590 research outputs found
Properties of the solar neighbor WISE J072003.20-084651.2
The severe crowding towards the Galactic plane suggests that the census of
nearby stars in that direction may be incomplete. Recently, Scholz reported a
new M9 object at an estimated distance d~7 pc (WISE J072003.20-084651.2;
hereafter WISE0720) at Galactic latitude b=2.3 degr.
Our goals are to determine the physical characteristics of WISE0720, its
kinematic properties, and to address the question if it is a binary object, as
suggested in the discovery paper.
Optical and infrared spectroscopy from the Southern African Large Telescope
and Magellan, respectively, and spectral energy distribution fitting were used
to determine the spectral type of WISE0720. The measured radial velocity,
proper motion and parallax yielded its Galactic velocities. We also
investigated if WISE0720 may show X-ray activity based on archival data.
Our spectra are consistent with spectral type L0+/-1. We find no evidence for
binarity, apart for a minor 2-sigma level difference in the radial velocities
taken at two different epochs. The spatial velocity of WISE0720 does not
connect it to any known moving group, instead it places the object with high
probability in the old thin disk or in the thick disk. The spectral energy
distribution fit hints at excess in the 12 and 22 micron WISE bands which may
be due to a redder companion, but the same excess is visible in other late type
objects, and it more likely implies a shortcoming of the models (e.g., issues
with the effective wavelengths of the filters for these extremely cool objects,
etc.) rather than a disk or redder companion. The optical spectrum shows some
Halpha emission, indicative of stellar activity. Archival X-ray observations
yield no detection.Comment: A&A, accepted; 9 pages, 6 figure
Spectra disentangling applied to the Hyades binary Theta^2 Tau AB: new orbit, orbital parallax and component properties
Theta^2 Tauri is a detached and single-lined interferometric-spectroscopic
binary as well as the most massive binary system of the Hyades cluster. The
system revolves in an eccentric orbit with a periodicity of 140.7 days. The
secondary has a similar temperature but is less evolved and fainter than the
primary. It is also rotating more rapidly. Since the composite spectra are
heavily blended, the direct extraction of radial velocities over the orbit of
component B was hitherto unsuccessful. Using high-resolution spectroscopic data
recently obtained with the Elodie (OHP, France) and Hermes (ORM, La Palma,
Spain) spectrographs, and applying a spectra disentangling algorithm to three
independent data sets including spectra from the Oak Ridge Observatory (USA),
we derived an improved spectroscopic orbit and refined the solution by
performing a combined astrometric-spectroscopic analysis based on the new
spectroscopy and the long-baseline data from the Mark III optical
interferometer. As a result, the velocity amplitude of the fainter component is
obtained in a direct and objective way. Major progress based on this new
determination includes an improved computation of the orbital parallax. Our
mass ratio is in good agreement with the older estimates of Peterson et al.
(1991, 1993), but the mass of the primary is 15-25% higher than the more recent
estimates by Torres et al. (1997) and Armstrong et al. (2006). Due to the
strategic position of the components in the turnoff region of the cluster,
these new determinations imply stricter constraints for the age and the
metallicity of the Hyades cluster. The location of component B can be explained
by current evolutionary models, but the location of the more evolved component
A is not trivially explained and requires a detailed abundance analysis of its
disentangled spectrum.Comment: in press, 13 pages, 10 Postscript figures, 5 tables. Table~4 is
available as online material. Keywords: astrometry - techniques: high angular
resolution - stars: binaries: visual - stars: binaries: spectroscopic -
stars: fundamental parameter
Hot stars observed by XMM-Newton I. The catalog and the properties of OB stars
Aims : Following the advent of increasingly sensitive X-ray observatories,
deep observations of early-type stars became possible. However, the results for
only a few objects or clusters have until now been reported and there has been
no large survey comparable to that based upon the ROSAT All-Sky Survey (RASS).
