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Die Musik in Geschichte und Gegenwart (2004)Detailed reference viewed: 11 (1 ULg) Une masse cervicale de diagnostic souvent errone: le chemodectome carotidien.Defraigne, Jean-Olivier ; Antoine, Paul ; SakalihasanN, Natzi et alin Revue Médicale de Liège (1997), 52(7), 485-97Detailed reference viewed: 14 (4 ULg) The Masses and Radii of HD186753B and TYC7096-222-1B: The First M-dwarfs known to Eclipse A-type StarsBentley, S. J.; Smalley, B.; Maxted, P. F. L. et alin Astronomy and Astrophysics (2009)We present observations of two new single-lined eclipsing binaries, both consisting of an Am star and an M-dwarf, discovered by the Wide Angle Search for Planets transit photometry survey. Using WASP ... [more ▼]We present observations of two new single-lined eclipsing binaries, both consisting of an Am star and an M-dwarf, discovered by the Wide Angle Search for Planets transit photometry survey. Using WASP photometry and spectroscopic measurements we find that HD186753B has an orbital period of $P=1.9194$ days, a mass of $M=0.24\pm0.02 M_{\odot}$ and radius of $R=0.31^{+0.06}_{-0.06} R_{\odot}$; and that TCY7096-222-1B has an orbital period of $P=8.9582$ days, a mass of between 0.29 and 0.54 $M_{\odot}$ depending on eccentricity and radius of $R=0.263^{+0.02}_{-0.07} R_{\odot}$. We find that the Am stars have relatively low rotational velocities that closely match the orbital velocities of the M-dwarfs, suggesting that they have been "spun-down" by the M-dwarfs. [less ▲]Detailed reference viewed: 19 (8 ULg) Masses of [70, l(+)] baryons in the 1/N-c expansionMatagne, Nicolas; Stancu, Floarea in Physical Review D (2006), 74(3), 034014The masses of positive parity [70,0(+)] and [70,2(+)] nonstrange and strange baryons are calculated in the 1/N-c expansion. The approach is based on the separation of a system of N-c quarks into an ... [more ▼]The masses of positive parity [70,0(+)] and [70,2(+)] nonstrange and strange baryons are calculated in the 1/N-c expansion. The approach is based on the separation of a system of N-c quarks into an excited core and an excited quark. The previous work for two flavor baryons is now extended to include strange baryons, to first order in SU(3)-flavor breaking. We show that the extension to N-f=3 maintains the regularities previously observed in the behavior of the linear term in N-c, of the spin-spin and of the spin-orbit terms. In particular the contribution of the spin-dependent terms decrease with the excitation energy, the dominant term remaining the spin-spin term. [less ▲]Detailed reference viewed: 10 (1 ULg) Masses of [70, l+] baryons in large N-c QCDMatagne, Nicolas; Stancu, Floarea in International Journal of Modern Physics A (2007), 22(2-3), 663-666Previous work is extended from SU(2) to SU(3) and we present results for the mass spectrum of the [70,l(+)](l=0,2) nonstrange and strange baryons in the 1/N-c expansion. We show that the dominant term is ... [more ▼]Previous work is extended from SU(2) to SU(3) and we present results for the mass spectrum of the [70,l(+)](l=0,2) nonstrange and strange baryons in the 1/N-c expansion. We show that the dominant term is the spin-spin interaction and its contribution vanishes at large excitations. [less ▲]Detailed reference viewed: 13 (1 ULg) Les masses rétropéritonéales chez l’enfant : à propos d’une tumeur de Wilms et d’un neuroblastomeMalaise, Olivier ; Vandenbosch, Kristel ; Uyttebroeck, Anna et alin Revue Médicale de Liège (2010), 65(3), 115-116Detection of a retroperitoneal mass in children needs a fast and accurate exploration. We present the case- reports of 2 children under the age of 5 years admitted to the University Hospital of Liège, one ... [more ▼]Detection of a retroperitoneal mass in children needs a fast and accurate exploration. We present the case- reports of 2 children under the age of 5 years admitted to the University Hospital of Liège, one with a Wilms tumor and one with a neuroblastoma. [less ▲]Detailed reference viewed: 91 (18 ULg) Massif anorthosites: another partisan reviewDuchesne, Jean-Clair in Brown, W. L. (Ed.) Feldspars and Feldspathoids (1984)Detailed reference viewed: 38 (1 ULg) Le massif anorthosito-leuconoritique d'Hidra et son faciès de bordureDemaiffe, Daniel; Duchesne, Jean-Clair ; Michot, Jean et alin Comptes Rendus des Séances de l'Académie des Sciences. Série D : Sciences Naturelles (1973), 277Detailed reference viewed: 34 (4 ULg) Massif-type anorthosites and related granitoids result from post-collisional remelting