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See detailObservation de comètes faites à l'Observatoire royal de Bruxelles
Folie, François ULg

in Astronomische Nachrichten (1886), 115(2754), 291-298

Table resuming a series of observations of comets made by E. Stuyvaert at the Brussels Royal Observatory in 1885 and 1886 and communicated by François Folie.

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See detailObservation de Jupiter faites à l'Observatoire de Cointe
Swings, Polydore ULg; Dehalu, M.

in Bulletin de la Classe des Sciences. Académie Royale de Belgique (1929), XV(2), 119-125

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See detailObservation de l’atmosphère de Vénus par le spectromètre imageur VIRTIS-M de Venus-Express : analyse des émissions nocturnes de O2 et OH
Soret, Lauriane ULg

Doctoral thesis (2013)

Venus, the second planet of the solar system, has a very dense CO2-dominated atmosphere. Above 50 km, its dynamics is usually decomposed into two main circulation patterns. The first one, the Retrograde ... [more ▼]

Venus, the second planet of the solar system, has a very dense CO2-dominated atmosphere. Above 50 km, its dynamics is usually decomposed into two main circulation patterns. The first one, the Retrograde Superrotating Zonal (RSZ) circulation, controls atmospheric layers below 65 km of altitude. This motion is related to the retrograde rotation of the planet. The second circulation operates above 120 km. This Subsolar-Antisolar (SS-AS) circulation generates a flux from the dayside to the nightside of Venus. It originates from the strong temperature gradients at the top of the atmospheric layer. Between 65 and 120km, the circulation is more complex and no in situ measurement has been performed to study this region of the atmosphere. However, it is possible to use minor atmospheric constituents and their spectral signatures as dynamic tracers to better understand this region. For example, oxygen atoms are produced by photodissociation of CO2 molecules which dominate the Venusian atmosphere. They are then carried by the SS-AS circulation to the planet nightside, where they recombine into O2 molecules in several metastable excited states. Their de-excitation produces measurable emissions, named nightglow which may be qualitatively investigated. This thesis focuses on the study of these emission phenomena. Data have been acquired by the Venus Express spacecraft, in a quasi-polar elliptical orbit around Venus since April 2006. More specifically, observations have been made with the VIRTIS-M instrument, a multispectral imager. As VIRTIS observes in the visible and near infrared domains, some molecular oxygen and hydroxyl transitions can be detected in the data. The main goal of this study has been to extract quantitative information from these observations and to analyze both the density of constituents (such as excited molecular oxygen, atomic oxygen and ozone) and the dynamical processes involved in this region of the Venusian atmosphere. In a first part, data acquired at 1.27 µm in nadir mode have been processed and analyzed in order to study the O2(a1Δg→X3Σg-) infrared atmospheric transition. Data processing consists in correcting the geometrical effects associated with the view angle, the cloud reflection and the thermal contribution. Data analysis following emission patches in individual data sets points out a large variability of the phenomenon, both in terms of brightness and localization. Emission peaks vary from 0.5 to 6 MegaRayleighs (MR) and may be observed over the entire southern hemisphere of the planet, which is the observable part in nadir mode. However, once the individual data are grouped together to generate a statistical map, our analysis shows that the emission at 1.27 µm is located around the antisolar point, which confirms the SS-AS circulation predominance. This map is improved in the northern hemisphere by adding vertical intensity profiles derived from limb images. These profiles are deconvolved to take into account VIRTIS-M spatial resolution and transformed by the Abel inversion to get a local profile of the volume emission rate. A vertical integration of these profiles simulates a nadir observation and completes the bidimensional statistical map of the O2(a1Δg) emission. The intensity reaches 1.6 MR at the antisolar point and the mean nightside value is 0.5 MR. This map, combined with limb profiles, allows to generate a tridimensional distribution of the emission. It shows that the emitting layer is located at ~96.5 km. These results, combined with a tridimensional distribution of the CO2 density (generated with the VTS3 model or measurements from the SPICAV spectrometer on board Venus Express) allows to generate a 3-D map of the atomic oxygen density. The mean nightside density value is 2.0x1011 cm-3 at 103.4 km. This empirical map validates the VTGCM model, as no measurements of the atomic oxygen density had ever been performed in this region of the Venus atmosphere. Other oxygen transitions have been detected in the visible domain (Migliorini et al., 2012): the Herzberg II (c1Σu-→X3Σg-) and Chamberlain (A’3Δu→a1Δg) transitions. Using CO2 and O density profiles derived from our previous study, these transitions have been modeled. Some reaction parameters, whose laboratory measurements are insufficient or inexistent, have thus been estimated. The distribution of the Herzberg I (A3Σu→X3Σg-) transition has also been simulated. Other emission limb profiles have also been extracted from the VIRTIS-M database: the OH(Δv=1) and OH(Δv=2) Meinel emission bands of the hydroxyl molecule. First, these profiles have been processed to subtract a stray signal. The simultaneous statistical study shows that IOH(Δv=1)= 0.60 MR and IOH(Δv=2)=0.23 MR at ~97 km and that their intensity are correlated. The spectral analysis with synthetic spectra demonstrates that only v’≤4 vibrational levels are populated. These emissions have been modeled taking into account excited OH production, deactivation by collisions and reaction and spontaneous emission loss. The CO2 and O density profiles derived from the oxygen study have been used. The quenching coefficients have been adjusted to consider the temperature of the emitting layer and two quenching mechanisms by CO2 have been implemented. This model showed that collisional quenching by single quantum jump (Δv=1) best reproduces the observations. Likewise, an ozone density of 5.8x106 cm-3 at 96.5 km (for the best case) is in good agreement with the recent SPICAV O3 detection. Finally, the study of simultaneous OH(Δv=1) and O2(a1Δg) limb profiles showed a very high spatial correlation of these two emissions. This result has been explained by the role of atomic oxygen as a common precursor for the formation of both molecular oxygen and hydroxyl. [less ▲]

