Identification and Ranking of risk factors for somatic cell count economic penalty in 349 southern Belgium dairy farms

in Maillard, R.; Navetat, H. (Eds.) European buiatrics forum 2009 (2009, December 02)

In Belgium, the main economic penalty accounted for bovine milk quality is the bulk milk somatic cell count geometric mean over 3 months reaching more than 400,000 cells/ml. Yet, it is still difficult to ... [more ▼]

In Belgium, the main economic penalty accounted for bovine milk quality is the bulk milk somatic cell count geometric mean over 3 months reaching more than 400,000 cells/ml. Yet, it is still difficult to make progress on udder health and milk quality because regional risks related to endemic farming practices are not broadly known. Hence, a first step in understanding specific udder health risks associated with herd management has to be a broad ecopathological survey. A random stratified sample of 349 dairy farms, representing 25% of producers registered for performance recording, was selected with a total of 16,000 cows. Thorough audits recording 400 farming practices were made in each farm by 2 different surveyors during milking. The practices were recorded across four categories: Herd structure, Housing, Milking practices and Herd Management (including Nutrition). Our chosen variable was the geometric mean of the herd composite somatic cell count from the last three months compared to the 400,000 cells/ml European threshold. The sample had a mean somatic cell count of 287,000 cells/ml following a normal distribution between 73,000 and 807,000 cells/ml. From 19 risk indicators identified through univariate logistic analysis (p<0.15), half were related to milking practices and 5 were underlined by significant odds-ratios (OR) found through multivariate logistic analysis (p<0.05). Therefore, it was found that cubicle housing had the least risk (OR= 0.59 compared with tightened stalls, OR= 0.42 compared with straw stalls); Presence of a calving pen (OR= 0.40), use of post-dipping (OR= 0.50) had a positive impact; whereas pre-dip had a negative impact in our study (OR= 3) though it was not clear if this routine was performed correctly. Stripping also had a bad impact on milk quality whether it was systematic (OR = 1.90) or occasional (OR = 2.43). It was also found that farms with poor milking liner hygiene had more trouble (OR = 2.34). The results were comparable to other ecopathological studies such as northern and southern American and European studies. This study is a prerequisite in operational veterinary advice in southern Belgium dairy farms, because it provides a cross-sectional study of dairy practices and states on major epidemiological risk factors in dairy management for this region. [less ▲]

Virtual model of the city of Liège in the eighteen century - "Virtual Leodium"

in Verly, Jacques (Ed.) Proceedings of 3D Stereo MEDIA 2009, International 3D Stereo Film and Technology Festival (3D Stereo MEDIA), Liège, Belgium, 1-3 Dec. 2009. (2009, December 01)

Virtual Leodium is a project aiming to scan and digitize a master piece of the collection of the University of Liège, the historical model of the city of Liège around 1730 realised by Gustave Ruhl. The ... [more ▼]

Virtual Leodium is a project aiming to scan and digitize a master piece of the collection of the University of Liège, the historical model of the city of Liège around 1730 realised by Gustave Ruhl. The two main originalities of the approach are to use a projected-fringes scanning technique and to generate a geo-database as a support for archaeological information. This interdisciplinary project gathers physicists, geomaticians, librarians, and archaeologists. [less ▲]

Collective pulsational velocity broadening due to gravity modes as a physical explanation for macroturbulence in hot massive stars

in Astronomy and Astrophysics (2009), 508

Aims. We aimed at finding a physical explanation for the occurrence of macroturbulence in the atmospheres of hot massive stars, a phenomenon found in observations for more than a decade but that remains ... [more ▼]

Aims. We aimed at finding a physical explanation for the occurrence of macroturbulence in the atmospheres of hot massive stars, a phenomenon found in observations for more than a decade but that remains unexplained.<BR /> Methods: We computed time series of line profiles for evolved massive stars broadened by rotation and by hundreds of low-amplitude nonradial gravity-mode pulsations which are predicted to be excited for evolved massive stars.<BR /> Results: In general, line profiles based on macrotubulent broadening can mimic those subject to pulsational broadening. In several cases, though, good fits require macroturbulent velocities that pass the speed of sound for realistic pulsation amplitudes. Moreover, we find that the rotation velocity can be seriously underestimated by using a simple parameter description for macroturbulence rather than an appropriate pulsational model description to fit the line profiles.<BR /> Conclusions: We conclude that macroturbulence is a likely signature of the collective effect of pulsations. We provide line diagnostics and their typical values to decide whether or not pulsational broadening is present in observed line profiles, as well as a procedure to avoid an inaccurate estimation of the rotation velocity. [less ▲]

Recurrent energization of plasma in the midnight-to-dawn quadrant of Saturn's magnetosphere, and its relationship to auroral UV and radio emissions

in Planetary and Space Science (2009), 57

We demonstrate that under some magnetospheric conditions protons and oxygen ions are accelerated once per Saturn magnetosphere rotation, at a preferred local time between midnight and dawn. Although ... [more ▼]