of a continental arc root: the Sveconorwegian caseVander Auwera, Jacqueline ; Bolle, Olivier ; Bingen, Bernard et alConference (2009)Detailed reference viewed: 26 (3 ULg) Massive binaries and colliding windsRauw, Grégor in EAS Publications Series (2004)In this contribution, I review recent results from observational investigations of early-type binaries of spectral types O and Wolf-Rayet. These studies aim at an accurate determination of fundamental ... [more ▼]In this contribution, I review recent results from observational investigations of early-type binaries of spectral types O and Wolf-Rayet. These studies aim at an accurate determination of fundamental parameters such as masses and radii of the most massive stars. In addition, multi-wavelength analyses of wind collisions in massive binaries provide constraints on the properties of stellar winds of massive stars and shock physics of cosmic plasmas. [less ▲]Detailed reference viewed: 4 (1 ULg) Massive binaries as seen with GAIAPalate, Matthieu ; Rauw, Grégor ; Gosset, Eric et alPoster (2010, July)Detailed reference viewed: 11 (3 ULg) Massive binaries as seen with GaiaPalate, Matthieu ; Rauw, Grégor ; Gosset, Eric et alin Bulletin de la Societe Royale des Sciences de Liege (2011), 80Gaia, ESA's forthcoming astrometric observatory, will observe a billion stars of our Galaxy, among which thousands of high-mass stars. In this contribution, we study the capabilities of Gaia's ... [more ▼]Gaia, ESA's forthcoming astrometric observatory, will observe a billion stars of our Galaxy, among which thousands of high-mass stars. In this contribution, we study the capabilities of Gaia's spectrometer (RVS) in the context of massive stars, especially the detectability of lower-mass companions to O-type stars. This preliminary study enables us to estimate to what extent Gaia will constrain the distribution of the physical and orbital parameters of massive binaries (luminosity, period, mass ratio, eccentricity...). [less ▲]Detailed reference viewed: 24 (4 ULg) The massive binary CPD-41 degrees 7742 - II. Optical light curve and X-ray observationsSana, H.; Antokhina, E.; Royer, P. et alin Astronomy and Astrophysics (2005), 441(1), 213-229In the first paper of this series, we presented a detailed high-resolution spectroscopic study of CPD - 41 degrees 7742, deriving for the first time an orbital solution for both components of the system ... [more ▼]In the first paper of this series, we presented a detailed high-resolution spectroscopic study of CPD - 41 degrees 7742, deriving for the first time an orbital solution for both components of the system. In this second paper, we focus on the analysis of the optical light curve and on recent XMM-Newton X-ray observations. In the optical, the system presents two eclipses, yielding an inclination i similar to 77 degrees. Combining the constraints from the photometry with the results of our previous work, we derive the absolute parameters of the system. We confirm that the two components of CPD- 41 degrees 7742 are main sequence stars (O9 V+ B1 - 1.5 V) with masses (M-1 similar to 18 M-. and M-2 similar to 10 M-.) and respective radii (R-1 similar to 7.5 R-. and R-2 similar to 5.4 R-.) close to the typical values expected for such stars. We also report an unprecedented set of X-ray observations that almost uniformly cover the 2.44-day orbital cycle. The X-ray emission from CPD-41 degrees 7742 is well described by a two-temperature thermal plasma model with energies close to 0.6 and 1.0 keV, thus slightly harder than typical early-type emission. The X-ray light curve shows clear signs of variability. The emission level is higher when the primary is in front of the secondary. During the high emission state, the system shows a drop of its X-ray emission that almost exactly matches the optical eclipse. We interpret the main features of the X-ray light curve as the signature of a wind-photosphere interaction, in which the overwhelming primary O9 star wind crashes into the secondary surface. Alternatively the light curve could result from a wind-wind interaction zone located near the secondary star surface. As a support to our interpretation, we provide a phenomenological geometric model that qualitatively reproduces the observed modulations of the X-ray emission. [less ▲]Detailed reference viewed: 18 (0 ULg) The massive binary CPD-41°7742 - I. High-resolution optical spectroscopySana, H.; Hensberge, H.; Rauw, Grégor et alin Astronomy and Astrophysics (2003), 405(3), 1063-1074We present the results of a