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See detailObservation de l'éclipse partielle de Lune du 16 janvier 1889
Folie, François ULg

in Astronomische Nachrichten (1889), 121(2889), 135-18

The author publishes the remarks and the observations of the moon partial eclipse of January 16th, 1889 made at the Belgium Royal Observatory by E. Stuyvaert.

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See detailObservation de la peau d'un hadrosaure vieux de 75 millions d'années.
Pierard, Sébastien ULg; Franchimont, Claudine ULg; Pierard, Gérald ULg

in Revue Verviétoise d'Histoire Naturelle (1998), 55

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See detailObservation des acteurs et de la dialectique comme marqueurs du genre dans la pratique scientifique
Sturnack, Lionel ULg

Conference (2013, April 20)

Avec ce travail, nous proposons de porter une réflexion sémiotique sur le genre dans le domaine de la médecine clinique.

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See detailL’observation des animaux comme mode d’interrogation de l’homme
Strivay, Lucienne ULg

Conference given outside the academic context (2002)

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See detailL'observation des conduites agressives chez les enfants de classes maternelles
Born, Michel ULg; Pire, B.

in Questions de Logopédie (1988), 17

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See detailL'observation des interactions précoces mère-bébé ultérieurement diagnostiqué autsite
Boulard, Aurore ULg

Conference given outside the academic context (2015)

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See detailObservation des lipides lors de la biotransformation du ricinoléate de méthyle en g-décalactone par Yarrowia lipolytica.
Aguedo, Mario ULg; Waché, Y.; Seguin, M. et al

Poster (1999, September)

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See detailObservation directe, sans mutilation, des pulsations cardiaques chez un mollusque gastéropode
Fredericq, Léon ULg

in Archives Internationales de Physiologie (1914), XIV

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See detailObservation du comportement des participants et des éducateurs sportifs dans le cadre d’activités parascolaires, organisées pour des enfants de 8 à 10 ans
Cloes, Marc ULg; Coulonval, Nathalie; Delfosse, Catherine et al

in Revue de l'Education Physique (1992), 32(4), 189-197

Le livre blanc sur la condition physique des jeunes en Belgique (Piéron & Vrijens, 1991) a attiré l'attention sur l'existence d'un déficit d'activité motrice dans les premières tranches d'âges de la ... [more ▼]

