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See detailL'assureur vie à la recherche des causes du décès de l'assuré
Paris, Catherine ULg

in Revue Générale des Assurances et des Responsabilités [=RGAR] (2011)

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See detailAssureurs et prédations: Les développements de l'assurance contre le vol en France
Lemaître, André ULg

in Les Cahiers de la Sécurité Intérieure (1996), N°25

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See detailAstatine production in a lead-bismuth target bombarded by a proton beam: A detailed study using INCL4.6-Abla07
David, J.-C.; Boudard, A.; Cugnon, Joseph ULg et al

in Progress in Nuclear Science and Technology (2014), 4

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See detailL'astaxanthine: de la biologie à l'industrie
Fratamico, Anthony ULg

Scientific conference (2014, May 06)

Detailed reference viewed: 42 (9 ULg)
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See detailAstects pratique de l'utilisation des antidépresseurs
PITCHOT, William ULg; Ansseau, Marc ULg

in Revue Médicale de Liège (1990)

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See detailAsteroid 45 Eugenia - Lightcurves and the pole orientation
Taylor, R. C.; Birch, P. V.; Pospieszalska-Surdej, Anna ULg et al

in ICARUS (1988), 73

Nine lightcurves of asteroid 45 Eugenia, three from 1969 and six from 1984, are given. In 1984 - 1985 the H[SUB]0[/SUB] magnitude of Eugenia, corrected to the lightcurve maximum, was 7.47 and the slope ... [more ▼]

Nine lightcurves of asteroid 45 Eugenia, three from 1969 and six from 1984, are given. In 1984 - 1985 the H[SUB]0[/SUB] magnitude of Eugenia, corrected to the lightcurve maximum, was 7.47 and the slope parameter G[SUB]0[/SUB] was 0.04. The north pole of Eugenia is within ±10° of ecliptic longitude 106° and latitude +26° (or 295° and +34°). This solution is consistent with an amplitude-aspect pole analysis. The sideral period is 0.2374645±0.0000002 day and the sense of rotation is retrograde. [less ▲]

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See detailAsteroid 532 Herculina - Lightcurves, pole orientation and a model
Taylor, R. C.; Birch, P. V.; Drummond, J. et al

in Icarus (1987), 69

Photoelectric lightcurves of 532 Herculina in 1984 show two maxima and two minima with a synodic rotation period of 0.39185±0.00002 day (1sigma). During some other oppositions the Herculina lightcurve has ... [more ▼]

Photoelectric lightcurves of 532 Herculina in 1984 show two maxima and two minima with a synodic rotation period of 0.39185±0.00002 day (1sigma). During some other oppositions the Herculina lightcurve has only one maximum and one minimum over that same rotation period. The absolute magnitude in V is 6.13±0.02 mag, the phase coefficient in V is 0.037±0.002, and the mean colors are B-V = +0.86±0.04 and U-B = +0.43±0.02. The authors applied photometric astrometry and the results indicate a sidereal period of 0.3918711±0.0000001 day with retrograde rotation for a north pole at 276° long and +1° lat. The uncertainty of the pole is ±1°. A model of Herculina is presented that generates lightcurves consistent with both the observed amplitudes and the timings of extrema over precisely 28,630 sidereal rotations during 30 years. [less ▲]

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See detailAsteroid lightcurves simulated by the rotation of a three-axes ellipsoid model
Surdej, Jean ULg; Surdej, Anna ULg

in Astronomy and Astrophysics (1978), 66

A triaxial-ellipsoid model is used to simulate the smooth and nearly symmetric light curves that are usually characteristic of asteroids which exhibit large brightness variations. The mathematical model ... [more ▼]

