Browsing
     by title


0-9 A B C D E F G H I J K L M N O P Q R S T U V W X Y Z

or enter first few letters:   
OK
Full Text
See detailChamps électromagnétiques: les règles belges et européennes
Beauvois, Véronique ULg

in Les carnets du préventeur (2007)

En matière de champs électromagnétiques, la législation européenne et par conséquent la législation belge évoluent rapidement ces dernières années. Le monde industriel ne peut rester ignorant dans ce ... [more ▼]

En matière de champs électromagnétiques, la législation européenne et par conséquent la législation belge évoluent rapidement ces dernières années. Le monde industriel ne peut rester ignorant dans ce domaine et doit regarder quelles sont les conséquences de cette évolution sur la vie de l’entreprise et sur celle de ses travailleurs. C’est ce que nous proposons d’aborder au travers de deux directives européennes de 2004: l’une concerne les équipements électroniques au sens large et l’autre s’intéresse aux travailleurs eux-mêmes. [less ▲]

Detailed reference viewed: 60 (7 ULg)
Peer Reviewed
See detailLa chance du malentendu : conflit, créativité et communication "réussie"
Servais, Christine ULg

Conference (2014, December 12)

Detailed reference viewed: 50 (2 ULg)
Full Text
Peer Reviewed
See detailChance in biology – Using probability to explore nature (M. Denny, S. Gaines).
Bogaert, Jan ULg

in Acta Biotheoretica (2003), 51(1), 55-57

Detailed reference viewed: 71 (0 ULg)
See detailChancen erneuerbarer Energien - Abschätzung mittels globaler Bilanzen
Kopriwa, Nicole; Pfennig, Andreas ULg

Conference (2009, November 18)

Detailed reference viewed: 3 (0 ULg)
Full Text
Peer Reviewed
See detailThe Chandra Carina Complex Project: Deciphering the Enigma of Carina's Diffuse X-ray Emission
Townsley, Leisa K; Broos, Patrick S; Chu, You-Hua et al

in Astrophysical Journal Supplement Series (2011), 194

We present a 1.42 deg[SUP]2[/SUP] mosaic of diffuse X-ray emission in the Great Nebula in Carina from the Chandra X-ray Observatory Advanced CCD Imaging Spectrometer camera. After removing >14,000 X-ray ... [more ▼]

We present a 1.42 deg[SUP]2[/SUP] mosaic of diffuse X-ray emission in the Great Nebula in Carina from the Chandra X-ray Observatory Advanced CCD Imaging Spectrometer camera. After removing >14,000 X-ray point sources from the field, we smooth the remaining unresolved emission, tessellate it into segments of similar apparent surface brightness, and perform X-ray spectral fitting on those tessellates to infer the intrinsic properties of the X-ray-emitting plasma. By modeling faint resolved point sources, we estimate the contribution to the extended X-ray emission from unresolved point sources and show that the vast majority of Carina's unresolved X-ray emission is truly diffuse. Line-like correlated residuals in the X-ray spectral fits suggest that substantial X-ray emission is generated by charge exchange at the interfaces between Carina's hot, rarefied plasma and its many cold neutral pillars, ridges, and clumps. [less ▲]

Detailed reference viewed: 24 (2 ULg)
See detailThe Chandra Carina Complex Project: massive stars
Gagné, M.; Fehon, G.; Dickerson, K. et al

Poster (2010)

Detailed reference viewed: 19 (0 ULg)
Full Text
See detailThe Chandra Delta Ori Large Project: Occultation Measurements of the Shocked Gas in the Nearest Eclipsing O-Star Binary
Corcoran, Michael; Nichols, Joy; Leutenegger, Maurice et al

Poster (2013, June 01)

Delta Ori is the nearest massive, single-lined eclipsing binary (O9.5 II+OB, P=5.7324d). High resolution X-ray spectrometry offers a unique opportunity to geometrically measure the dynamics of the shocked ... [more ▼]

