77 research outputs found
Chemical abundances of fast-rotating massive stars. I. Description of the methods and individual results
Aims: Recent observations have challenged our understanding of rotational
mixing in massive stars by revealing a population of fast-rotating objects with
apparently normal surface nitrogen abundances. However, several questions have
arisen because of a number of issues, which have rendered a reinvestigation
necessary; these issues include the presence of numerous upper limits for the
nitrogen abundance, unknown multiplicity status, and a mix of stars with
different physical properties, such as their mass and evolutionary state, which
are known to control the amount of rotational mixing. Methods: We have
carefully selected a large sample of bright, fast-rotating early-type stars of
our Galaxy (40 objects with spectral types between B0.5 and O4). Their
high-quality, high-resolution optical spectra were then analysed with the
stellar atmosphere modelling codes DETAIL/SURFACE or CMFGEN, depending on the
temperature of the target. Several internal and external checks were performed
to validate our methods; notably, we compared our results with literature data
for some well-known objects, studied the effect of gravity darkening, or
confronted the results provided by the two codes for stars amenable to both
analyses. Furthermore, we studied the radial velocities of the stars to assess
their binarity. Results: This first part of our study presents our methods and
provides the derived stellar parameters, He, CNO abundances, and the
multiplicity status of every star of the sample. It is the first time that He
and CNO abundances of such a large number of Galactic massive fast rotators are
determined in a homogeneous way.Comment: accepted for publication by A&
High-resolution X-ray spectroscopy of the magnetic Of?p star HD148937
High-resolution data of the peculiar magnetic massive star HD148937 were
obtained with Chandra-HETGS, and are presented here in combination with a
re-analysis of the older XMM-RGS data. The lines of the high-Z elements (Mg,
Si, S) were found to be unshifted and relatively narrow (FWHM of about
800km/s), i.e. narrower than the O line recorded by RGS, which possibly
indicates that the hot plasma is multi-thermal and has several origins. These
data further indicate a main plasma temperature of about 0.6keV and a formation
of the X-ray emission at about one stellar radius above the photosphere. From
the spectral fits and the H-to-He line ratios, the presence of very hot plasma
is however confirmed, though with a smaller relative strength than for the
prototype magnetic oblique rotator \,Ori\,C. Both stars thus share
many similarities, but HD148937 appears less extreme than \,Ori\,C
despite having also a large magnetic confinement parameter.Comment: 13 pages, accepted for publication by Ap
First constraints on the magnetic field strength in extra-Galactic stars: FORS2 observations of Of?p stars in the Magellanic Clouds
Massive O-type stars play a dominant role in our Universe, but many of their
properties remain poorly constrained. In the last decade magnetic fields have
been detected in all Galactic members of the distinctive Of?p class, opening
the door to a better knowledge of all O-type stars. With the aim of extending
the study of magnetic massive stars to nearby galaxies, to better understand
the role of metallicity in the formation of their magnetic fields and
magnetospheres, and to broaden our knowledge of the role of magnetic fields in
massive star evolution, we have carried out spectropolarimetry of five
extra-Galactic Of?p stars, as well as a couple of dozen neighbouring stars. We
have been able to measure magnetic fields with typical error bars from 0.2 to
1.0 kG, depending on the apparent magnitude and on weather conditions. No
magnetic field has been firmly detected in any of our measurements, but we have
been able to estimate upper limits to the field values of our target stars. One
of our targets, 2dFS 936, exhibited an unexpected strengthening of emission
lines. We confirm the unusual behaviour of BI 57, which exhibits a 787 d period
with two photometric peaks and one spectroscopic maximum. The observed
strengthening of the emission lines of 2dFS 936, and the lack of detection of a
strong magnetic field in a star with such strong emission lines is at odd with
expectations. Together with the unusual periodic behaviour of BI 57, it
represents a challenge for the current models of Of?p stars. The limited
precision that we obtained in our field measurements (in most cases as a
consequence of poor weather) has led to field-strength upper limits that are
substantially larger than those typically measured in Galactic magnetic O
stars. Further higher precision observations and monitoring are clearly
required.Comment: Accepted by A&
How unique is Plaskett's star? A search for organized magnetic fields in short period, interacting or post-interaction massive binary systems
Amongst O-type stars with detected magnetic fields, the fast rotator in the
close binary called Plaskett's star shows a variety of unusual properties.
