1,321 research outputs found
High-resolution X-ray spectroscopy reveals the special nature of Wolf-Rayet star winds
We present the first high-resolution X-ray spectrum of a putatively single
Wolf-Rayet star. 400 ks observations of WR 6 by the XMM-Newton-telescope
resulted in a superb quality high-resolution X-ray spectrum. Spectral analysis
reveals that the X-rays originate far out in the stellar wind, more than 30
stellar radii from the photosphere, and thus outside the wind acceleration zone
where the line-driving instability could create shocks. The X-ray emitting
plasma reaches temperatures up to 50\,MK, and is embedded within the
un-shocked, "cool" stellar wind as revealed by characteristic spectral
signatures. We detect a fluorescent Fe line at approx 6.4 keV. The presence of
fluorescence is consistent with a two-component medium, where the cool wind is
permeated with the hot X-ray emitting plasma. The wind must have a very porous
structure to allow the observed amount of X-rays to escape. We find that
neither the line-driving instability nor any alternative binary scenario can
explain the data. We suggest a scenario where X-rays are produced when the fast
wind rams into slow "sticky clumps" that resist acceleration. Our new data show
that the X-rays in single WR-star are generated by some special mechanism
different from the one operating in the O-star winds.Comment: ApJL, Figure 3 is update
X-ray Emission from Nitrogen-Type Wolf-Rayet Stars
We summarize new X-ray detections of four nitrogen-type Wolf-Rayet (WR) stars
obtained in a limited survey aimed at establishing the X-ray properties of WN
stars across their full range of spectral subtypes. None of the detected stars
is so far known to be a close binary. We report Chandra detections of WR 2
(WN2), WR 18 (WN4), and WR 134 (WN6), and an XMM-Newton detection of WR79a
(WN9ha). These observations clearly demonstrate that both WNE and WNL stars are
X-ray sources. We also discuss Chandra archive detections of the WN6h stars WR
20b, WR 24, and WR 136 and ROSAT non-detections of WR 16 (WN8h) and WR 78
(WN7h). The X-ray spectra of all WN detections show prominent emission lines
and an admixture of cool (kT 2 keV) plasma. The hotter
plasma is not predicted by radiative wind shock models and other as yet
unidentified mechanisms are at work. Most stars show X-ray absorption in excess
of that expected from visual extinction (Av), likely due to their strong winds
or cold circumstellar gas. Existing data suggest a falloff in X-ray luminosity
toward later WN7-9 subtypes, which have higher Lbol but slower, denser winds
than WN2-6 stars. This provides a clue that wind properties may be a more
crucial factor in determining emergent X-ray emission levels than bolometric
luminosity.Comment: 42 pages, 5 tables, 10 figure
X-rays from Colliding Stellar Winds: the case of close WR+O binary systems
We have analysed the X-ray emission from a sample of close WR+O binaries
using data from the public Chandra and XMM-Newton archives. Global spectral
fits show that two-temperature plasma is needed to match the X-ray emission
from these objects as the hot component (kT > 2 keV) is an important ingredient
of the spectral models. In close WR+O binaries, X-rays likely originate in
colliding stellar wind (CSW) shocks driven by the massive winds of the binary
components. CSW shocks in these objects are expected to be radiative due to the
high density of the plasma in the interaction region. Opposite to this, our
analysis shows that the CSW shocks in the sample of close WR+O binaries are
adiabatic. This is possible only if the mass-loss rates of the stellar
components in the binary are at least one order of magnitude smaller than the
values currently accepted. The most likely explanation for the X-ray properties
of close WR+O binaries could be that their winds are two-component flows. The
more massive component (dense clumps) play role for the optical/UV emission
from these objects, while the smooth rarefied component is a key factor for
their X-ray emission.Comment: MNRAS, accepted for publication (Feb 6, 2012); 13 pages, 6 figures, 3
table
New Constraints on the Origin of the Short-Term Cyclical Variability of the Wolf-Rayet Star WR 46
The Wolf-Rayet star WR 46 is known to exhibit a very complex variability
pattern on relatively short time scales of a few hours. Periodic but
intermittent radial velocity shifts of optical lines as well as multiple