Delta Ori is the nearest massive, single-lined eclipsing binary (O9.5 II+OB, P=5.7324d). High resolution X-ray spectrometry offers a unique opportunity to geometrically measure the dynamics of the shocked gas around the primary star. We summarize our recent campaign of phase-constrained high-resolution X-ray spectra obtained with the CHANDRA/HETGS plus high-precision photometry with MOST. These observations provide local measurement of the distribution of the embedded, X-ray emitting shocks in the wind of an O star via radial velocity variations and occultation effects, along with standard f/i ratio diagnostics, and enable us to look for correlations with the broad-band photometric variability. We discuss how these observations can help determine the primary star's clumping-corrected mass loss rate, and resolve critical uncertainties in our understanding of the connection between stellar and mass loss parameters. [less ▲]

Detailed reference viewed: 21 (4 ULg)
See detailChandra HRC Observations of X-rays from the Jupiter System
Gladstone, G. R.; Waite, J. H.; Grodent, Denis ULg et al

Conference (2001, June 25)

Detailed reference viewed: 8 (0 ULg)
Full Text
Peer Reviewed
See detailChandra monitoring of the very massive binary WR20a and the young massive cluster Westerlund 2
Nazé, Yaël ULg; Rauw, Grégor ULg; Manfroid, Jean ULg

in Astronomy and Astrophysics (2008), 483(1), 171-182

Context. Westerlund 2 is a young and massive, obscured stellar cluster of our Galaxy. It harbors the most massive star with well-determined parameters, WR20a (82 + 83 M-circle dot), a dozen very early O ... [more ▼]

Context. Westerlund 2 is a young and massive, obscured stellar cluster of our Galaxy. It harbors the most massive star with well-determined parameters, WR20a (82 + 83 M-circle dot), a dozen very early O-type stars (O3-7), and a wealth of PMS stars. Although of clear significance, this star cluster has not been well-studied. Aims. The high-energy properties of this cluster, especially those of its early-type stars are examined in detail. The variability of the X-ray sources is investigated. Methods. A monitoring of the field was performed using three Chandra observations. This dataset probes daily as well as monthly to yearly timescales and provides the deepest X-ray view of the cluster to date. Results. The two Wolf-Rayet stars WR20a (WN6ha+WN6ha) and WR20b (WN6ha) were analyzed in detail. They are both luminous and display hard spectra, but WR20b does not appear to vary. In contrast, WR20a, a known eclipsing, colliding-wind binary, brightens in the X-ray domain during eclipses, i.e. when the collision is seen face-on. This can be explained by the properties of the wind-wind collision zone, whose high density leads to a large absorbing column (2 x 10(24) cm(-2)). All twelve O-type stars previously classified spectroscopically, two eclipsing binaries previously identified and nine newly-identified, O-type star candidates are detected in the high-energy domain; ten of those could be analyzed spectroscopically. Four are overluminous, but the others have typical LX/LBOL ratios, suggesting that several O-type objects are actually binaries. Variability at the similar to 2 sigma level is detected for a majority of the sources, of unknown origin for single objects. Faint, soft, diffuse emission pervades the entire field-of-view but no clear structure can be identified, even at the position of a blister proposed to correspond to the TeV source HESS J1023-575. The X-ray properties of PMS objects, in particular the brightest flaring ones, are also investigated. They provided an additional argument in favor of a large distance (similar to 8 kpc) for the cluster. [less ▲]

Detailed reference viewed: 40 (2 ULg)
See detailA Chandra search for low-mass companions of late B-stars in Tr16
Evans, N. R.; DeGioia-Eastwood, K.; Gagné, M. et al

Poster (2011)

Detailed reference viewed: 22 (3 ULg)
See detailThe Chandra survey of Carina OB stars
Gagné, Marc; Fehon, Garrett; Savoy, Michael R et al

in Neiner, Coralie; Wade, G.; Meynet, G. (Eds.) et al Active OB stars: structure, evolution, mass loss and critical limits (2011, July 01)