Le livre blanc sur la condition physique des jeunes en Belgique (Piéron & Vrijens, 1991) a attiré l'attention sur l'existence d'un déficit d'activité motrice dans les premières tranches d'âges de la population de notre pays. Afin d'en limiter les effets néfastes, il est opportun que la communauté éducative offre aux enfants plus de possibilités d'engagement dans des programmes d'éducation physique et motrice. ... [less ▲]

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See detailL'observation en psychosomatique
Gauthier, Jean-Marie ULg

in Médecine et psychosomatique (2005)

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See detailL'observation en psychothérapie d'enfants
Gauthier, Jean-Marie ULg

Book published by Dunod (2002)

La pratique de la cure psychanalytique reste étroitement associée à un dispositif spatial particulier : le patient, allongé sur un divan, n'a pas accès au visage de l'analyste placé derrière lui. En ... [more ▼]

La pratique de la cure psychanalytique reste étroitement associée à un dispositif spatial particulier : le patient, allongé sur un divan, n'a pas accès au visage de l'analyste placé derrière lui. En matière de psychanalyse d'enfants, le dispositif de la cure est différent.(...)Partant de ces constats, les auteurs de cet ouvrage se concentrent sur un aspect particulièrement important de l'engagement du corps dans la cure d'enfants, celui de la vision et du regard. Ils montrent, à l'aide de vignettes cliniques détaillées et commentées, comment, chez l'enfant, le geste et le regard sont indissociables de ses représentations. [less ▲]

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See detailObservation n°5 (cas particulier de Parsonage & Turner)
Wang, François ULg; Kaux, Jean-François ULg; Dive, Dominique ULg

in Correspondances en Nerf & Muscle (2005, June), (Numéro spécial), 20-23

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See detailObservation of dayside subauroral proton flashes with IMAGE-FUV.
Hubert, Benoît ULg; Gérard, Jean-Claude ULg; Fuselier, S. A. et al

in EGS - AGU - EUG Joint Assembly (2003, April 01)

The IMAGE-FUV experiment onboard the IMAGE satellite includes three imagers: the WIC and SI13 instruments produce a global scale imaging of the N_2 LBH wavelength range and of the OI 130.4 nm emission ... [more ▼]

The IMAGE-FUV experiment onboard the IMAGE satellite includes three imagers: the WIC and SI13 instruments produce a global scale imaging of the N_2 LBH wavelength range and of the OI 130.4 nm emission respectively, and are thus devoted to the study of the electron aurora. The third imager, SI12, remotely senses the Doppler shifted Lyman-alpha emission, that is solely due to the proton aurora, at the global scale. We present here a new auroral feature observed with the SI12 instrument, consisting of sudden dayside subauroral injections of protons at magnetic latitudes sometimes lower than 60^o MLAT, at the foot of field lines of L shells as low as 4 RE. The extension of the feature in magnetic local time is variable and cases extending from Ë 0700 to Ë 1500 MLT were seen. The relaxation time of these features will be discussed. Most of these dayside subauroral proton flashes are found to be related to sudden solar wind dynamic pressure pulses, but a few counter examples were found. The relationship with the IMF orientation is investigated. [less ▲]

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See detailObservation of dayside subauroral proton flashes with the IMAGE-FUV imagers
Hubert, Benoît ULg; Gérard, Jean-Claude ULg; Fuselier, S. A. et al

in Geophysical Research Letters (2003), 30(3),

[1] A detailed description of an intense flash of auroral emissions that occurs equatorward of the dayside auroral oval observed with the IMAGE-FUV imagers is presented. The comparison of simultaneous ... [more ▼]

[1] A detailed description of an intense flash of auroral emissions that occurs equatorward of the dayside auroral oval observed with the IMAGE-FUV imagers is presented. The comparison of simultaneous snapshots of this subauroral flash obtained with the three FUV cameras indicates that proton precipitation is dominant. This transient proton aurora is triggered by the sudden increase of a solar wind dynamic pressure pulse. It occurs on closed field lines mapping to the equatorial plane at distances as small as similar to4 RE. A second similar event is presented, and several other cases are mentioned. These shock induced transcient emissions develop with a time scale of a few minutes (typically similar to5 min), and have a relaxation time on the order of similar to10 minutes. [less ▲]

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