65% for hypertension). Frail individuals had a worse cardiovascular risk profile with an increased risk of high heart rate, poor lung function (forced expiratory volume in 1â
s (FEV1)), raised white cell count (WCC), poor renal function (low estimated glomerular filtration rate), low alanine transaminase and low serum sodium. Some risk factors (HDL-C, hypertension, WCC, FEV1, renal function and albumin) were also associated with being pre-frail. These associations remained when men with prevalent CVD were excluded.
CONCLUSIONS: Frailty was associated with increased risk of a range of cardiovascular factors (including obesity, HDL-C, hypertension, heart rate, lung function, renal function) in older people; these associations were independent of established CVD
Polarization properties of OH masers in AGB and post-AGB stars
Context: Ground-state OH maser emission from late-type stars is usually
polarized and remains a powerful probe of the magnetic field structure in the
outer regions of circumstellar envelopes if observed with high angular and
spectral resolutions. Observations in all four Stokes parameters are quite
sparse and this is the most thorough, systematic study published to date.
Aims: We aim to determine polarization properties of OH masers in an
extensive sample of stars that show copious mass loss and search for candidate
objects that are well-suited for high angular resolution studies.
Methods: Full-polarization observations of the OH 1612 and 1667 MHz maser
transitions were carried out for a sample of 117 AGB and post-AGB stars.
Several targets were also observed in the 1665 MHz line.
Results: Polarized features occur in more than 75% of the sources in the
complete sample and there is no intrinsic difference in the occurrence of
polarized emission between the three classes of objects of different infrared
characteristics. The highest fractional polarization occurs for the post-AGB+PN
and the Mira+SR classes at 1612 and 1667 MHz, respectively. Differences in the
fractional polarization between the sources at different evolutionary stages
appear to be related to depolarization caused by blending. The alignment of the
polarization angles at the extreme sides of the shell implies a regular
structure of the magnetic field of a strength of 0.3-2.3 mG.
Conclusions: Polarized OH maser features are widespread in AGB and post-AGB
stars. The relationship between the circular and linear fractional
polarizations for a representative sample are consistent with the standard
models of polarization for the Zeeman splitting higher than the Doppler line
width, whereas the polarized features are the sigma components.Comment: Accepted for publication in Astronomy and Astrophysics. A version
with appendices (Tab. A.1 and Fig. B.1) can be downloaded from
http://paulo.astro.uni.torun.pl/~pw/arXiv_
Dust and the spectral energy distribution of the OH/IR star OH 127.8+0.0: Evidence for circumstellar metallic iron
We present a fit to the spectral energy distribution of OH 127.8+0.0, a
typical asymptotic giant branch star with an optically thick circumstellar dust
shell. The fit to the dust spectrum is achieved using non-spherical grains
consisting of metallic iron, amorphous and crystalline silicates and water ice.
Previous similar attempts have not resulted in a satisfactory fit to the
observed spectral energy distributions, mainly because of an apparent lack of
opacity in the 3--8 micron region of the spectrum. Non-spherical metallic iron
grains provide an identification for the missing source of opacity in the
near-infrared. Using the derived dust composition, we have calculated spectra
for a range of mass-loss rates in order to perform a consistency check by
comparison with other evolved stars. The L-[12 micron] colours of these models
correctly predict the mass-loss rate of a sample of AGB stars, strengthening
our conclusion that the metallic iron grains dominate the near-infrared flux.