We have combined 22 deep Chandra ACIS-I pointings to map over one square degree of the Carina complex. Our x-ray survey detects 69 of 70 known O-type stars and 61 of 130 known early B stars. The majority ... [more ▼]

We have combined 22 deep Chandra ACIS-I pointings to map over one square degree of the Carina complex. Our x-ray survey detects 69 of 70 known O-type stars and 61 of 130 known early B stars. The majority of single O stars display soft X-ray spectra and have a mean log L[SUB]X[/SUB]/L[SUB]bol[/SUB] ~ -7.5 suggesting shocks embedded in the O-star winds. Over OB stars show unusually high X-ray luminosities, high shock temperatures or time variability, not predicted for embedded wind shocks. [less ▲]

Detailed reference viewed: 26 (3 ULg)
Full Text
Peer Reviewed
See detailChandra View of Magnetically Confined Wind in HD191612: Theory Versus Observations
Nazé, Yaël ULg; ud-Doula, Asif; Zhekov, Svetozar A.

in Astrophysical Journal (2016), 831(#138), 11

High-resolution spectra of the magnetic star HD 191612 were acquired using the Chandra X-ray Observatory at both maximum and minimum emission phases. We confirm the flux and hardness variations previously ... [more ▼]

High-resolution spectra of the magnetic star HD 191612 were acquired using the Chandra X-ray Observatory at both maximum and minimum emission phases. We confirm the flux and hardness variations previously reported with XMM-Newton, demonstrating the high repeatability of the behavior of HD 191612 over a decade. The line profiles appear typical for magnetic massive stars: no significant line shift, relatively narrow lines for high-Z elements, and formation radius at about 2 {R}[SUB]* [/SUB]. Line ratios confirm the softening of the X-ray spectrum at the minimum emission phase. Shift or width variations appear of limited amplitude at most (slightly lower velocity and slightly increased broadening at minimum emission phase, but within 1–2σ of values at maximum). In addition, a fully self-consistent 3D magnetohydrodynamic simulation of the confined wind in HD 191612 was performed. The simulation results were directly fitted to the data, leading to a remarkable agreement overall between them. [less ▲]

Detailed reference viewed: 17 (2 ULg)
See detailChandra X-ray Observations of the Jovian System
Elsner, R. F.; Waite, J. H.; Crary, F. et al

Conference (2002)

High-spatial resolution Chandra x-ray obsrvations have demonstrated that most of Jupiter's northern auroral x-rays come from a hot spot located significantly poleward of the latitudes connected to the ... [more ▼]

High-spatial resolution Chandra x-ray obsrvations have demonstrated that most of Jupiter's northern auroral x-rays come from a hot spot located significantly poleward of the latitudes connected to the inner magnetosphere. This hot spot appears fixed in magnetic latitude and longitude and coincides with a region exhibiting anomalous ultraviolet and infrared emissions. The hot spot also exhibited approximately 45 minute quasi-periodic oscillations, a period similar to those reported for high-latitude radio and energetic electron bursts observed by near-Jupiter spacecraft. These results invalidate the idea that jovian auroral x-ray emissions are mainly excited by steady precipitation of energetic heavy ions from the inner magnetosphere. Instead, the x-rays appear to result from currently unexplained processes in the outer magnetosphere that produce highly localized and highly variable emissions over an extremely wide range of wavelengths. The Chandra observations also revealed for the first time x-ray emission (about 0.1 GW) from the Io Plasma Torus, as well as very faint x-ray emission (about 1-2 MW) from the Galilean moons Io, Europa, and possibly Ganymede. The emission from the moons is almost certainly due to Kalpha emission of surface atoms (and possibly impact atoms) excited by the impact of highly energetic protons, oxygen, and sulfur atoms and ions from the Torus. The Torus emission is less well understood at present, although bremsstrahlung from the non-thermal tail of the electron distribution may provide a significant fraction. In any case, further observations, already accepted and in the process of being planned, with Chandra, some with the moderate energy resolution of the CCD camera, together with simultaneous Hubble Space Telescope observations and hopefully ground-based IRTF observations should soon provide greater insight into these various processes. [less ▲]

