390 research outputs found
Carbon chemistry in Galactic Bulge Planetary Nebulae
Galactic Bulge Planetary Nebulae show evidence of mixed chemistry with
emission from both silicate dust and PAHs. This mixed chemistry is unlikely to
be related to carbon dredge up, as third dredge-up is not expected to occur in
the low mass Bulge stars. We show that the phenomenon is widespread, and is
seen in 30 nebulae out of 40 of our sample, selected on the basis of their
infrared flux. HST images and UVES spectra show that the mixed chemistry is not
related to the presence of emission-line stars, as it is in the Galactic disk
population. We also rule out interaction with the ISM as origin of the PAHs.
Instead, a strong correlation is found with morphology, and the presence of a
dense torus. A chemical model is presented which shows that hydrocarbon chains
can form within oxygen-rich gas through gas-phase chemical reactions. The model
predicts two layers, one at where small hydrocarbons form from
reactions with C, and one at , where larger chains (and by
implication, PAHs) form from reactions with neutral, atomic carbon. These
reactions take place in a mini-PDR. We conclude that the mixed chemistry
phenomenon occurring in the Galactic Bulge Planetary Nebulae is best explained
through hydrocarbon chemistry in an UV-irradiated, dense torus.Comment: 13 pages, 10 figue
Dust mass-loss rates from AGB stars in the Fornax and Sagittarius dwarf Spheroidal galaxies
To study the effect of metallicity on the mass-loss rate of asymptotic giant
branch (AGB) stars, we have conducted mid-infrared photometric measurements of
such stars in the Sagittarius (Sgr dSph) and Fornax dwarf spheroidal galaxies
with the 10-m camera VISIR at the VLT. We derive mass-loss rates for 29
AGB stars in Sgr dSph and 2 in Fornax. The dust mass-loss rates are estimated
from the and colours. Radiative transfer models are used to
check the consistency of the method. Published IRAS and Spitzer data confirm
that the same tight correlation between colour and dust mass-loss
rates is observed for AGB stars from galaxies with different metallicities,
i.e. the Galaxy, the LMC and the SMC.
The derived dust mass-loss rates are in the range 5 to
3 Myr for the observed AGB stars in Sgr dSph
and around 5 Myr for those in Fornax; while
values obtained with the two different methods are of the same order of
magnitude. The mass-loss rates for these stars are higher than the nuclear
burning rates, so they will terminate their AGB phase by the depletion of their
stellar mantles before their core can grow significantly. Some observed stars
have lower mass-loss rates than the minimum value predicted by theoretical
models.Comment: 12 pages, 9 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&
Modelling of intermediate-age stellar populations: III Effects of dust-shells around AGB stars
In this paper,we present single stellar population models of intermediate age
stellar populations where dust-enshrouded AGB stars are introduced. The
formation of carbon stars is also accounted for, and is taken to be a function
of both initial mass and metallicity. The effect of the dusty envelopes around
AGB stars on the optical/near-infrared spectral energy distribution were
introduced using semi-emipirical models where the mass-loss and the
photospheric chemistry determine the spectral properties of a star along the
AGB sequence. The spectral dichotomy between O-rich stars and C-rich stars is
taken into account in the modelling. We have investigated the AGB sequence
morphology in he near-infrared CMD as a function of time and metallicity. We
show that this diaggram is characterized by three morphological features,
occupied by optically bright O-rich stars, optically bright C-rich stars, and
dust-enshrouded O-rich and C-rich stars respectively. Our models are able to
reproduce the distribution of the three AGB subtype stellar populations in
colour-colour diagrams. Effects of dusty envelopes on the luminosity function
are also investigated (Abriged).Comment: 11 pages, 9 figures, accepted for publication in A&
RS-invariant all-orders renormalon resummations for some QCD observables
We propose a renormalon-inspired resummation of QCD perturbation theory based
on approximating the renormalization scheme (RS) invariant effective charge
beta-function coefficients by the portion containing the highest power of
=--, for SU() QCD with quark flavours.