We demonstrate that under some magnetospheric conditions protons and oxygen ions are accelerated once per Saturn magnetosphere rotation, at a preferred local time between midnight and dawn. Although enhancements in energetic neutral atom (ENA) emission may in general occur at any local time and at any time in a Saturn rotation, those enhancements that exhibit a recurrence at a period very close to Saturn's rotation period usually recur in the same magnetospheric location. We suggest that these events result from current sheet acceleration in the 15-20 Rs range, probably associated with reconnection and plasmoid formation in Saturn's magnetotail. Simultaneous auroral observations by the Hubble Space Telescope (HST) and the Cassini Ultraviolet Imaging Spectrometer (UVIS) suggest a close correlation between these dynamical magnetospheric events and dawn-side transient auroral brightenings. Likewise, many of the recurrent ENA enhancements coincide closely with bursts of Saturn kilometric radiation, again pointing to possible linkage with high latitude auroral processes. We argue that the rotating azimuthal asymmetry of the ring current pressure revealed in the ENA images creates an associated rotating field aligned current system linking to the ionosphere and driving the correlated auroral processes. [less ▲]

Physical Properties of the 0.94-Day Period Transiting Planetary System WASP-18

in Astrophysical Journal (2009), 707

We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we ... [more ▼]

We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The data are analyzed using the JKTEBOP code and three different sets of stellar evolutionary models. We find the mass and radius of the planet to be M [SUB]b[/SUB] = 10.43 ± 0.30 ± 0.24 M [SUB]Jup[/SUB] and R [SUB]b[/SUB] = 1.165 ± 0.055 ± 0.014 R [SUB]Jup[/SUB] (statistical and systematic errors), respectively. The systematic errors in the orbital separation and the stellar and planetary masses, arising from the use of theoretical predictions, are of a similar size to the statistical errors and set a limit on our understanding of the WASP-18 system. We point out that seven of the nine known massive transiting planets (M [SUB]b[/SUB] > 3 M [SUB]Jup[/SUB]) have eccentric orbits, whereas significant orbital eccentricity has been detected for only four of the 46 less-massive planets. This may indicate that there are two different populations of transiting planets, but could also be explained by observational biases. Further radial velocity observations of low-mass planets will make it possible to choose between these two scenarios. Based on data collected by MiNDSTEp with the Danish 1.54  m telescope at the ESO La Silla Observatory. [less ▲]

Intérêt de la chromatographie liquide d'interactions hydrophiles pour l'analyse de composés polaires dans des matrices complexes

Conference (2009, December 01)

Impact of helium diffusion and helium-flash-induced carbon production on gravity-mode pulsations in subdwarf B stars

in Astronomy and Astrophysics (2009), 508

Context: Realistic stellar models are essential to the forward modelling approach in asteroseismology. For practicality however, certain model assumptions are also required. For example, in the case of ... [more ▼]

Context: Realistic stellar models are essential to the forward modelling approach in asteroseismology. For practicality however, certain model assumptions are also required. For example, in the case of subdwarf B stars, one usually starts with zero-age horizontal branch structures without following the progenitor evolution. <BR /> Aims: We analyse the effects of common assumptions in subdwarf B models on the g-mode pulsational properties. We investigate if and how the pulsation periods are affected by the H-profile in the core-envelope transition zone. Furthermore, the effects of C-production and convective mixing during the core helium flash are evaluated. Finally, we reanalyse the effects of stellar opacities on the mode excitation in subdwarf B stars.<BR /> Methods: We computed detailed stellar evolutionary models of subdwarf B stars, and their non-adiabatic pulsational properties. Atomic diffusion of H and He is included consistently during the evolution calculations. The number fractions of Fe and Ni are gradually increased by up to a factor of 10 around log T = 5.3. This is necessary for mode excitation and to approximate the resulting effects of radiative levitation. We performed a pulsational stability analysis on a grid of subdwarf B models constructed with OPAL and OP opacities.<BR /> Results: We find that helium settling causes a shift in the theoretical blue edge of the g-mode instability domain to higher effective temperatures. This results in a closer match to the observed instability strip of long-period sdB pulsators, particularly for l â ¤ 3 modes. We show further that the g-mode spectrum is extremely sensitive to the H-profile in the core-envelope transition zone. If atomic diffusion is efficient, details of the initial shape of the profile become less important in the course of evolution. Diffusion broadens the chemical gradients, and results in less effective mode trapping and different pulsation periods. Furthermore, we report on the possible consequences of the He-flash for the g-modes. The outer edge of a flash-induced convective region introduces an additional chemical transition in the stellar models, and the corresponding spike in the Brünt-Väisälä frequency produces a complicated mode trapping signature in the period spacings. <BR /> [less ▲]