spectroscopic campaign on the early-type binary CPD-41degrees 7742. For the first time, we unambiguously detect the secondary's spectral signature and derive an accurate ... [more ▼]We present the results of a spectroscopic campaign on the early-type binary CPD-41degrees 7742. For the first time, we unambiguously detect the secondary's spectral signature and derive an accurate orbital solution for both components of the system. We confirm that the orbit displays a slight but definite eccentricity (e=0.027+/-0.006) despite the short period (P=2.44070+/-0.00043 days). Previous radial velocity measurements available in the literature constitute together with our new observations a data set that spans more than 30 years. The combined primary orbital solution inferred is in excellent agreement with our solution and gives a period P=2.44062+/-0.00005 days. Based on spectroscopic criteria, we derive a spectral and luminosity classification of O9 III + B1 III. However, the luminosities and radii inferred from the membership of NGC6231 rather indicate lower luminosity classes. We show that the equivalent widths of well isolated primary lines display variations that suggest that CPD-41degrees 7742 is an eclipsing binary. This makes CPD-41degrees 7742 the second known SB2 eclipsing early-type binary of the NGC 6231 cluster. We approximately constrain the inclination of the system i(min) approximate to 60degrees. This may indicate that the system does not offer enough room for two stars with radii typical of giant stars and lends further support to a less evolved luminosity classification for at least one of the objects. [less ▲]Detailed reference viewed: 4 (0 ULg) The massive binary HD 152218 revisited: A new colliding wind system in NGC 6231Sana, H.; Nazé, Yaël ; O'Donnell, B. et alin New Astronomy (2008), 13(4), 202-215We present the results of an optical and X-ray monitoring campaign on the short-period massive SB2 binary HD 152218. Combining our HiRes spectroscopic data with previous observations, we unveil the ... [more ▼]We present the results of an optical and X-ray monitoring campaign on the short-period massive SB2 binary HD 152218. Combining our HiRes spectroscopic data with previous observations, we unveil the contradictions between the published orbital solutions. In particular, we solve the aliasing on the period and derive a value close to 5.604 d. Our eccentricity e = 0.259 +/- 0.006 is slightly lower than previously admitted. We show that HD 152218 is probably undergoing a relatively rapid apsidal motion of about 3 degrees yr(-1) and we confirm the O9IV + O9.7V classification. We derive minimal masses of 15.82 +/- 0.26 M-circle dot and 12.00 +/- 0.19 M-circle dot and constrain the radius of the components to R-1 = 10.3 +/- 1.3 R-circle dot and R-2 = 7.8 +/- 1.7 R-circle dot. We also report the results of an XMM-Newton monitoring of the HD 152218 X-ray emission throughout its orbital motion. The averaged X-ray spectrum is relatively soft and it is well reproduced by a 2-T optically thin thermal plasma model with component temperatures about 0.3 and 0.7 keV. The system presents an increase of its X-ray flux by about 30% near apastron compared to periastron, which is interpreted as the signature of an ongoing wind-wind interaction process occurring within the wind acceleration region. (C) 2007 Elsevier B.V. All rights reserved. [less ▲]Detailed reference viewed: 40 (3 ULg) Massive Depletion of Bovine Leukemia Virus Proviral Clones Located in Genomic Transcriptionally Active Sites During Primary InfectionGillet, Nicolas ; Gutiérrez, Gerónimo; Rodriguez, Sabrina et alin PLoS Pathogens (2013), 9(10), Deltaretroviruses such as human T-lymphotropic virus type 1 (HTLV-1) and bovine leukemia virus (BLV) induce a persistent infection generally asymptomatic but can also lead to leukemia or lymphoma. These ... [more ▼]Deltaretroviruses such as human T-lymphotropic virus type 1 (HTLV-1) and bovine leukemia virus (BLV) induce a persistent infection generally asymptomatic but can also lead to leukemia or lymphoma. These viruses replicate by infecting new lymphocytes (i.e. the infectious cycle) or via clonal expansion of the infected cells (mitotic cycle). The relative importance of these two cycles in viral replication varies during infection. The majority of infected clones are created early before the onset of an efficient immune response. Later on, the main replication route is mitotic expansion of pre-existing infected clones. Due to the paucity of available samples and for ethical reasons, only