Since strong binary interactions are believed to have occurred in this system,
one may wonder about their potential role in generating magnetic fields. Stokes
V spectra collected with the low-resolution FORS2 and high-resolution ESPaDOnS
and Narval spectropolarimeters were therefore used to search for magnetic
fields in 15 interacting or post-interaction massive binaries. No magnetic
field was detected in any of them, with 0G always being within 2sigma of the
derived values. For 17 out of 25 stars in the systems observed at
high-resolution, the 90% upper limit on the individual dipolar fields is below
the dipolar field strength of Plaskett's secondary; a similar result is found
for five out of six systems observed at low resolution. If our sample is
considered to form a group of stars sharing similar magnetic properties, a
global statistical analysis results in a stringent upper limit of ~200G on the
dipolar field strength. Moreover, the magnetic incidence rate in the full
sample of interacting or post-interaction systems (our targets + Plaskett's
star) is compatible with that measured from large surveys, showing that they
are not significantly different from the general O-star population. These
results suggest that binary interactions play no systematic role in the
magnetism of such massive systems.Comment: 11 pages, accepted for publication in MNRA
Validation of the performance of a GMO multiplex screening assay based on microarray detection
A new screening method for the detection and identification of GMO, based on the use of multiplex PCR followed by microarray, has been developed and is presented. The technology is based on the identification of quite ubiquitous GMO genetic target elements first amplified by PCR, followed by direct hybridisation of the amplicons on a predefined microarray (DualChip® GMO, Eppendorf, Germany). The validation was performed within the framework of a European project (Co-Extra, contract no 007158) and in collaboration with 12 laboratories specialised in GMO detection. The present study reports the strategy and the results of an ISO complying validation of the method carried out through an inter-laboratory study. Sets of blind samples were provided consisting of DNA reference materials covering all the elements detectable by specific probes present on the array. The GMO concentrations varied from 1% down to 0.045%. In addition, a mixture of two GMO events (0.1% RRS diluted in 100% TOPAS19/2) was incorporated in the study to test the robustness of the assay in extreme conditions. Data were processed according to ISO 5725 standard. The method was evaluated with predefined performance criteria with respect to the EC CRL method acceptance criteria. The overall method performance met the acceptance criteria; in particular, the results showed that the method is suitable for the detection of the different target elements at 0.1% concentration of GMO with a 95% accuracy rate. This collaborative trial showed that the method can be considered as fit for the purpose of screening with respect to its intra- and inter-laboratory accuracy. The results demonstrated the validity of combining multiplex PCR with array detection as provided by the DualChip® GMO (Eppendorf, Germany) for the screening of GMO. The results showed that the technology is robust, practical and suitable as a screening too
An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H II Region W4
We present deep wide-field optical CCD photometry and mid-infrared
Spitzer/IRAC and MIPS 24micron data for about 100,000 stars in the young open
cluster IC 1805. The members of IC 1805 were selected from their location in
the various color-color and color-magnitude diagrams, and the presence of
Halpha emission, mid-infrared excess emission, and X-ray emission. The
reddening law toward IC 1805 is nearly normal (R_V = 3.05+/-0.06). However, the
distance modulus of the cluster is estimated to be 11.9+/-0.2 mag (d =
2.4+/-0.2 kpc) from the reddening-free color-magnitude diagrams, which is
larger than the distance to the nearby massive star-forming region W3(OH)
measured from the radio VLBA astrometry. We also determined the age of IC 1805
(tau_MSTO = 3.5 Myr). In addition, we critically compared the age and mass
scale from two pre-main-sequence evolution models. The initial mass function
with a Salpeter-type slope of Gamma = -1.3+/-0.2 was obtained and the total
mass of IC 1805 was estimated to be about 2700+/-200 M_sun. Finally, we found
our distance determination to be statistically consistent with the Tycho-Gaia
Astrometric Solution Data Release 1, within the errors. The proper motion of
the B-type stars shows an elongated distribution along the Galactic plane,
which could be explained by some of the B-type stars being formed in small
clouds dispersed by previous episodes of star formation or supernova
explosions.Comment: 45 pages, 32 figures, 9 tables, accepted for publication in ApJ
Investigating the Magnetospheres of Rapidly Rotating B-type Stars
Recent spectropolarimetric surveys of bright, hot stars have found that ~10%
of OB-type stars contain strong (mostly dipolar) surface magnetic fields (~kG).