Methods : A limited survey of X-ray sources, consisting of all public XMM
observations (2XMMi) and slew survey data (XMMSL1), is now available. The X-ray
counterparts to hot, massive stars have been searched for in these catalogs.
Results : About 300 OB stars were detected with XMM. Half of them were bright
enough for a spectral analysis to be possible, and we make available the
detailed spectral properties that were derived. The X-ray spectra of O stars
are represented well by low (<1keV) temperature components and seem to indicate
that an absorption column is present in addition to the interstellar
contribution. The X-ray fluxes are well correlated with the bolometric fluxes,
with a scatter comparable to that of the RASS studies and thus larger than
found previously with XMM for some individual clusters. These results contrast
with those of B stars that exhibit a large scatter in the L_X-L_BOL relation,
no additional absorption being found, and the fits indicate a plasma at higher
temperatures. Variability (either within one exposure or between multiple
exposures) was also investigated whenever possible: short-term variations are
far more rare than long-term ones (the former affects a few percent of the
sample, while the latter concerns between one third and two thirds of the
sources). Conclusions : This paper presents the results of the first
high-sensitivity investigation of the overall high-energy properties of a
sizable sample of hot stars.Comment: 10 pages, 4 figures, accepted for publication by A&
Masses of the components of SB2 binaries observed with Gaia. II. Masses derived from PIONIER interferometric observations for Gaia validation
In anticipation of the Gaia astrometric mission, a sample of spectroscopic
binaries is being observed since 2010 with the Sophie spectrograph at the
Haute--Provence Observatory. Our aim is to derive the orbital elements of
double-lined spectroscopic binaries (SB2s) with an accuracy sufficient to
finally obtain the masses of the components with relative errors as small as 1
% when combined with Gaia astrometric measurements. In order to validate the
masses derived from Gaia, interferometric observations are obtained for three
SB2s in our sample with F-K components: HIP 14157, HIP 20601 and HIP 117186.
The masses of the six stellar components are derived. Due to its edge-on
orientation, HIP 14157 is probably an eclipsing binary. We note that almost all
the derived masses are a few percent larger than the expectations from the
standard spectral-type-mass calibration and mass-luminosity relation. Our
calculation also leads to accurate parallaxes for the three binaries, and the
Hipparcos parallaxes are confirmed.Comment: 10 pages, 3 figures, accepted by MNRA
The interface between the stellar wind and interstellar medium around R Cassiopeiae revealed by far-infrared imaging
The circumstellar dust shells of intermediate initial-mass (about 1 to 8
solar masses) evolved stars are generated by copious mass loss during the
asymptotic giant branch phase. The density structure of their circumstellar
shell is the direct evidence of mass loss processes, from which we can
investigate the nature of mass loss. We used the AKARI Infrared Astronomy
Satellite and the Spitzer Space Telescope to obtain the surface brightness maps
of an evolved star R Cas at far-infrared wavelengths, since the temperature of
dust decreases as the distance from the star increases and one needs to probe
dust at lower temperatures, i.e., at longer wavelengths. The observed shell
structure and the star's known proper motion suggest that the structure
represents the interface regions between the dusty wind and the interstellar
medium. The deconvolved structures are fitted with the analytic bow shock
structure to determine the inclination angle of the bow shock cone. Our data
show that (1) the bow shock cone of 1 - 5 x 10^-5 solar masses (dust mass) is
inclined at 68 degrees with respect to the plane of the sky, and (2) the dust
temperature in the bow shock cone is raised to more than 20 K by collisional
shock interaction in addition to the ambient interstellar radiation field. By
comparison between the apex vector of the bow shock and space motion vector of
the star we infer that there is a flow of interstellar medium local to R Cas
whose flow velocity is at least 55.6 km/s, consistent with an environment
conducive to dust heating by shock interactions.Comment: 7 pages, 2 figures, accepted for publication in Astronomy and
Astrophysic
Tracing the young massive high-eccentricity binary system Theta 1 Orionis C through periastron passage
The nearby high-mass star binary system Theta 1 Orionis C is the brightest