The use of an adapted model allows contributing to the “Reduction” of mice used in experimental protocols: the case of the apoE–deficient (apo E-/-) mice in a model of atherosclerosis control

Poster (2009, December 01)

Atherosclerosis is a chronic vascular disease whose development is influenced by several mediators 1. Among them, the prostanoids large family lipids generated from the metabolism of arachidonic acid by ... [more ▼]

Atherosclerosis is a chronic vascular disease whose development is influenced by several mediators 1. Among them, the prostanoids large family lipids generated from the metabolism of arachidonic acid by the action of COX includes various types of PGs and thromboxane. Thromboxane A2 and PGI2 are present in abnormally elevated concentration in atherosclerosis 2-3. To exert its effects TXA2 and its precursor PGH2 act at a specific receptor termed TP receptor 4. As a result, TXA2 synthase inhibitors and TP antagonists have been developed to reduce and to prevent TXA2 production and actions, respectively. The present study was undertaken in order to investigate whether BM-573, an original sulfonylurea derivate synthesized in our lab 5, and aspirin would be effective in preventing the progression of atherosclerosis in an apo E deficient mouse model. [less ▲]

Phase-resolved XMM-Newton observations of the massive WR+O binary WR 22

in Astronomy and Astrophysics (2009), 508

Aims. To better understand the phenomenon of colliding winds in massive binary stars, we study the X-ray lightcurve of a WR+O system of the Carina region, a system well known for the high mass of its ... [more ▼]

Aims. To better understand the phenomenon of colliding winds in massive binary stars, we study the X-ray lightcurve of a WR+O system of the Carina region, a system well known for the high mass of its primary.<BR /> Methods: Phase-resolved X-ray observations of the massive WR+O binary system WR 22 were performed with the XMM-Newton facility. We observed the object at seven different phases from near apastron to near periastron.<BR /> Results: The X-ray spectrum can be represented by a two-component, optically thin, thermal plasma model with a first one at a typical temperature of 0.6 keV and a second hotter one in the range 2.0-4.5 keV. The hot component is indicative of a colliding wind phenomenon, but its flux is remarkably constant with time despite the high eccentricity of the orbit. Although surprising at first, this actually does not contradict the results of the hydrodynamical simulations of the wind collision that we performed. When the system goes from apastron to periastron, the soft part of the X-ray flux is progressively lowered by an increasing intervening absorbing column. This behaviour can be interpreted in terms of an X-ray emitting plasma located near the O star, but not fully intrinsic to it, and accompanying the star when it dives into the wind of the WR component. A model is presented that interprets most of the observational constraints. This model suggests that the mass-loss rate of dot{M}[SUB]WR[/SUB] 1.6 à 10[SUP]-5[/SUP] {M}[SUB]ȯ[/SUB] yr[SUP]-1[/SUP] assumed for the WR could still be slightly too high, whereas it is already lower than other published values. From the comparison of the observed and the expected absorptions at phases near periastron, we deduce that the hard X-ray emitting collision zone should at least have a typical size of 50-60 R[SUB]ȯ[/SUB], but that the size for the soft X-ray emitting region could reach 244 R[SUB]ȯ[/SUB] if the assumed mass-loss rate is correct. We also present an upper limit to the X-ray luminosity of the WR component that further questions the existence of intrinsic X-ray emission from single WN stars.<BR /> Based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). Research Associate FNRS (Belgium). Postdoctoral Researcher FNRS (Belgium). [less ▲]

Continuous Characterization of Growth Phase Using Ground Optical and Magnetic Data

Conference (2009, December 01)

The growth phase of substorms is characterized by equatorward motion of the auroral oval as manifested by optical emissions and the electrojet currents detected on the ground through magnetic ... [more ▼]

The growth phase of substorms is characterized by equatorward motion of the auroral oval as manifested by optical emissions and the electrojet currents detected on the ground through magnetic perturbations. We will demonstrate the use of an inversion procedure for magnetic data that follows the optical borders detected in the CANOPUS Churchill meridian well. Multispectral meridian scanning photometry allows identification of 486 nm H-beta emission with the equatorward edge of the evening sector growth phase electrojet, consistent with downward field-aligned current at this location. The 630 nm and 557 nm emissions due to the precipitation of electrons are identified with the more poleward regions or the poleward border, and upward field-aligned current. While these results are already known, the use of magnetic data is a new way of continuously monitoring growth phase. The identifications are supported by satellite imaging from Image and POLAR in individual cases. Despite separation of the proton and electron emissions as observed from the ground, our results are consistent with the polar cap boundary determined using proton imaging by SI12 on Image. We have also confirmed precipitation region and FAC coincidence using FAST, and corrected the electrojet position when FAST did not fly directly over the ground array, based on imaging from the high altitude satellites. [less ▲]