Detailed reference viewed: 6 (0 ULg)
See detailChandra/ACIS observation of NGC 346
Nazé, Yaël ULg; Stevens, I. R.; Hartwell, J. et al

in Bulletin of the American Astronomical Society (2001, December 01)

The cluster NGC346 is the largest star formation region in the SMC. It contains a large fraction of the early-type O stars of this galaxy. In the outskirts of this cluster lies HD 5980, a unique system of ... [more ▼]

The cluster NGC346 is the largest star formation region in the SMC. It contains a large fraction of the early-type O stars of this galaxy. In the outskirts of this cluster lies HD 5980, a unique system of massive stars of which one component underwent a LBV-type eruption in 1993. The XMEGA consortium has obtained one deep (100 ks) Chandra exposure of NGC 346. It shows ~70 point sources, of which only half possess an optical counterpart; strong emission from HD 5980; and diffuse emission associated with the cluster and SNR 0057-7226. [less ▲]

Detailed reference viewed: 25 (0 ULg)
See detailChanel catfish virus vaccine
Vanderheijden, Nathalie; Martial, Joseph ULg; Hanson, Larry

Patent (2001)

An attenuated, avirulent recombinant vaccine providing challenged protection against channel catfish virus comprises deletion of gene 50. Gene 50 encodes a secreted glycoprotein. Removal of gene 50, or ... [more ▼]

An attenuated, avirulent recombinant vaccine providing challenged protection against channel catfish virus comprises deletion of gene 50. Gene 50 encodes a secreted glycoprotein. Removal of gene 50, or replacement of gene 50 with foreign genetic material, provides a vaccine with which induces virus specific immunity against CCV disease. [less ▲]

Detailed reference viewed: 53 (1 ULg)
Peer Reviewed
See detailChange blindness to gradual changes in facial expressions
Laloyaux, Cédric ULg; Devue, Christel ULg; David, Elodie et al

Poster (2006)

Detailed reference viewed: 39 (3 ULg)
Full Text
Peer Reviewed
See detailChange blindness to gradual changes in facial expressions
David, E.; Laloyaux, Cédric ULg; Devue, Christel ULg et al

in Psychologica Belgica (2006), 46(4), 253-268

Change blindness—our inability to detect changes in a stimulus—occurs even when the change takes place gradually, without disruption (Simons et al., 2000). Such gradual changes are more difficult to ... [more ▼]

Change blindness—our inability to detect changes in a stimulus—occurs even when the change takes place gradually, without disruption (Simons et al., 2000). Such gradual changes are more difficult to detect than changes that involve a disruption. In this experiment, we extend previous findings to the domain of facial expressions of emotions occurring in the context of a realistic scene. Even with changes occurring in central, highly relevant stimuli such as faces, gradual changes still produced high levels of change blindness: Detection rates were three times lower for gradual changes than for displays involving disruption, with only 15% of the observers perceiving the gradual change within a single trial. However, despite this high rate of change blindness, changes on faces were significantly better detected than color changes occurring on non facial objects in the same scene. [less ▲]

Detailed reference viewed: 79 (3 ULg)
Full Text
Peer Reviewed
See detailChange in ATP-binding cassette B1/19, glutamine synthetase and alcohol dehydrogenase gene expression during root elongation in Betula pendula Roth and Alnus glutinosa L. Gaertn in response to leachate and leonardite humic substances
Tahiri, Abdelghani ULg; Delporte, Fabienne ULg; Muhovski, Yordan et al

in Plant Physiology & Biochemistry (2015), 98

Humic substances (HS) are complex and heterogeneous compounds of humified organic matter resulting from the chemical and microbiological decomposition of organic residues. HS have a positive effect on ... [more ▼]

