Continuous VM-ADCP (vessel-mounted acoustic Doppler current profiler) profiles of horizontal velocities and raw acoustic gain control data during Polarstern cruise ANT-XVIII/2

The mixing regime of the upper 180 m of a mesoscale eddy in the vicinity of the Antarctic Polar Front at 47° S and 21° E was investigated during the R.V. Polarstern cruise ANT-XVIII/2 within the scope of the iron fertilization experiment EisenEx. On the basis of hydrographic CTD and ADCP profiles we deduced the vertical diffusivity Kz from two different parameterizations. Since these parameterizations bear the character of empirical functions, based on theoretical and idealized assumptions, they were inter alia compared with Cox-number and Thorpe-scale related diffusivities deduced from microstructure measurements, which supplied the first direct insights into turbulence of this ocean region. Values of Kz in the range of 10**-4 - 10**-3 m**2/s appear as a rather robust estimate of vertical diffusivity within the seasonal pycnocline. Values in the mixed layer above are more variable in time and reach 10**-1 m**2/s during periods of strong winds. The results confirm a close agreement between the microstructure-based eddy diffusivities and eddy diffusivities calculated after the parameterization of Pacanowski and Philander [1981, Journal of Physical Oceanography 11, 1443-1451, doi:10.1175/1520-0485(1981)011<1443:POVMIN>2.0.CO;2].

The VLT-FLAMES Tarantula Survey: XVIII. Classifications and radial velocities of the B-type stars

We present spectral classifications for 438 B-type stars observed as part of the VLT-FLAMES Tarantula Survey (VFTS) in the 30 Doradus region of the Large Magellanic Cloud. Radial velocities are provided for 307 apparently single stars, and for 99 targets with radial-velocity variations which are consistent with them being spectroscopic binaries. We investigate the spatial distribution of the radial velocities across the 30 Dor region, and use the results to identify candidate runaway stars. Excluding potential runaways and members of two older clusters in the survey region (SL 639 and Hodge 301), we determine a systemic velocity for 30 Dor of 271.6 ± 12.2 km s^-1 from 273 presumed single stars. Employing a 3σ criterion we identify nine candidate runaway stars (2.9% of the single stars with radial-velocity estimates). The projected rotational velocities of the candidate runaways appear to be significantly different to those of the full B-type sample, with a strong preference for either large (≥345 km s^-1) or small (≤65 km s^-1) rotational velocities. Of the candidate runaways, VFTS 358 (classified B0.5: V) has the largest differential radial velocity (-106.9 ± 16.2 km s^-1), and a preliminary atmospheric analysis finds a significantly enriched nitrogen abundance of 12 + log (N/H) ≳ 8.5. Combined with a large rotational velocity (υ_e sin i = 345 ± 22 km s^-1), this is suggestive of past binary interaction for this star.

Rotational velocities of single and binary O-type stars in the Tarantula Nebula

Rotation is a key parameter in the evolution of massive stars, affecting their evolution, chemical yields, ionizing photon budget, and final fate. We determined the projected rotational velocity, υ e sin i, of ~330 O-type objects, i.e. ~210 spectroscopic single stars and ~110 primaries in binary systems, in the Tarantula nebula or 30 Doradus (30 Dor) region. The observations were taken using VLT/FLAMES and constitute the largest homogeneous dataset of multi-epoch spectroscopy of O-type stars currently available. The most distinctive feature of the υ e sin i distributions of the presumed-single stars and primaries in 30 Dor is a low-velocity peak at around 100 km s^-1. Stellar winds are not expected to have spun-down the bulk of the stars significantly since their arrival on the main sequence and therefore the peak in the single star sample is likely to represent the outcome of the formation process. Whereas the spin distribution of presumed-single stars shows a well developed tail of stars rotating more rapidly than 300 km s^-1, the sample of primaries does not feature such a high-velocity tail. The tail of the presumed-single star distribution is attributed for the most part - and could potentially be completely due - to spun-up binary products that appear as single stars or that have merged. This would be consistent with the lack of such post-interaction products in the binary sample, that is expected to be dominated by pre-interaction systems. The peak in this distribution is broader and is shifted toward somewhat higher spin rates compared to the distribution of presumed-single stars. Systems displaying large radial velocity variations, typical for short period systems, appear mostly responsible for these differences.

