2,349 research outputs found
Wolf-Rayet stars in the Small Magellanic Cloud: I. Analysis of the single WN stars
Wolf-Rayet (WR) stars have a severe impact on their environments owing to
their strong ionizing radiation fields and powerful stellar winds. Since these
winds are considered to be driven by radiation pressure, it is theoretically
expected that the degree of the wind mass-loss depends on the initial
metallicity of WR stars. Following our comprehensive studies of WR stars in the
Milky Way, M31, and the LMC, we derive stellar parameters and mass-loss rates
for all seven putatively single WN stars known in the SMC. Based on these data,
we discuss the impact of a low-metallicity environment on the mass loss and
evolution of WR stars. The quantitative analysis of the WN stars is performed
with the Potsdam Wolf-Rayet (PoWR) model atmosphere code. The physical
properties of our program stars are obtained from fitting synthetic spectra to
multi-band observations. In all SMC WN stars, a considerable surface hydrogen
abundance is detectable. The majority of these objects have stellar
temperatures exceeding 75 kK, while their luminosities range from 10^5.5 to
10^6.1 Lsun. The WN stars in the SMC exhibit on average lower mass-loss rates
and weaker winds than their counterparts in the Milky Way, M31, and the LMC. By
comparing the mass-loss rates derived for WN stars in different Local Group
galaxies, we conclude that a clear dependence of the wind mass-loss on the
initial metallicity is evident, supporting the current paradigm that WR winds
are driven by radiation. A metallicity effect on the evolution of massive stars
is obvious from the HRD positions of the SMC WN stars at high temperatures and
high luminosities. Standard evolution tracks are not able to reproduce these
parameters and the observed surface hydrogen abundances. Homogeneous evolution
might provide a better explanation for their evolutionary past.Comment: 18+12 pages; 22+8 figures; accepted for publication in A&
Weak magnetic fields in central stars of planetary nebulae?
It is not yet clear whether magnetic fields play an essential role in shaping
planetary nebulae (PNe), or whether stellar rotation alone and/or a close
binary companion can account for the variety of the observed nebular
morphologies. In a quest for empirical evidence verifying or disproving the
role of magnetic fields in shaping PNe, we follow up on previous attempts to
measure the magnetic field in a representative sample of PN central stars. We
obtained low-resolution polarimetric spectra with FORS 2 at VLT for a sample of
twelve bright central stars of PNe with different morphology, including two
round nebulae, seven elliptical nebulae, and three bipolar nebulae. Two targets
are Wolf-Rayet type central stars. For the majority of the observed central
stars, we do not find any significant evidence for the existence of surface
magnetic fields. However, our measurements may indicate the presence of weak
mean longitudinal magnetic fields of the order of 100 Gauss in the central star
of the young elliptical planetary nebula IC 418, as well as in the Wolf-Rayet
type central star of the bipolar nebula Hen2-113 and the weak emission line
central star of the elliptical nebula Hen2-131. A clear detection of a 250 G
mean longitudinal field is achieved for the A-type companion of the central
star of NGC 1514. Some of the central stars show a moderate night-to-night
spectrum variability, which may be the signature of a variable stellar wind
and/or rotational modulation due to magnetic features. We conclude that strong
magnetic fields of the order of kG are not widespread among PNe central stars.
Nevertheless, simple estimates based on a theoretical model of magnetized wind
bubbles suggest that even weak magnetic fields below the current detection
limit of the order of 100 G may well be sufficient to contribute to the shaping
of PNe throughout their evolution.Comment: 16 pages, 11 figures, 3 tables, accepted for publication in A&A;
References updated, minor correction
On X-ray pulsations in beta Cephei-type variables
Beta Cephei-type variables are early B-type stars that are characterized by
oscillations observable in their optical light curves. At least one Beta
Cep-variable also shows periodic variability in X-rays. Here we study the X-ray
light curves in a sample of beta Cep-variables to investigate how common X-ray
pulsations are for this type of stars. We searched the Chandra and XMM-Newton
X-ray archives and selected stars that were observed by these telescopes for at
least three optical pulsational periods. We retrieved and analyzed the X-ray
data for kappa Sco, beta Cru, and alpha Vir. The X-ray light curves of these
objects were studied to test for their variability and periodicity. While there
is a weak indication for X-ray variability in beta Cru, we find no
statistically significant evidence of X-ray pulsations in any of our sample
stars. This might be due either to the insufficient data quality or to the
physical lack of modulations. New, more sensitive observations should settle
this question.Comment: accepted in A&
Approaches to the mechanisms of song memorization and singing provide evidence for a procedural memory
The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud: spectroscopy, orbital analysis, formation, and evolution
Massive Wolf-Rayet (WR) stars dominate the radiative and mechanical energy
budget of galaxies and probe a critical phase in the evolution of massive stars
prior to core-collapse. It is not known whether core He-burning WR stars
(classical WR, cWR) form predominantly through wind-stripping (w-WR) or binary
stripping (b-WR). With spectroscopy of WR binaries so-far largely avoided due
to its complexity, our study focuses on the 44 WR binaries / binary candidates
of the Large Magellanic Cloud (LMC, metallicity Z~0.5 Zsun), identified on the
basis of radial velocity variations, composite spectra, or high X-ray
luminosities. Relying on a diverse spectroscopic database, we aim to derive the
physical and orbital parameters of our targets, confronting evolution models of
evolved massive stars at sub-solar metallicity, and constraining the impact of
binary interaction in forming them. Spectroscopy is performed using the Potsdam
Wolf-Rayet (PoWR) code and cross-correlation techniques. Disentanglement is
performed using the code Spectangular or the shift-and-add algorithm.