This can be accomplished using exact large- all-orders results. The
resulting resummation is RS-invariant and the exact next-to-leading order (NLO)
and next-to-NLO (NNLO) coefficients in any RS are included. This improves on a
previously employed naive resummation of the leading- piece of the
perturbative coefficients which is RS-dependent, making its comparison with
fixed-order perturbative results ambiguous. The RS-invariant resummation is
used to assess the reliability of fixed-order perturbation theory for the
-ratio, the analogous -lepton decay ratio , and
Deep Inelastic Scattering (DIS) sum rules, by comparing it with the exact NNLO
results in the effective charge RS. For the -ratio and , where
large-order perturbative behaviour is dominated by a leading ultra-violet
renormalon singularity, the comparison indicates fixed-order perturbation
theory to be very reliable. For DIS sum rules, which have a leading infra-red
renormalon singularity, the performance is rather poor. In this way we estimate
that at LEP/SLD energies ideal data on the -ratio could determine
to three-significant figures, and for the we
estimate a theoretical uncertainty
corresponding to . This encouragingly small
uncertainty is much less than has recently been deduced from comparison with
the ambiguous naive resummation.Comment: 25 pages, uses LaTeX, 12 Postscript figures, epsfig.sty 'elsart.sty'
and 'elsart12.sty' are available via anonymous-ftp at
ftp://ftp.tex.ac.uk/tex-archive/macros/latex/contrib/supported/elsevie
The stellar remnant of SN 1181
We report observations and modelling of the stellar remnant and presumed
double-degenerate merger of Type~Iax supernova SN 1181 AD. It is the only known
bound stellar SN remnant and the only star with Wolf-Rayet features that is
neither a planetary nebula central star nor a massive Pop I progenitor. We
model the unique emission-line spectrum with broad, strong O VI and O VIII
lines as a fast stellar wind and shocked, hot gas. Non-LTE wind modeling
indicates a mass-loss rate of and a
terminal velocity of 15,000 km s, consistent with earlier results.
O VIII lines indicate shocked gas temperatures of MK. We derive a
magnetic field upper limit of MG, below earlier suggestions. The
luminosity indicates a remnant mass of with ejecta
mass . Archival photometry suggests the stellar
remnant has dimmed by 0.5 magnitudes over 100 years. A low Ne/O
argues against a O-Ne white dwarf in the merger. A cold dust shell is only the
second detection of dust in a SN Iax and the first of cold dust. Our ejecta
mass and kinetic energy estimates of the remnant are consistent with Type Iax
extragalactic sources.Comment: 19 pages, 13 figures, 3 tables. Submitte
Evolution of the dust mass loss with luminosity along the giant branch of the globular cluster 47 Tuc
The paper investigates the properties of the dust mass loss in stars
populating the giant branch of the globular cluster 47 Tuc, by combining ISOCAM
and DENIS data. Raster maps of 5 fields covering areas ranging from 4 x 4 to 15
x 15 arcmin2 at different distances from the center of the cluster have been
obtained with ISOCAM at 11.5 mum (LW10 filter). The covered fields include most
of the red variables known in this cluster. A detection threshold of about 0.2
mJy is achieved, allowing to detect giant stars at 11.5 mum all the way down to
the horizontal branch. No dust-enshrouded asymptotic giant branch stars have
been found in the observed fields, contrary to the situation encountered in
LMC/SMC globular clusters with larger turnoff masses. The color index [12]-[2]
(based on the ISO 11.5 mum flux and on the DENIS Ks magnitude) is used as a
diagnostic of dust emission (and hence dust mass loss). Its evolution with
luminosity along the giant branch reveals that dust mass loss is only present
in V3 (the only cluster Mira variable observed in the present study) and in
V18, a star presenting intermittent variability. This conclusion confirms the
importance of stellar pulsations in the dust formation and ensuing mass loss.Comment: 16 pages, accepted in Astronomy & Astrophysic
Reprocessing the Hipparcos data for evolved stars III Revised Hipparcos period-luminosity relationship for galactic long-period variable stars
We analyze the K band luminosities of a sample of galactic long-period
variables using parallaxes measured by the Hipparcos mission. The parallaxes
are in most cases re-computed from the Hipparcos Intermediate Astrometric Data
using improved astrometric fits and chromaticity corrections. The K band