photometric periods have been found in the past. Non-radial pulsations, rapid
rotational modulation or the presence of a putative low-mass companion have
been proposed to explain the short-term behaviour. In an effort to unveil its
true nature, we observed WR 46 with FUSE (Far Ultraviolet Spectroscopic
Explorer) over several short-term variability cycles. We found significant
variations on a time scale of ~8 hours in the far-ultraviolet (FUV) continuum,
in the blue edge of the absorption trough of the OVI {\lambda}{\lambda}1032,
1038 doublet P Cygni profile and in the SVI {\lambda}{\lambda}933, 944 P Cygni
absorption profile. We complemented these observations with X-ray and UV
light-curves and an X-ray spectrum from archival XMM-Newton (X-ray Multi-Mirror
Mission - Newton Space Telescope) data. The X-ray and UV light-curves show
variations on a time scale similar to the variability found in the FUV. We
discuss our results in the context of the different scenarios suggested to
explain the short-term variability of this object and reiterate that non-radial
pulsations is the most likely to occur.Comment: 36 pages, 11 figures. Accepted for publication in Ap
WR 110: A Single Wolf-Rayet Star With Corotating Interaction Regions In Its Wind?
A 30-day contiguous photometric run with the MOST satellite on the WN5-6b
star WR 110 (HD 165688) reveals a fundamental periodicity of P = 4.08 +/- 0.55
days along with a number of harmonics at periods P/n, with n ~ 2,3,4,5 and 6,
and a few other possible stray periodicities and/or stochastic variability on
timescales longer than about a day. Spectroscopic RV studies fail to reveal any
plausible companion with a period in this range. Therefore, we conjecture that
the observed light-curve cusps of amplitude ~ 0.01 mag that recur at a 4.08 day
timescale may arise in the inner parts, or at the base of, a corotating
interaction region (CIR) seen in emission as it rotates around with the star at
constant angular velocity. The hard X-ray component seen in WR 110 could then
be a result of a high velocity component of the CIR shock interacting with the
ambient wind at several stellar radii. Given that most hot, luminous stars
showing CIRs have two CIR arms, it is possible that either the fundamental
period is 8.2 days or, more likely in the case of WR 110, there is indeed a
second weaker CIR arm for P = 4.08 days, that occurs ~ two thirds of a rotation
period after the main CIR. If this interpretation is correct, WR 110 therefore
joins the ranks with three other single WR stars, all WN, with confirmed CIR
rotation periods (WR 1, WR 6, and WR 134), albeit with WR 110 having by far the
lowest amplitude photometric modulation. This illustrates the power of being
able to secure intense, continuous high-precision photometry from space-based
platforms such as MOST. It also opens the door to revealing low-amplitude
photometric variations in other WN stars, where previous attempts have failed.
If all WN stars have CIRs at some level, this could be important for revealing
sources of magnetism or pulsation in addition to rotation periods.Comment: 25 pages, 8 figures, 2 tables, accepted in Ap
Multiple shells around G79.29+0.46 revealed from near-IR to millimeter data
Aiming to perform a study of the warm dust and gas in the luminous blue
variable star G79.29+0.46 and its associated nebula, we present infrared
Spitzer imaging and spectroscopy, and new CO J=2-->1 and 4-->3 maps obtained
with the IRAM 30m radio telescope and with the Submillimeter Telescope,
respectively. We have analyzed the nebula detecting multiple shells of dust and
gas connected to the star. Using Infrared Spectrograph-Spitzer spectra, we have
compared the properties of the central object, the nebula, and their
surroundings. These spectra show a rich variety of solid-state features
(amorphous silicates, polycyclic aromatic hydrocarbons, and CO2 ices) and
narrow emission lines, superimposed on a thermal continuum. We have also
analyzed the physical conditions of the nebula, which point to the existence of
a photo-dissociation region.Comment: Received by ApJ 2009 November 20, accepted for publication 2010
February 25, Published 2010 March 2
Wind clumping and the wind-wind collision zone in the Wolf-Rayet binary gamma Velorum
We present XMM-Newton observations of gamma^2 Velorum (WR 11, WC8+O7.5III, P
= 78.53 d), a nearby Wolf-Ray binary system, at its X-ray high and low states.