and most massive of the Trapezium OB stars at the core of the Orion Nebula
Cluster, and it represents a perfect laboratory to determine the fundamental
parameters of young hot stars and to constrain the distance of the Orion
Trapezium Cluster. Between January 2007 and March 2008, we observed T1OriC with
VLTI/AMBER near-infrared (H- and K-band) long-baseline interferometry, as well
as with bispectrum speckle interferometry with the ESO 3.6m and the BTA 6m
telescopes (B'- and V'-band). Combining AMBER data taken with three different
3-telescope array configurations, we reconstructed the first VLTI/AMBER
closure-phase aperture synthesis image, showing the T1OriC system with a
resolution of approx. 2 mas. To extract the astrometric data from our
spectrally dispersed AMBER data, we employed a new algorithm, which fits the
wavelength-differential visibility and closure phase modulations along the H-
and K-band and is insensitive to calibration errors induced, for instance, by
changing atmospheric conditions. Our new astrometric measurements show that the
companion has nearly completed one orbital revolution since its discovery in
1997. The derived orbital elements imply a short-period (P=11.3 yrs) and
high-eccentricity orbit (e=0.6) with periastron passage around 2002.6. The new
orbit is consistent with recently published radial velocity measurements, from
which we can also derive the first direct constraints on the mass ratio of the
binary components. We employ various methods to derive the system mass
(M_system=44+/-7 M_sun) and the dynamical distance (d=410+/-20 pc), which is in
remarkably good agreement with recently published trigonometric parallax
measurements obtained with radio interferometry.Comment: 15 pages, 15 figures, accepted by A&
Deposition of nanoscale multilayer CrN/NbN physical vapor deposition coatings by high power impulse magnetron sputtering
Nanoscale multilayer CrN/NbN physical vapor deposition (PVD) coatings are gaining reputation for their high corrosion and wear resistance. However, the CrN/NbN films deposited by ABS(TM) (are bond sputtering) technology have some limitations such as macrodroplets, porosity, and less dense structures. The novel HIPIMS (high power impulse magnetron sputtering) technique produces macroparticle-free, highly ionized metal plasma, which brings advantages in both surface pretreatment and coating deposition stages of the PVD process. In this study, nanoscale multilayer CrN/NbN PVD coatings were pretreated and deposited with HIPIMS technology and compared with those deposited by HIPIMS-UBM (unbalanced magnetron) and by the ABSTM technique. In all cases Cr+ etching was utilized to enhance adhesion by low energy ion implantation. The coatings were deposited at 400 degrees C with substrate biased (Ub) at -75 V. During coating deposition, HIPIMS produced significantly high activation of nitrogen compared to the UBM as observed with mass spectroscopy. HIPIMS-deposited coatings revealed a bilayer period of 4.1 nm (total thickness: 2.9 mu m) and hardness of 3025 HK0.025. TEM results revealed droplet free, denser microstructure with (200) preferred orientation for the HIPIMS coating owing to the increased ionization as compared to the more porous structure with random orientation observed in UBM coating. The dry sliding wear coefficient (K-c) of the coating was 1.8 X 10(-15) m(3) N-1 m(-1), whereas the steady state coefficient of friction was 0.32. Potentiodynamic polarization tests revealed higher E-corr values, higher pitting resistance (around potentials +400 to +600 mV), and lower. corrosion current densities for HIPIMS deposited coatings as compared to the coatings deposited by ABS or HIPIMS-UBM. The corrosion behavior of the coatings qualitatively improved with the progressive use of HIPIMS from pretreatment stage to the coating deposition step. (C) 2008 American Vacuum Society
Visual/infrared interferometry of Orion Trapezium stars: Preliminary dynamical orbit and aperture synthesis imaging of the Theta 1 Orionis C system
Located in the Orion Trapezium cluster, Theta 1 Orionis C is one of the
youngest and nearest high-mass stars (O5-O7) and also known to be a close
binary system. Using new multi-epoch visual and near-infrared bispectrum
speckle interferometric observations obtained at the BTA 6 m telescope, and
IOTA near-infrared long-baseline interferometry, we trace the orbital motion of
the Theta 1 Ori C components over the interval 1997.8 to 2005.9, covering a
significant arc of the orbit. Besides fitting the relative position and the
flux ratio, we apply aperture synthesis techniques to our IOTA data to
reconstruct a model-independent image of the Theta 1 Ori C binary system.