The VLT-FLAMES tarantula survey:XII. Rotational velocities of the single O-type stars

Context. The 30 Doradus (30 Dor) region of the Large Magellanic Cloud, also known as the Tarantula nebula, is the nearest starburst region. It contains the richest population of massive stars in the Local Group, and it is thus the best possible laboratory to investigate open questions on the formation and evolution of massive stars. Aims. Using ground-based multi-object optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS), we aim to establish the (projected) rotational velocity distribution for a sample of 216 presumably single O-type stars in 30 Dor. The sample is large enough to obtain statistically significant information and to search for variations among subpopulations - in terms of spectral type, luminosity class, and spatial location - in the field of view. Methods. We measured projected rotational velocities, 3e sin i, by means of a Fourier transform method and a profile fitting method applied to a set of isolated spectral lines. We also used an iterative deconvolution procedure to infer the probability density, P(3e), of the equatorial rotational velocity, 3e. Results. The distribution of 3e sin i shows a two-component structure: a peak around 80 km s1 and a high-velocity tail extending up to 600 km s^-1 This structure is also present in the inferred distribution P(3e) with around 80% of the sample having 0 <3e ≤ 300 km s^-1 and the other 20% distributed in the high-velocity region. The presence of the low-velocity peak is consistent with what has been found in other studies for late O- and early B-type stars. Conclusions. Most of the stars in our sample rotate with a rate less than 20% of their break-up velocity. For the bulk of the sample, mass loss in a stellar wind and/or envelope expansion is not efficient enough to significantly spin down these stars within the first few Myr of evolution. If massive-star formation results in stars rotating at birth with a large portion of their break-up velocities, an alternative braking mechanism, possibly magnetic fields, is thus required to explain the present-day rotational properties of the O-type stars in 30 Dor. The presence of a sizeable population of fast rotators is compatible with recent population synthesis computations that investigate the influence of binary evolution on the rotation rate of massive stars. Even though we have excluded stars that show significant radial velocity variations, our sample may have remained contaminated by post-interaction binary products. That the highvelocity tail may be populated primarily (and perhaps exclusively) by post-binary interaction products has important implications for the evolutionary origin of systems that produce gamma-ray bursts. © 2013 Author(s).

The VLT-FLAMES tarantula survey:X. Evidence for a bimodal distribution of rotational velocities for the single early B-type stars

Aims. Projected rotational velocities (ve sin i) have been estimated for 334 targets in the VLT-FLAMES Tarantula Survey that do not manifest significant radial velocity variations and are not supergiants. They have spectral types from approximately O9.5 to B3. The estimates have been analysed to infer the underlying rotational velocity distribution, which is critical for understanding the evolution of massive stars. Methods. Projected rotational velocities were deduced from the Fourier transforms of spectral lines, with upper limits also being obtained from profile fitting. For the narrower lined stars, metal and non-diffuse helium lines were adopted, and for the broader lined stars, both non-diffuse and diffuse helium lines; the estimates obtained using the different sets of lines are in good agreement. The uncertainty in the mean estimates is typically 4% for most targets. The iterative deconvolution procedure of Lucy has been used to deduce the probability density distribution of the rotational velocities. Results. Projected rotational velocities range up to approximately 450 kms-1 and show a bi-modal structure. This is also present in the inferred rotational velocity distribution with 25% of the sample having 0 <ve <100 km s^-1 and the high velocity component having v_e ∼ 250 km s^-1. There is no evidence from the spatial and radial velocity distributions of the two components that they represent either field and cluster populations or different episodes of star formation. Be-type stars have also been identified. Conclusions. The bi-modal rotational velocity distribution in our sample resembles that found for late-B and early-A type stars.While magnetic braking appears to be a possible mechanism for producing the low-velocity component, we can not rule out alternative explanations. © ESO 2013.