At high state, emission from a hot collisional plasma dominates from about 1 to
8 keV. At low state, photons between 1 and 4 keV are absorbed. The hot plasma
is identified with the shock zone between the winds of the primary Wolf-Rayet
star and the secondary O giant. The absorption at low state is interpreted as
photoelectric absorption in the Wolf-Rayet wind. This absorption allows us to
measure the absorbing column density and to derive a mass loss rate 8x10^{-6}
M_sun/yr for the WC8 star. This mass loss rate, in conjunction with a previous
Wolf-Rayet wind model, provides evidence for a clumped WR wind. A clumping
factor of 16 is required. The X-ray spectra below 1 keV (12 Ang) show no
absorption and are essentially similar in both states. There is a rather clear
separation in that emission from a plasma hotter than 5 MK is heavily absorbed
in low state while the cooler plasma is not. This cool plasma must come from a
much more extended region than the hot material. The Neon abundance in the
X-ray emitting material is 2.5 times the solar value. The unexpected detection
of CV (25.3 Ang) and CVI (31.6 Ang) radiative recombination continua at both
phases indicates the presence of a cool (~40,000 K) recombination region
located far out in the binary system.Comment: 16 page
Challenges in the Analysis of Historic Concrete:Understanding the Limitations of Techniques, the Variability of the Material and the Importance of Representative Samples
Study protocol: can a school gardening intervention improve children's diets?
BACKGROUND: The current academic literature suggests there is a potential for using gardening as a tool to improve children's fruit and vegetable intake. This study is two parallel randomised controlled trials (RCT) devised to evaluate the school gardening programme of the Royal Horticultural Society (RHS) Campaign for School Gardening, to determine if it has an effect on children's fruit and vegetable intake. METHOD/DESIGN: Trial One will consist of 26 schools; these schools will be randomised into two groups, one to receive the intensive intervention as "Partner Schools" and the other to receive the less intensive intervention as "Associate Schools". Trial Two will consist of 32 schools; these schools will be randomised into either the less intensive intervention "Associate Schools" or a comparison group with delayed intervention. Baseline data collection will be collected using a 24-hour food diary (CADET) to collect data on dietary intake and a questionnaire exploring children's knowledge and attitudes towards fruit and vegetables. A process measures questionnaire will be used to assess each school's gardening activities. DISCUSSION: The results from these trials will provide information on the impact of the RHS Campaign for School Gardening on children's fruit and vegetable intake. The evaluation will provide valuable information for designing future research in primary school children's diets and school based interventions. TRIAL REGISTRATION: ISRCTN11396528
Eddy-mediated transport of warm Circumpolar Deep Water across the Antarctic Shelf Break
The Antarctic Slope Front (ASF) modulates ventilation of the abyssal ocean via the export of dense Antarctic Bottom Water (AABW) and constrains shoreward transport of warm Circumpolar Deep Water (CDW) toward marine-terminating glaciers. Along certain stretches of the continental shelf, particularly where AABW is exported, density surfaces connect the shelf waters to the middepth Circumpolar Deep Water offshore, offering a pathway for mesoscale eddies to transport CDW directly onto the continental shelf. Using an eddy-resolving process model of the ASF, the authors show that mesoscale eddies can supply a dynamically significant transport of heat and mass across the continental shelf break. The shoreward transport of surface waters is purely wind driven, while the shoreward CDW transport is entirely due to mesoscale eddy transfer. The CDW flux is sensitive to all aspects of the model's surface forcing and geometry, suggesting that shoreward eddy heat transport may be localized to favorable sections of the continental slope
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