A triaxial-ellipsoid model is used to simulate the smooth and nearly symmetric light curves that are usually characteristic of asteroids which exhibit large brightness variations. The mathematical model is developed and applied to two problems involving an asteroid moving with its rotational axis either perpendicular to or lying within the plane containing the sun and earth. The numerical results obtained are compared with Dunlap's (1971) simulations of asteroid brightness variations, and it is argued that typical asteroid phase coefficients cannot be interpreted unambiguously. The results are shown to favor the Hapke-Irvine relation for describing the scattering properties of a dark asteroid surface. [less ▲]

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See detailAsteroid polarimetry : validation run on the CAPS polarimeter
Devogele, Maxime ULg; Cellino, A.; Massone, G. et al

Conference (2015)

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See detailAsteroid rotation - Hunting for a record: 1689 Floris-Jan
Schober, H. J.; Surdej, Jean ULg

in The Messenger (1982), 29

Last year, in June 1981 - ESO Messenger No. 24, p. 22-23 - H. J. Schober published areport on "Spinning Asteroids and Photometry". There he mainly gave a general introduction about what can be done using ... [more ▼]

Last year, in June 1981 - ESO Messenger No. 24, p. 22-23 - H. J. Schober published areport on "Spinning Asteroids and Photometry". There he mainly gave a general introduction about what can be done using UBV photometry in order to derive physical properties of asteroids such as geometrie forms, diameters, reflectance on the surface, bimodality of asteroids with respect to typology. A special effort was made to report about the activities to deal with asteroids as "variable objects" like variable stars - showing Iightcurves with defined rotation rates to be derived. Among asteroids it was stated that the longest rotation periods found before 1975 were not larger than 20 hours - followed by 654 Zelinda 31 ~9 (1975). 393 Lampetia 38h7, 128 Nemesis 39h0 (1979), 709 Fringilla 52h4 (1979) and 182 Eisa 80~00 (1980), the latter corresponding to 3d33. [less ▲]

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See detailASTEROID: regression de l'atherosclerose coronaire avec la rosuvastatine 'a une dose maximale de 40 mg par jour.
Scheen, André ULg

in Revue Médicale de Liège (2006), 61(4), 267-72

ASTEROID is a prospective, open-label blinded end-points trial aiming to assess whether very intensive statin therapy with rosuvastatin 40 mg/day could regress coronary atherosclerosis as determined by ... [more ▼]

ASTEROID is a prospective, open-label blinded end-points trial aiming to assess whether very intensive statin therapy with rosuvastatin 40 mg/day could regress coronary atherosclerosis as determined by intravascular ultrasound (IVUS). This multinational study included 507 patients, among whom 349 had evaluable serial IVUS examinations at 24 months. Rosuvastatin decreased LDL cholesterol level from 130 mg/dl to 61 mg/dl (- 53.2%) and increased HDL cholesterol from 43 to 49 mg/dl (+ 14.7%). The three prespecified IVUS efficacy parameters were positively altered by rosuvastatin, demonstrating regression of coronary atherosclerosis : the mean change in percent atheroma volume (- 0.98%), the change in atheroma volume in the most diseased 10-mm subsegment me (- 6.1 mm3) and the change in total atheroma volume (- 6.8%) were all significant (p < 0,001). Adverse events were infrequent and similar to other statin trials. The present study demonstrates that a 2-year treatment with a high dose of rosuvastatin 40 mg/day is able to induce significant regression of coronary atherosclerosis as determined by IVU imaging. Further ongoing studies in the GALAXY clinical investigation programme should now demonstrate that rosuvastatin, the most potent statin to reduce LDL and increase HDL cholesterol, is also able to diminish the incidence of clinical outcomes, cardiovascular events in general and major coronary events in particular. [less ▲]

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See detailThe asteroseismic analysis of the pulsating sdB Feige 48 revisited
Van Grootel, Valérie ULg; Charpinet, Stéphane; Fontaine, Gilles et al

Conference (2007, July)

We present a new detailed analysis of the short period pulsating sdB star Feige 48, based on the same observations than in our previous work (Charpinet et al., 2005, A&A 443, 251) but with our new codes ... [more ▼]