Crack propagation in non-homogenous materials: Evaluation of mixed-mode SIFs, T-stress and kinking angle using a variant EFG method

A new variant of the Element-Free Galerkin (EFG) method, that combines the diffraction method, to characterize the crack tip solution, and the Heaviside enrichment function for representing discontinuity due to a crack, has been used to model crack propagation through non-homogenous materials. In the case of interface crack propagation, the kink angle is predicted by applying the maximum tangential principal stress (MTPS) criterion in conjunction with consideration of the energy release rate (ERR). The MTPS criterion is applied to the crack tip stress field described by both the stress intensity factor (SIF) and the T-stress, which are extracted using the interaction integral method. The proposed EFG method has been developed and applied for 2D case studies involving a crack in an orthotropic material, crack along an interface and a crack terminating at a bi-material interface, under mechanical or thermal loading; this is done to demonstrate the advantages and efficiency of the proposed methodology. The computed SIFs, T-stress and the predicted interface crack kink angles are compared with existing results in the literature and are found to be in good agreement. An example of crack growth through a particle-reinforced composite materials, which may involve crack meandering around the particle, is reported.

La sécrétion de la protéine tau : mécanisme de propagation de la pathologie de tau dans la maladie d’Alzheimer.

Dans la maladie d’Alzheimer, il existe deux marqueurs histopathologiques : les plaques amyloïdes composées de la protéine amyloïde-bêta et les enchevêtrements neurofibrillaires (NFTs) composés de la protéine tau agrégée. Dans le cerveau, la propagation de la pathologie de tau est observée le long des circuits neuronaux connectés synaptiquement, selon une séquence de stades, caractérisés par le Docteur Braak en 1991. Chez les patients, le degré de démence corrèle avec le nombre de NFTs. Ces derniers apparaissent dans des régions précises du cerveau et se propagent, de manière prédictible, le long des projections neuronales à des stades plus tardifs de la pathologie. Il reste à éclaircir la manière dont les NFTs se propagent dans les différentes régions du cerveau. Dans notre laboratoire, nous avons émis l’hypothèse que la propagation de tau pourrait se produire par un processus de transmission de cellule à cellule. Ainsi, la protéine tau serait tout d’abord sécrétée par un neurone, puis endocytée par un neurone adjacent. Nos travaux de recherche se sont concentrés sur la sécrétion de la protéine tau. Dans une première étape, nous avons démontré l’existence de la sécrétion active de tau dans l’espace extracellulaire, en utilisant des modèles in vitro de cellules non neuronales et neuronales. Par la suite, nous avons caractérisé les formes de protéines tau sécrétées. Enfin dans un dernier temps, nous avons exploré les voies de sécrétion de la protéine tau ainsi que les mécanismes régulant ce phénomène. Nous avons réussi à moduler la sécrétion de tau en reproduisant plusieurs insultes observées dans la maladie d’Alzheimer. Nos recherches nous ont permis d’identifier l’appareil de Golgi comme étant une organelle dont la fragmentation augmente la sécrétion de la protéine tau. A la lumière de cette découverte, nous avons été capable de moduler la sécrétion de tau en ciblant spécifiquement l’activité de cdk5 et l’expression de rab1A contrôlant la morphologie du Golgi. Ainsi, nous avons réussi à diminuer significativement la sécrétion de la protéine tau. Nos travaux de recherche proposent de nouvelles cibles thérapeutiques pour la maladie d’Alzheimer, visant à diminuer la propagation de la pathologie de tau par de nouveaux mécanismes cellulaires.

Numerical Simulation Of Ultrasonic Wave Propagation In Elastically Anisotropic Media

The ultrasonic non-destructive testing of components may encounter considerable difficulties to interpret some inspections results mainly in anisotropic crystalline structures. A numerical method for the simulation of elastic wave propagation in homogeneous elastically anisotropic media, based on the general finite element approach, is used to help this interpretation. The successful modeling of elastic field associated with NDE is based on the generation of a realistic pulsed ultrasonic wave, which is launched from a piezoelectric transducer into the material under inspection. The values of elastic constants are great interest information that provide the application of equations analytical models, until small and medium complexity problems through programs of numerical analysis as finite elements and/or boundary elements. The aim of this work is the comparison between the results of numerical solution of an ultrasonic wave, which is obtained from transient excitation pulse that can be specified by either force or displacement variation across the aperture of the transducer, and the results obtained from a experiment that was realized in an aluminum block in the IEN Ultrasonic Laboratory. The wave propagation can be simulated using all the characteristics of the material used in the experiment evaluation associated to boundary conditions and from these results, the comparison can be made.