The prominent paradigm describing the interaction between the stellar winds and
the surface magnetic field is the magnetically confined wind shock (MCWS)
model. In this model, the stellar wind plasma is forced to move along the
closed field loops of the magnetic field, colliding at the magnetic equator,
and creating a shock. As the shocked material cools radiatively it will emit
X-rays. Therefore, X-ray spectroscopy is a key tool in detecting and
characterizing the hot wind material confined by the magnetic fields of these
stars. Some B-type stars are found to have very short rotational periods. The
effects of the rapid rotation on the X-ray production within the magnetosphere
have yet to be explored in detail. The added centrifugal force due to rapid
rotation is predicted to cause faster wind outflows along the field lines,
leading to higher shock temperatures and harder X-rays. However, this is not
observed in all rapidly rotating magnetic B-type stars. In order to address
this from a theoretical point of view, we use the X-ray Analytical Dynamical
Magnetosphere (XADM) model, originally developed for slow rotators, with an
implementation of new rapid rotational physics. Using X-ray spectroscopy from
ESA's XMM-Newton space telescope, we observed 5 rapidly rotating B-type stars
to add to the previous list of observations. Comparing the observed X-ray
luminosity and hardness ratio to that predicted by the XADM allows us to
determine the role the added centrifugal force plays in the magnetospheric
X-ray emission of these stars.Comment: IAUS Conference Proceeding
Extreme mass ratios and fast rotation in three massive binaries
The origin of rapid rotation in massive stars remains debated, although
binary interactions are now often advocated as a cause. However, the broad and
shallow lines in the spectra of fast rotators make direct detection of binarity
difficult. In this paper, we report on the discovery and analysis of
multiplicity for three fast-rotating massive stars: HD25631 (B3V), HD191495
(B0V), and HD46485 (O7V). They display strikingly similar TESS light curves,
with two narrow eclipses superimposed on a sinusoidal variation due to
reflection effects. We complement these photometric data by spectroscopy from
various instruments (X-Shooter, Espadons, FUSE...), to further constrain the
nature of these systems. The detailed analyses of these data demonstrates that
the companions of the massive OB stars have low masses (~1Msol) with rather
large radii (2-4 Rsol) and low temperatures (<15 kK). These companions display
no UV signature, which would exclude a hot subdwarf nature, but disentangling
of the large set of X-Shooter spectra of HD25631 revealed the typical signature
of chromospheric activity in the companion's spectrum. In addition, despite the
short orbital periods (P=3-7d), the fast-rotating OB-stars still display
non-synchronized rotation and all systems appear young (<20Myr). This suggests
that, as in a few other cases, these massive stars are paired in those systems
with non-degenerate, low-mass PMS companions, implying that fast rotation would
not be a consequence of a past binary interactions in their case.Comment: accepted for publication by MNRA
X-ray emission from the double-binary OB-star system QZ Car (HD 93206)
X-ray observations of the double-binary OB-star system QZ Car (HD 93206)
obtained with the Chandra X-ray Observatory over a period of roughly 2 years
are presented. The orbit of systems A (O9.7 I+b2 v, PA = 21 d) and B (O8 III+o9
v, PB = 6 d) are reasonably well sampled by the observations, allowing the
origin of the X-ray emission to be examined in detail. The X-ray spectra can be
well fitted by an attenuated three temperature thermal plasma model,
characterised by cool, moderate, and hot plasma components at kT ~ 0.2, 0.7,
and 2 keV, respectively, and a circumstellar absorption of ~ 0.2 x 10^22 cm-2.
Although the hot plasma component could be indicating the presence of wind-wind
collision shocks in the system, the model fluxes calculated from spectral fits,
with an average value of ~ 7 x 10^-13 erg s-1 cm-2, do not show a clear
correlation with the orbits of the two constituent binaries. A semi-analytical
model of QZ Car reveals that a stable momentum balance may not be established
in either system A or B. Yet, despite this, system B is expected to produce an
observed X-ray flux well in excess of the observations. If one considers the
wind of the O8 III star to be disrupted by mass transfer the model and
observations are in far better agreement, which lends support to the previous
suggestion of mass-transfer in the O8 III + o9 v binary. We conclude that the
X-ray emission from QZ Car can be reasonably well accounted for by a
combination of contributions mainly from the single stars and the mutual
wind-wind collision between systems A and B.Comment: 11 pages, 7 figures. Accepted for the ApJS Special Issue on the
Chandra Carina Complex Project (CCCP), scheduled for publication in May 2011.
All 16 CCCP Special Issue papers are available at
http://cochise.astro.psu.edu/Carina_public/special_issue.html through 2011 at
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