We present a new detailed analysis of the short period pulsating sdB star Feige 48, based on the same observations than in our previous work (Charpinet et al., 2005, A&A 443, 251) but with our new codes including the rotation of the star. Feige 48 is supposed to be a relatively fast rotator, showing a fine structure in its pulsation spectrum about 28 µHz on three groups in the 9 frequencies. On the other side, Feige 48 belongs to a close binary system (likely with a white dwarf) where the orbital period is 9.02 +/- 0.03h (S. O'Toole 2004). With our new codes including the rotation (for a given rotation law, we calculate associated multiplets for each frequency with the perturbative approach on the first order), avoiding us to make assumptions about the m=0 modes, we were able to fit all the 9 periods together, leading to sligthly different estimations for the structural parameters of Feige 48 than in our previous work. Moreover, the rotation of the star is found to be solid with a period of 32,540s <=> 9.038h, very close to the orbital period of the system determined by spectroscopy, confirming the reasonable assumption that the system is tidally locked. In this context, it was possible to exclude that Feige 48 has a fast rotating core in term of much poorer merit functions. [less ▲]

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See detailAsteroseismic hare & hound exercises: the case of β Cephei stars
Salmon, Sébastien ULg; Montalbán, J.; Miglio, A. et al

in Martins, F.; Boissier, S.; Buat, V. (Eds.) et al SF2A-2015: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: F. Martins, S. Boissier, V. Buat, L. Cambrésy, P. Petit, pp.423-428 (2015, December 01)

The β Cephei pulsating stars present a unique opportunity to test and probe our knowledge of the interior of massive stars. The information that we can get depends on the quality and number of ... [more ▼]

The β Cephei pulsating stars present a unique opportunity to test and probe our knowledge of the interior of massive stars. The information that we can get depends on the quality and number of observational constraints, both seismic and classical ones. The asteroseismology of β Cephei stars proceeds by a forward approach, which can result in multiple solutions, without clear indication on the level of confidence. We seek a method to derive confidence intervals on stellar parameters and investigate how these latter behave depending on the seismic data accessible to the observer. We realise forward modelling with the help of a grid of pre-computed models. We also use Monte-Carlo simulations to build confidence intervals on the inferred stellar parameters. We apply and test this method in a series of hare and hound exercises on a subset of theoretical models simulating observed stars. Results show that a set of 5 frequencies (with knowledge of their associated angular degree) yields precise seismic constraints. Significant errors on the determination of the extent of the central mixed region may result when the theoretical models do not present the same chemical mixture as the observed star. [less ▲]

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See detailAsteroseismic inversions in the context of Plato
Buldgen, Gaël ULg; Dupret, Marc-Antoine ULg; Reese, Daniel Roy

Conference (2014)

The determination of stellar characteristics such as the mass, the age or the radius, is crucial when studying both stellar evolution and exoplanetary systems. In the context of the Plato mission, the ... [more ▼]

The determination of stellar characteristics such as the mass, the age or the radius, is crucial when studying both stellar evolution and exoplanetary systems. In the context of the Plato mission, the high quality data allows us to reach a new level of accuracy and model-independence for stellar characterization by using inversion techniques. In this study, we will use the SOLA method (F. Pijpers and M. J. Thompson 1994), known for its successes in helioseismology, and show how it can offer us new insights into the structure of observed stars. We will present results for the mean density, building on the approach of Reese et al. 2012, and other custom-made structural characteristics constraining the outer layers of stars and the chemical content of their cores. We will show that inversions can determine these characteristics within 0.5%, a significant improvement over the capabilities of the classical forward modelling process. Consequently, such inversions lead to better stellar models and help us obtain more accurate estimates of fundamental parameters such as the age, mass or radius. [less ▲]