Evolutionary status is interpreted using the Binary Population and Spectral
Synthesis (BPASS) code, exploring binary interaction and chemically-homogeneous
evolution.
No obvious dichotomy in the locations of apparently-single and binary WN
stars on the Hertzsprung-Russell diagram is apparent. According to commonly
used stellar evolution models (BPASS, Geneva), most apparently-single WN stars
could not have formed as single stars, implying that they were stripped by an
undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing
(e.g., during the red supergiant phase) are strongly underestimated in standard
stellar evolution models.Comment: accepted to A&A on 10.05.2019; 69 pages (25 main paper + 44
appendix); Corrigendum: Shenar et al. 2020, A&A, 641, 2: An unfortunate typo
in the implementation of the "transformed radius" caused errors of up to
~0.5dex in the derived mass-loss rates. This has now been correcte
Abyssal fauna of the UK-1 polymetallic nodule exploration area, Clarion-Clipperton Zone, central Pacific Ocean: Mollusca
The file attached is the Published/publisher’s pdf version of the article. This is an OpenAccess article.Copyright Helena Wiklund et al. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY 4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited
A " high 4 He/ 3 He " mantle material detected under the East Pacific Rise (15°4′N)
International audienceWe investigate in details helium isotope data reported in Mougel et al. (2014) for 14 basaltic samples collected on the East Pacific Rise by submersible (15°4′N) where the ridge interacts with the Mathematician seamounts. Samples locations are separated by only few hundred meters across a 15 km along-axis profile. The data reveal a strong geochemical variability that has never been observed at such high spatial resolution for helium isotope compositions. Moreover, they reveal an unusually high 4 He/ 3 He mantle component also characterized by unradiogenic lead, atypical in oceanic basalts. He-Pb systematics suggests a mixture between a nonradiogenic lead and radiogenic helium pyroxenitic component, recycled from the deep continental lithosphere and the ambient peridotitic mantle. The He isotope difference between these two end-members can be interpreted as a time evolution of two distinct mantle sources after a slight (U + Th)/ 3 He fractionation, likely due to some ancient degassing during the formation of deep continental pyroxenites
Fabrication of Large Domain YBa2Cu3O(x) for Magnetic Suspension Applications
Large domain YBa2Cu3O(x) levitators have been fabricated using a seeded melt processing technique. Depending upon the seed, either a single or five domained sample can be obtained. The grain boundaries separating each domains in the five domain levitator are found to be 90 degrees. Similar levitation forces can be observed for single and five domained samples. After thermal cycling, however, a small decrease in the levitation force of the five domain levitator was observed as a function of thermal cycles while nearly no change in force was observed in the single domain levitator. Finally, it is shown that both, single and five domain YBCO, behave similarly as a function of sample thickness
PoWR grids of non-LTE model atmospheres for OB-type stars of various metallicities
The study of massive stars in different metallicity environments is a central
topic of current stellar research. The spectral analysis of massive stars
requires adequate model atmospheres. The computation of such models is
difficult and time-consuming. Therefore, spectral analyses are greatly
facilitated if they can refer to existing grids of models. Here we provide
grids of model atmospheres for OB-type stars at metallicities corresponding to
the Small and Large Magellanic Clouds, as well as to solar metallicity. In
total, the grids comprise 785 individual models. The models were calculated
using the state-of-the-art Potsdam Wolf-Rayet (PoWR) model atmosphere code. The
parameter domain of the grids was set up using stellar evolution tracks. For
all these models, we provide normalized and flux-calibrated spectra, spectral
energy distributions, feedback parameters such as ionizing photons, Zanstra
temperatures, and photometric magnitudes. The atmospheric structures (the
density and temperature stratification) are available as well. All these data
are publicly accessible through the PoWR website.Comment: 12 pages, 14 figures, accepted for publication in Astronomy &
Astrophysic
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