magnitudes are taken from the literature and from measurements by COBE, and are
corrected for interstellar and circumstellar extinction. The sample contains
stars of several spectral types: M, S and C, and of several variability
classes: Mira, semiregular SRa, and SRb. We find that the distribution of stars
in the period-luminosity plane is independent of circumstellar chemistry, but
that the different variability types have different P-L distributions. Both the
Mira variables and the SRb variables have reasonably well-defined
period-luminosity relationships, but with very different slopes. The SRa
variables are distributed between the two classes, suggesting that they are a
mixture of Miras and SRb, rather than a separate class of stars. New
period-luminosity relationships are derived based on our revised Hipparcos
parallaxes. The Miras show a similar period-luminosity relationship to that
found for Large Magellanic Cloud Miras by Feast et al. (1989). The maximum
absolute K magnitude of the sample is about -8.2 for both Miras and
semi-regular stars, only a little fainter than the expected AGB limit. We show
that the stars with the longest periods (P>400d) have high mass loss rates and
are almost all Mira variables.Comment: Comments welcome. Submitted to A&A 11 pages, 7 figs, 3 table
Search for radiative pumping lines of OH masers: I. The 34.6um absorption line towards 1612 MHz OH maser sources
The 1612 MHz hydroxyl maser in circumstellar envelopes has long been thought
to be pumped by 34.6um photons. Only recently, the Infrared Space Observatory
has made possible spectroscopic observations which enable the direct
confirmation of this pumping mechanism in a few cases. To look for the presence
of this pumping line, we have searched the Infrared Space Observatory Data
Archive and found 178 spectra with data around 34.6um for 87 galactic 1612MHz
masers. The analysis performed showed that the noise level and the spectral
resolution of the spectra are the most important factors affecting the
detection of the 34.6um absorption line. Only 5 objects from the sample (3 red
supergiants and 2 galactic center sources) are found to show clear 34.6um
absorption (all of them already known) while two additional objects only
tentatively show this line. The 3 supergiants show similar pump rates and their
masers might be purely radiatively pumped. The pump rates of OH masers in late
type stars are found to be about 0.05, only 1/5 of the theoretical value of
0.25 derived by Elitzur (1992). We have also found 16 maser sources which,
according to the analysis assuming Elitzur's pump rate, should show the 34.6
m absorption line but do not. These non-detections can be tentatively
explained by far-infrared photon pumping, clumpy nature of the OH masing region
or a limb-filling emission effect in the OH shell.Comment: 11 pages, 8 figures, 3 table
The Illumination and Growth of CRL 2688: An Analysis of New & Archival HST Observations
We present four-color images of CRL 2688 obtained in 2009 using the
Wide-Field Camera 3 on HST. The F606W image is compared with archival images in
very similar filters to monitor the proper motions of nebular structure. We
find that the bright N-S lobes have expanded uniformly by 2.5% and that the
ensemble of rings has translated radially by 0.07 in 6.65 y. The rings were
ejected every 100y for ~4 millennia until the lobes formed 250y ago. Starlight
scattered from the edges of the dark E-W dust lane is coincident with extant H2
images and leading tips of eight pairs of CO outflows. We interpret this as
evidence that fingers lie within geometrically opposite cones of opening angles
{\approx} 30{\circ} like those in CRL618. By combining our results of the rings
with 12CO absorption from the extended AGB wind we ascertain that the rings
were ejected at ~18 km s-1 with very little variation and that the distance to
CRL2688, v_{exp}{\dot\theta}_exp$, is 300 - 350 pc. Our 2009 imaging
program included filters that span 0.6 to 1.6{\mu}m. We constructed a
two-dimensional dust scattering model of stellar radiation through CRL2688 that
successfully reproduces the details of the nebular geometry, its integrated
spectral energy distribution, and nearly all of its color variations. The model
implies that the optical opacity of the lobes >~ 1, the dust particle density
in the rings decreases as radius^{-3} and that the mass and momentum of the AGB
winds and their rings have increased over time.Comment: (51 pages, 6 figures; accepted by ApJ
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