Testing a linear propagation module on some acoustic scattering problems

Abstract not available

Étude paramétrique de la propagation d'ondes ultrasonores guidées dans les structures aéronautiques

La mise en oeuvre de systèmes de détection de défauts à même les structures ou infrastructures en génie est le sujet d’étude du Structural Health Monitoring (SHM). Le SHM est une solution efficace à la réduction des coûts associés à la maintenance de structures. Une stratégie prometteuse parmi les technologies émergentes en SHM est fondée sur l’utilisation d’ondes ultrasonores guidées. Ces méthodes sont basées sur le fait que les structures minces agissent comme guides d’ondes pour les ondes ultrasonores. Puisque les structures aéronautiques sont majoritairement minces, les ondes guidées constituent une stratégie pertinente afin d’inspecter de grandes surfaces. Toutefois, les assemblages aéronautiques sont constitués de plusieurs éléments modifiant et compliquant la propagation des ondes guidées dans celles-ci. En effet, la présence de rivets, de raidisseurs, de joints ainsi que la variation de la nature des matériaux utilisés complexifie la propagation des ondes guidées. Pour envisager la mise en oeuvre de systèmes de détection basés sur les ondes guidées, une compréhension des interactions intervenant dans ces diverses structures est nécessaire. Un tel travail entre dans le cadre du projet de collaboration CRIAQ DPHM 501 dont l’objectif principal est de développer une banque de connaissances quant à la propagation d’ondes guidées dans les structures aéronautiques. Le travail de ce mémoire présente d’abord les résultats d’études paramétriques numériques obtenus dans le cadre de ce projet CRIAQ. Puis, afin de faciliter la caractérisation expérimentale de la propagation des ondes guidées, une seconde partie du travail a porté sur le développement d’un absorbant d’ondes guidées. Cet absorbant permet également d’envisager l’extension des régions observables par les systèmes SHM. Ce deuxième volet contribue donc également au projet CRIAQ par l’atténuation de réflexions non désirées dans l’étude menée sur les maintes structures aéronautiques nourrissant la banque de connaissances. La première partie de ce mémoire relève l’état des connaissances de la littérature sur la propagation d’ondes guidées dans les structures aéronautiques. La deuxième partie présente rapidement le formalisme derrière les ondes de Lamb ainsi que les différentes approches analytiques pour caractériser les interactions entre ondes guidées et discontinuités. Par la suite, les outils utilisés pour effectuer les simulations par éléments finis sont présentés et validés par le biais d’une phase expérimentale. La deuxième partie se termine avec la présentation des différentes structures et discontinuités étudiées dans le cadre du projet CRIAQ. Finalement, la troisième et dernière partie de ce mémoire présente les travaux numériques orientés vers la conception d’un absorbant idéal pour ondes guidées. Afin d’y parvenir, une étude paramétrique quant à la forme, les dimensions et les propriétés mécaniques de l’absorbant est entreprise. Enfin, une étude expérimentale permettant de valider les résultats numériques est présentée.

Phenobarbital reduces EEG amplitude and propagation of neonatal seizures but does not alter performance of automated seizure detection

Objective: Phenobarbital increases electroclinical uncoupling and our preliminary observations suggest it may also affect electrographic seizure morphology. This may alter the performance of a novel seizure detection algorithm (SDA) developed by our group. The objectives of this study were to compare the morphology of seizures before and after phenobarbital administration in neonates and to determine the effect of any changes on automated seizure detection rates. Methods: The EEGs of 18 term neonates with seizures both pre- and post-phenobarbital (524 seizures) administration were studied. Ten features of seizures were manually quantified and summary measures for each neonate were statistically compared between pre- and post-phenobarbital seizures. SDA seizure detection rates were also compared. Results: Post-phenobarbital seizures showed significantly lower amplitude (p < 0.001) and involved fewer EEG channels at the peak of seizure (p < 0.05). No other features or SDA detection rates showed a statistical difference. Conclusion: These findings show that phenobarbital reduces both the amplitude and propagation of seizures which may help to explain electroclinical uncoupling of seizures. The seizure detection rate of the algorithm was unaffected by these changes. Significance: The results suggest that users should not need to adjust the SDA sensitivity threshold after phenobarbital administration.