243 research outputs found
Can an underestimation of opacity explain B-type pulsators in the SMC?
Slowly Pulsating B and Cephei are mechanism driven pulsating
B stars. That mechanism works since a peak in the opacity due to a
high number of atomic transitions from iron-group elements occurs in the area
of . Theoretical results predict very few SPBs and no
Cep to be encountered in low metallicity environments such as the Small
Magellanic Cloud. However recent variability surveys of B stars in the SMC
reported the detection of a significant number of SPB and Cep
candidates. Though the iron content plays a major role in the excitation of
Cep and SPB pulsations, the chemical mixture representative of the SMC
B stars such as recently derived does not leave room for a significant increase
of the iron abundance in these stars. Whilst abundance of iron-group elements
seems reliable, is the opacity in the iron-group elements bump underestimated?
We determine how the opacity profile in B-type stars should change to excite
SPB and Cep pulsations in early-type stars of the SMC.Comment: 5 pages, 7 figures, to appear under electronic form in : Proceedings
of the 4th HELAS International Conference: Seismological Challenges for
Stellar Structur
Symbol-asynchronous transmission in multibeam satellite user down-link : rate regions for novel superposition coding schemes
We consider the forward link of a multibeam satellite system with high spectral reuse and the novel low-complexity transmission and detection strategies from [1]. More specifically, we study the impact of a time offset between the antenna beams that cooperate to simultaneously serve a given user. Assuming Gaussian signaling, we provide closed-form expressions for the achievable rate region. It is demonstrated that, in the absence of timing information at the gateway, this region is not affected by a time offset. Our numerical results further show that, in case timing is known at the gateway, an offset of half a symbol period at both user terminals is optimal in terms of spectral efficiency.Grant numbers : Satellite Network of Experts IV. © 2018 IEEE. Personal use of this material is permitted. Permission from IEEE must be obtained for all other uses, in any current or future media, including reprinting/republishing this material for advertising or promotional purposes, creating new collective works, for resale or redistribution to servers or lists, or reuse of any copyrighted component of this work in other works
Non-coherent rate-splitting for multibeam satellite forward link : practical coding and decoding algorithms
Non-Coherent Rate-Splitting (NCRS) was recently proposed as a practical multiuser coding and decoding scheme to increase the spectral efficiency of multibeam satellite communication systems. In this paper, we further study the practical realization of NCRS. We propose a modified coding scheme (NCRS*) that is robust to a nonzero time offset among beams. In NCRS*, as opposed to NCRS, the beams send independently channel encoded and modulated waveforms. We assess the performance of NCRS* in terms of the achievable rate region. It is shown that NCRS* performs worse than NCRS, but better than or comparable to other competing schemes, which, as opposed to NCRS*, require flexible bandwidth allocation or perfect synchronization at the transmitter. We also propose a new N-MAP algorithm for the practical implementation of NCRS* receivers. Similar to the existing UMAP algorithm, N-MAP takes into account the modulation used by, and the time offset between, the signals received from the different beams. In most cases, however, N-MAP has a significantly lower complexity than U-MAP
An Apparatus to Measure the Thermal Conductivity of Graphite Near Room Temperature. EUR 3909.
Periodic mass loss episodes due to an oscillation mode with variable amplitude in the hot supergiant HD50064
We aim to interpret the photometric and spectroscopic variability of the
luminous blue variable supergiant HD\,50064 ().CoRoT space photometry
and follow-up high-resolution spectroscopy, with a time base of 137\,d and
169\,d, respectively, was gathered, analysed and interpreted using standard
time series analysis and light curve modelling methods as well as spectral line
diagnostics.The space photometry reveals one period of 37\,d, which undergoes a
sudden amplitude change with a factor 1.6. The pulsation period is confirmed in
the spectroscopy, which additionally reveals metal line radial velocity values
differing by km\,s depending on the spectral line and on the
epoch. We estimate \teff13\,500\,K, \logg1.5 from the equivalent
width of Si lines. The Balmer lines reveal that the star undergoes episodes of
changing mass loss on a time scale similar to the changes in the photometric
and spectroscopic variability, with an average value of (in M\,yr). We tentatively interpret the 37\,d
period as due to a strange mode oscillation.Comment: 4 pages, accepted for publication in Astronomy & Astrophysics Letter
Solar-like oscillations in a massive star
Seismology of stars provides insight into the physical mechanisms taking
place in their interior, with modes of oscillation probing different layers.