scarce data is available on early infection by HTLV-1. Therefore, we addressed this question in a comparative BLV model. We used high-throughput sequencing to map and quantify the insertion sites of the provirus in order to monitor the clonality of the BLV-infected cells population (i.e. the number of distinct clones and abundance of each clone). We found that BLV propagation shifts from cell neoinfection to clonal proliferation in about 2 months from inoculation. Initially, BLV proviral integration significantly favors transcribed regions of the genome. Negative selection then eliminates 97% of the clones detected at seroconversion and disfavors BLV-infected cells carrying a provirus located close to a promoter or a gene. Nevertheless, among the surviving proviruses, clone abundance positively correlates with proximity of the provirus to a transcribed region. Two opposite forces thus operate during primary infection and dictate the fate of long term clonal composition: (1) initial integration inside genes or promoters and (2) host negative selection disfavoring proviruses located next to transcribed regions. The result of this initial response will contribute to the proviral load set point value as clonal abundance will benefit from carrying a provirus in transcribed regions. [less ▲]Detailed reference viewed: 44 (20 ULg) Massive Depletion of Bovine Leukemia Virus Proviral Clones Located in Genomic Transcriptionally Active Sites During Primary InfectionGillet, Nicolas ; Gutiérrez, Gerónimo; Rodriguez, Sabrina et alConference (2013, June 29)Detailed reference viewed: 12 (5 ULg) A 'Massive Dramatic Plumpudding': The Politics of Reception in the Antwerp Performance of Shelley’s The Cenci’Steyaert, Kris in Keats-Shelley Journal (2001), 50Detailed reference viewed: 21 (2 ULg) Massive Ketonuria During Sedation with Propofol in a 12 Year Old Girl with Severe Head TraumaCanivet, Jean-Luc ; Gustad, K.; Leclercq, P. et alin Acta Anaesthesiologica Belgica (1994), 45(1), 19-22Severe ketonuria developed during sedation with propofol in a 12 year old girl with brain injury. Deep sedation with propofol (5.1 mg/kg/h) was required because of agitation and severe intracranial ... [more ▼]Severe ketonuria developed during sedation with propofol in a 12 year old girl with brain injury. Deep sedation with propofol (5.1 mg/kg/h) was required because of agitation and severe intracranial hypertension; as a part of our management protocol, glucose intake was restricted to 5 Kcal/h. After 18 hours of propofol infusion there was intense ketonuria (8+ by Ketostix) without any evidence of metabolic acidosis (pH, HCO3- and anion gap were within normal values). At this time, indirect calorimetry (Deltatrac) confirmed that energy expenditure was principally based on fat consumption (70% of energy expenditure). Lowering the propofol infusion rate and increasing glucose intake reduced fat consumption to 39% within 8 hours: at this time, Ketostix was negative for ketone bodies. This case illustrates a potential risk of ketonuria during prolonged sedation with propofol (a 10% solution of intralipid), particularly if glucose intake is restricted. Monitoring urinary ketone bodies is recommended under these circumstances. [less ▲]Detailed reference viewed: 28 (4 ULg) Massive Non-Thermal Radio Emitters: New Data and their ModelingVolpi, D.; Blomme, R.; De Becker, Michaël et alin Astronomical Society of the Pacific Conference Series (2013, January 01)During recent years some non-thermal radio emitting OB stars have been discovered to be binary or multiple systems. The non-thermal emission is due to synchrotron radiation that is emitted by electrons ... [more ▼]During recent years some non-thermal radio emitting OB stars have been discovered to be binary or multiple systems. The non-thermal emission is due to synchrotron radiation that is emitted by electrons accelerated up to high energies. The electron acceleration occurs at the strong shocks created by the collision of radiatively-driven winds. Here we summarize the available radio data and more recent observations for the binary Cyg OB2 No. 9. We also show a new emission model which is being developed to compare the theoretical total radio flux and the spectral index with the observed radio light curves. This comparison will be useful in order to solve fundamental questions, such as the determination of the stellar mass-loss rates, which are perturbed by clumping. [less ▲]Detailed reference viewed: 14 (3 ULg)
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