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See detailChampion (Emptinne, Nr), Villa romaine (signalement archéologique)
Longrée, Dominique ULg; Breyer, Catherine; De Poorter, Alexandra

in Vie archéologique (1991), 36

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See detailLes Champs de Maldoror
Durand, Pascal ULg; Aron, Paul; Bertrand, Jean-Pierre ULg

in Aron, Paul; Bertrand, Jean-Pierre; Durand, Pascal (Eds.) La Littérature Maldoror (2005)

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See detailLes champs écoles paysans maraichers dans la cuvette de Guidimouni, Niger
Baboussouna, Awal; Andres, Ludovic ULg

Conference given outside the academic context (2016)

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See detailChamps électriques et magnétiques et santé : quel message au grand public ?
Ledent, Maryse ULg; Beauvois, Véronique ULg; Demaret, Isabelle ULg et al

in Revue Médicale de Liège (2015), 70(4), 172-178

Les revues de littérature scientifique ne permettent pas de conclure de manière définitive à l’absence d’un effet des champs électriques et magnétiques 50 Hz sur la santé. L’incertitude entraîne de ... [more ▼]

Les revues de littérature scientifique ne permettent pas de conclure de manière définitive à l’absence d’un effet des champs électriques et magnétiques 50 Hz sur la santé. L’incertitude entraîne de nombreux questionnements. Dans cet article, nous aborderons les concepts-clés permettant de bien comprendre les effets potentiels des champs électriques et magnétiques sur la santé. Nous donnerons également des valeurs d’exposition de la vie quotidienne et proposerons des pistes à suivre face à un patient posant des questions sur les effets sur la santé des champs électriques et magnétiques 50 Hz. [less ▲]

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See detailLes champs électromagnétiques de faible intensité produisent une vague calcique dans les fibroblastes
Bomans, J.; Lambert, C. A.; Scarpa, B. et al

in Bulletin et Mémoires de l'Académie Royale de Médecine de Belgique (1996), 151(3-4), 243-9250-2

Human fibroblasts display a Ca2+ wave after irradiation with an electromagnetic field (EMF) of low intensity (100 to 900 microT) as seen by LASER confocal microscopy and excitation of Fluo 3. The number ... [more ▼]

Human fibroblasts display a Ca2+ wave after irradiation with an electromagnetic field (EMF) of low intensity (100 to 900 microT) as seen by LASER confocal microscopy and excitation of Fluo 3. The number of excited cells is proportional to the intensity of EMF between 100 and 900 microT. Cellular activation by a dialysable serum factor is required to induce the Ca2+ wave. It also depends on extracellular Ca2+ and active tyrosine kinases and phospholipase C gamma. [less ▲]

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See detailLes champs électromagnétiques ELF ont-ils un effet sur la santé? Revue de la littérature
Crasson, Marion ULg; Timsit-Berthier, Martine; Legros, Jean-Jacques ULg

in Psychologie Médicale (1992), 24(11), 1205-1215

De nombreuses études ont été entreprises les dernières décénnies sur les effets des champs électromagnétiques de très basse fréquence (TBF ou ELF). Les rapports publiés sont tantôt optimistes tantôt ... [more ▼]

De nombreuses études ont été entreprises les dernières décénnies sur les effets des champs électromagnétiques de très basse fréquence (TBF ou ELF). Les rapports publiés sont tantôt optimistes tantôt pessimistes. Les auteurs passent en revue les recherches épidémiologiques et expérimentales effectuées chez l'homme avant d'envisager une hypothèse explicative des effets observés, en relation avec le rôle joué par la glande pinéale [less ▲]

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See detailChamps électromagnétiques et santé publique. Controverse expliquée par Jean-Louis Lilien
Piet, Grégory ULg

Article for general public (2011)

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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 ▲]

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See detailLa chance du malentendu : conflit, créativité et communication "réussie"
Servais, Christine ULg

Conference (2014, December 12)

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See detailChance in biology – Using probability to explore nature (M. Denny, S. Gaines).
Bogaert, Jan ULg

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

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See detailChancellerie et secrétaires à Florence de la république au principat
Miesse, Hélène ULg

Scientific conference (2016, July 07)

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See detailChancen erneuerbarer Energien - Abschätzung mittels globaler Bilanzen
Kopriwa, Nicole; Pfennig, Andreas ULg

Conference (2009, November 18)

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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 ▲]

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See detailThe Chandra Carina Complex Project: massive stars
Gagné, M.; Fehon, G.; Dickerson, K. et al

Poster (2010)

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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 ▲]

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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)

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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 ▲]

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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 ▲]

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