Low-amplitude acoustic oscillations excited by turbulent convection were
detected four decades ago in the Sun and more recently in low-mass
main-sequence stars. Using data gathered by the Convection Rotation and
Planetary Transits mission, we report here on the detection of solar-like
oscillations in a massive star, V1449 Aql, which is a known large-amplitude (b
Cephei) pulsator.Comment: Published in Sience, 19 June 2009, vol. 324, p. 154
Stellar ages and convective cores in field main-sequence stars: first asteroseismic application to two Kepler targets
Using asteroseismic data and stellar evolution models we make the first
detection of a convective core in a Kepler field main-sequence star, putting a
stringent constraint on the total size of the mixed zone and showing that extra
mixing beyond the formal convective boundary exists. In a slightly less massive
target the presence of a convective core cannot be conclusively discarded, and
thus its remaining main-sequence life time is uncertain. Our results reveal
that best-fit models found solely by matching individual frequencies of
oscillations corrected for surface effects do not always properly reproduce
frequency combinations. Moreover, slightly different criteria to define what
the best-fit model is can lead to solutions with similar global properties but
very different interior structures. We argue that the use of frequency ratios
is a more reliable way to obtain accurate stellar parameters, and show that our
analysis in field main-sequence stars can yield an overall precision of 1.5%,
4%, and 10% in radius, mass and age, respectively. We compare our results with
those obtained from global oscillation properties, and discuss the possible
sources of uncertainties in asteroseismic stellar modeling where further
studies are still needed.Comment: 46 pages, 10 figures, ApJ accepte
Core properties of alpha Cen A using asteroseismology
A set of long and nearly continuous observations of alpha Centauri A should
allow us to derive an accurate set of asteroseismic constraints to compare to
models, and make inferences on the internal structure of our closest stellar
neighbour. We intend to improve the knowledge of the interior of alpha Centauri
A by determining the nature of its core. We combined the radial velocity time
series obtained in May 2001 with three spectrographs in Chile and Australia:
CORALIE, UVES, and UCLES. The resulting combined time series has a length of
12.45 days and contains over 10,000 data points and allows to greatly reduce
the daily alias peaks in the power spectral window. We detected 44 frequencies
that are in good overall agreement with previous studies, and found that 14 of
these show possible rotational splittings. New values for the large and small
separations have been derived. A comparison with stellar models indicates that
the asteroseismic constraints determined in this study allows us to set an
upper limit to the amount of convective-core overshooting needed to model stars
of mass and metallicity similar to those of alpha Cen A.Comment: 8 pages, 11 figures, A&A accepte
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
Management of hepatocellular adenoma during pregnancy
Background & Aims: Hepatocellular adenoma in pregnant women requires special considerations because of the risk of hormone induced growth and rupture. To prevent these potential lethal complications, pregnancy is either often discouraged or the surgical resection of large adenomas is recommended. It may be questioned whether it is justified to deny a young woman a pregnancy, as the biological behaviour of hepatocellular adenoma may be less threatening than presumed. In this study we establish the management of hepatocellular adenoma during pregnancy based on our own experience and literature. Methods: Twelve women with documented hepatocellular adenoma were closely monitored during a total of 17 pregnancies between 2000 and 2009. Their files were reviewed. Results: In four cases, hepatocellular adenomas grew during pregnancy, requiring a Caesarean section in one patient (two pregnancies) at 36 and 34 weeks because of an assumed high risk of rupture. In one case radiofrequency ablation therapy was applied in the first trimester to treat a hormone sensitive hepatocellular adenoma, thereby excluding potential growth later in pregnancy. No intervention was performed in the other 14 cases and all pregnancies had an uneventful course with a successful maternal and fetal outcome. Conclusions: A "wait and see" management may be advocated in pregnant women presenting with a hepatocellular adenoma. In women with large tumours or in whom hepatocellular adenoma had complicated previous pregnancies, surgical resection may be recommended. In women with smaller adenomas it may no longer be necessary to discourage pregnancy
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