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See detailAn asteroseismic Main Sequence model for the delta Scuti star 44 Tau
Garrido, R.; Suárez, J. C.; Grigahcène, A. et al

in Communications in Asteroseismology (2007), 150

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See detailAsteroseismic observations and modelling of 70 Ophiuchi AB
Eggenberger, P.; Miglio, Andrea ULg; Carrier, F. et al

in Journal of Physics Conference Series (2008), 118(1), 012053-

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See detailThe Asteroseismic Potential of Kepler: First Results for Solar-Type Stars
Chaplin, W. J.; Appourchaux, T.; Elsworth, Y. et al

in Astrophysical Journal Letters (2010), 713

We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise ... [more ▼]

We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: about 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses, and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe. [less ▲]

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See detailAsteroseismic probing of internal rotation in hot B subdwarf stars: Testing spin-orbit synchronism in two close binary systems
Van Grootel, Valérie ULg; Charpinet, Stéphane; Fontaine, Gilles et al

in Journal of Physics: Conference Series (2009, June), 172

We present internal rotation profiles derived from asteroseismology for the hot pulsating B subdwarf stars PG 1336-018 and Feige 48. These two pulsators are primaries of close binary systems of known ... [more ▼]

We present internal rotation profiles derived from asteroseismology for the hot pulsating B subdwarf stars PG 1336-018 and Feige 48. These two pulsators are primaries of close binary systems of known orbital period and, therefore, provide laboratories to test, for the first time, spin-orbit synchronization as a function of depth. We show that PG 1336-018 and Feige 48 clearly rotate as solid bodies with periods equal to their orbital periods from the surface down to at least ~ 0.5 and ~ 0.3 their radius, respectively. Deep tidal locking has therefore developed within the relatively short lifetime of these stars (~ 10^8 yr). [less ▲]

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See detailAsteroseismic Solutions for the Two Fast Subdwarf B Pulsators Balloon 090100001 and PG 1336-018
Charpinet, Stéphane; Van Grootel, Valérie ULg; Brassard, Pierre et al

in Leaflet - Astronomical Society of the Pacific (2008, January), 392

We present two new asteroseismic studies of the rapid sdB pulsator PG 1336-018 and the hybrid sdB pulsator Balloon (BAL) 090100001. For PG 1336-018, the analysis is based on 25 periods extracted from the ... [more ▼]

We present two new asteroseismic studies of the rapid sdB pulsator PG 1336-018 and the hybrid sdB pulsator Balloon (BAL) 090100001. For PG 1336-018, the analysis is based on 25 periods extracted from the white-light photometry of the Xcov17 Whole Earth Telescope campaign (Kilkenny et al. 2003). For BAL 090100001, we use 10 periods of high amplitudes for which constraints on the ℓ-index have been derived from high S/N multicolour photometry. From asteroseismology, we estimate important structural parameters for these two stars, including the stellar mass and the H-rich envelope thickness. The analyses presented here are of particular interest since the asteroseismic results can be tested using independent constraints, which confirm the robustness of the solutions in both cases. [less ▲]

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See detailAn asteroseismic study of the beta Cephei CoRoT main target HD 180642: results from the ground-based campaign
Briquet, Maryline ULg; Uytterhoeven, K.; Morel, Thierry ULg et al

in American Institute of Physics Conference Series (2009, September 01)

The β Cephei star HD 180642 was observed by the CoRoT satellite during a run of 156 days in 2007. The space white light photometry revealed the rich frequency spectrum of the star (Degroote et al. 2009 ... [more ▼]

The β Cephei star HD 180642 was observed by the CoRoT satellite during a run of 156 days in 2007. The space white light photometry revealed the rich frequency spectrum of the star (Degroote et al. 2009). In the present study, we provide additional information on the target, based on both ground-based multi-colour photometry and high-resolution spectroscopy. We place our object in the (T[SUB]eff[/SUB], log g) diagram. In addition, we derive the chemical abundances of several elements as well as the metallicity of HD 180642. Finally, we put constraints on the identification of some modes. All these observational constraints will be used to compute stellar models of the target. [less ▲]

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