Humic substances (HS) are complex and heterogeneous compounds of humified organic matter resulting from the chemical and microbiological decomposition of organic residues. HS have a positive effect on plant growth and development by improving soil structure and fertility. They have long been recognized as plant growth-promoting substances, particularly with regard to influencing nutrient uptake, root growth and architecture. The biochemical and molecular mechanisms through which HS influence plant physiology are not well understood. This study evaluated the bioactivity of landfill leachate and leonardite HS on alder (Alnus glutinosa L. Gaertn) and birch (Betula pendula Roth) during root elongation in vitro. Changes in root development were studied in relation to auxin, carbon and nitrogen metabolisms, as well as to the stress adaptive response. The cDNA fragments of putative genes encoding two ATP-binding cassette (ABC) transporters (ABCB1 and ABCB19) belonging to the B subfamily of plant ABC auxin transporters were cloned and sequenced. Molecular data indicate that HS and their humic acid (HA) fractions induce root growth by influencing polar auxin transport (PAT), as illustrated by the modulation of the ABCB transporter transcript levels (ABCB1 and ABCB19). There were also changes in alcohol dehydrogenase (ADH) and glutamine synthetase (GS) gene transcript levels in response to HS exposure. These findings confirmed that humic matter affects plant growth and development through various metabolic pathways, including hormonal, carbon and nitrogen metabolisms and stress response or signalization. [less ▲]

Detailed reference viewed: 50 (9 ULg)
Full Text
Peer Reviewed
See detailChange in blood antioxidant status of horses moved from a stable following diagnosis of equine motor neuron disease
Delguste, Catherine ULg; de Moffarts, B.; Kirschvink, N. et al

in Canadian Veterinary Journal = Revue Vétérinaire Canadienne (2007), 48(11), 1165-1167

The antioxidant status of 10 horses living in stable 1 where 2 cases of equine motor neuron disease had previously been diagnosed was assessed before and 9 weeks after moving to another stable. Duration ... [more ▼]

The antioxidant status of 10 horses living in stable 1 where 2 cases of equine motor neuron disease had previously been diagnosed was assessed before and 9 weeks after moving to another stable. Duration of residence in stable 1, subsequent moving, or both, significantly affected several parameters of the antioxidant status. [less ▲]

Detailed reference viewed: 232 (7 ULg)
Full Text
Peer Reviewed
See detailChange in naming abilities between the ages of 50 and 90: The importance of analyzing naming latency
Verhaegen, Clémence ULg; Poncelet, Martine ULg

in Stem-, spraak- en taalpathologie (2012, September), 17(2), 126-128

This study tests the controversial hypothesis that word naming difficulties may arise in individuals as young as their 50s. Participants of 25-35, 50-59, 60-69 and above 70 years of age were given a ... [more ▼]

This study tests the controversial hypothesis that word naming difficulties may arise in individuals as young as their 50s. Participants of 25-35, 50-59, 60-69 and above 70 years of age were given a picture naming task. To uncover subtle naming difficulties, correct naming latencies were analyzed, in addition to accuracy. Moreover, in order to control whether the expected slower naming latencies could be due to a general slowing affecting all cognitive tasks, participants were also given an odd/even judgment task to assess cognitive processing speed. In participants in their 50s, we found subtle naming difficulties revealed by longer naming latencies, unaccompanied by any decrease in naming accuracy. The age-related naming disadvantage increased with age with the onset of naming errors. Thus, in adults in their 60s and their 70s, the results showed both a decrease in accuracy and an increase in correct naming latencies. Moreover, the increase in naming latencies remained significant even after controlling for odd/even judgment latencies, suggesting a degradation specific to the picture naming task. We assumed that these slower latencies may result from a language-specific impairment. [less ▲]

Detailed reference viewed: 36 (8 ULg)