The orbital solutions suggest a high eccentricity (e approx. 0.91) and
short-period (P approx. 10.9 yrs) orbit. As the current astrometric data only
allows rather weak constraints on the total dynamical mass, we present the two
best-fit orbits. From these orbital solutions one can be favoured, implying a
system mass of 48 M_sun and a distance to the Trapezium cluster of 434 pc. When
also taking the measured flux ratio and the derived location in the HR-diagram
into account, we find good agreement for all observables, assuming a spectral
type of O5.5 for Theta 1 Ori C1 (M=34.0 M_sun) and O9.5 for C2 (M=15.5 M_sun).
We find indications that the companion C2 is massive itself, which makes it
likely that its contribution to the intense UV radiation field of the Trapezium
cluster is non-negligible. Furthermore, the high eccentricity of the
preliminary orbit solution predicts a very small physical separation during
periastron passage (approx. 1.5 AU, next passage around 2007.5), suggesting
strong wind-wind interaction between the two O stars.Comment: 13 pages, 9 figures, Accepted for publication in Astronomy &
Astrophysic
On the Corrosion Resistance of Porous Electroplated Zinc Coatings in Different Corrosive Media
The corrosion resistance of an electroplated (EP) Zn coating whose surface
was chemically etched to produce surface defects (pores) is investigated in
this work. Impedance and DC polarisation measururements were employed to study
the behaviour of such coating in various corrosive media (NaCl, NaOH and rain
water). Four different faradaic relaxation processes were clearly revealed in
different NaCl concentrations (from 0.1M to 1M). In the most concentrated
solutions at least three relaxation processes at low frequencies (LF) appeared
and were related to zinc deposition and dissolution. At lower concentrations
and depending on the pH, only one process was observed. The charge transfer
resistance (Rct) and the corrosion current (Icorr) were practically stable in
the pH range 5 to 10. In deaerated NaCl 0.1M, the EIS diagrams showed two
time-constants at very close frequencies. From the EIS diagrams the porous
nature of the coating was highlighted and showed that the dissolution
mechanisms occurred at the base of the pores
Abundances of neutron-capture elements in G 24-25. A halo-population CH subgiant
The differences between the neutron-capture element abundances of halo stars
are important to our understanding of the nucleosynthesis of elements heavier
than the iron group. We present a detailed abundance analysis of carbon and
twelve neutron-capture elements from Sr up to Pb for a peculiar halo star
G24-25 with [Fe/H] = -1.4 in order to probe its origin. The equivalent widths
of unblended lines are measured from high resolution NOT/FIES spectra and used
to derive abundances based on Kurucz model atmospheres. In the case of CH, Pr,
Eu, Gd, and Pb lines, the abundances are derived by fitting synthetic profiles
to the observed spectra. Abundance analyses are performed both relative to the
Sun and to a normal halo star G16-20 that has similar stellar parameters as
G24-25. We find that G24-25 is a halo subgiant star with an unseen component.
It has large overabundances of carbon and heavy s-process elements and mild
overabundances of Eu and light s-process elements. This abundance distribution
is consistent with that of a typical CH giant. The abundance pattern can be
explained by mass transfer from a former asymptotic giant branch component,
which is now a white dwarf.Comment: 11 pages, 9 figures, accepted for publication in A&
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