We discuss a formation mechanism for non-spherical metallic iron grains.Comment: 10 pages, 6 figures, accepted for publication by A&
A Galactic Bar to Beyond the Solar Circle and its Relevance for Microlensing
The Galactic kinematics of Mira variables have been studied using infrared
photometry, radial velocities, and Hipparcos parallaxes and proper motions. For
Miras in the period range 145 to 200 days (probably corresponding to [Fe/H] in
the range -0.8 to -1.3) the major axes of the stellar orbits are concentrated
in the first quadrant of Galactic longitude. This is interpreted as a
continuation of the bar-like structure of the Galactic Bulge out to the solar
circle and beyond.Comment: 6 pages, 2 figures. To be published in: Microlensing 2000. ASP
Conference Series, Eds. J W Menzies, P Sacket
The variable mass loss of the AGB star WX Psc as traced by the CO J=1-0 through 7-6 lines and the dust emission
Low and intermediate mass stars lose a significant fraction of their mass
through a dust-driven wind during the Asymptotic Giant Branch (AGB) phase.
Recent studies show that winds from late-type stars are far from being smooth.
Mass-loss variations occur on different time scales, from years to tens of
thousands of years. The variations appear to be particularly prominent towards
the end of the AGB evolution. The occurrence, amplitude and time scale of these
variations are still not well understood.
The goal of our study is to gain insight into the structure of the
circumstellar envelope (CSE) of WX Psc and map the possible variability of the
late-AGB mass-loss phenomenon.
We have performed an in-depth analysis of the extreme infrared AGB star WX
Psc by modeling (1) the CO J=1-0 through 7-6 rotational line profiles and the
full spectral energy distribution (SED) ranging from 0.7 to 1300 micron. We
hence are able to trace a geometrically extended region of the CSE.
Both mass-loss diagnostics bear evidence of the occurrence of mass-loss
modulations during the last ~2000 yr. In particular, WX Psc went through a high
mass-loss phase (Mdot~5e-5 Msun/yr) some 800 yr ago. This phase lasted about
600 yr and was followed by a long period of low mass loss (Mdot~5e-8 Msun/yr).
The present day mass-loss rate is estimated to be ~6e-6 Msun/yr.
The AGB star WX Psc has undergone strong mass-loss rate variability on a time
scale of several hundred years during the last few thousand years. These
variations are traced in the strength and profile of the CO rotational lines
and in the SED. We have consistently simulated the behaviour of both tracers
using radiative transfer codes that allow for non-constant mass-loss rates.Comment: 12 pages, accepted for publication in A&
Critical behavior of the planar magnet model in three dimensions
We use a hybrid Monte Carlo algorithm in which a single-cluster update is
combined with the over-relaxation and Metropolis spin re-orientation algorithm.
Periodic boundary conditions were applied in all directions. We have calculated
the fourth-order cumulant in finite size lattices using the single-histogram
re-weighting method. Using finite-size scaling theory, we obtained the critical
temperature which is very different from that of the usual XY model. At the
critical temperature, we calculated the susceptibility and the magnetization on
lattices of size up to . Using finite-size scaling theory we accurately
determine the critical exponents of the model and find that =0.670(7),
=1.9696(37), and =0.515(2). Thus, we conclude that the
model belongs to the same universality class with the XY model, as expected.Comment: 11 pages, 5 figure
Bisecting the mental number line in near and far space
Much evidence suggests that common posterior parietal mechanisms underlie the orientation of attention in physical space and along the mental number line. For example, the small leftward bias (pseudoneglect) found in paper-and-pencil line bisection is also found when participants "bisect" number pairs, estimating (without calculating) the number midway between two others. For bisection of physical lines, pseudoneglect has been found to shift rightward as lines are moved from near space (immediately surrounding the body) to far space. We investigated whether the presentation of stimuli in near or far space also modulated spatial attention for the mental number line. Participants bisected physical lines or number pairs presented at four distances (60, 120, 180, 240 cm). Clear rightward shifts in bias were observed for both tasks. Furthermore, the rate at which this shift occurred in the two tasks, as measured by least squares regression slopes, was significantly correlated across participants, suggesting that the transition from near to far distances induced a common modulation of lateral attention in physical and numerical space. These results demonstrate a tight coupling between number and physical space, and show that even such prototypically abstract concepts as number are modulated by our on-line interactions with the world
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