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
See detailForaminifères, Spores et Coraux du Famennien supérieur et du Dinantien du Massif de l'Omolon (Extrème-Orient soviétique).
Conil, R; Poty, E; Simakov, K.V. et al

in Annales de la Société Géologique de Belgique (1982), 105

Detailed reference viewed: 24 (0 ULg)
Full Text
See detailForbidden FeIII-lines in celestial spectra
Edlén, B.; Swings, Polydore ULg

in Observatory (The) (1939), 62

Detailed reference viewed: 6 (0 ULg)
Full Text
Peer Reviewed
See detailThe forbidden line spectrum in the edges of H II regions
Manfroid, Jean ULg

in Astrophysics & Space Science (1977), 48

It is shown analytically that the motion of exciting stars can affect the forbidden emission-line spectra of H II regions in an observable manner. A model is used which comprises a small solid angle of a ... [more ▼]

It is shown analytically that the motion of exciting stars can affect the forbidden emission-line spectra of H II regions in an observable manner. A model is used which comprises a small solid angle of a spherical nebula that is symmetric with respect to the direction of stellar motion and consists of a mixture of H, He, C, N, O, and Ne with ionization states up to He II, C III, N III, O III, and Ne III. Consideration is given to the case of a 36-solar-mass O5 star with an effective temperature of 43,000 K moving at a velocity of 10 km/s in a nebula having a density of 10 times the proton mass per cu cm. The results obtained indicate that: (1) the region where forbidden lines characteristic of ionization fronts are produced is broadened considerably at the trailing edge of the nebula; (2) the spectrum in this region is comparable to that of fossil H II regions; and (3) the ionization front at the leading edge is sharper, the temperature there is higher, and the forbidden-line spectrum is similar to that of young ionization fronts. [less ▲]

Detailed reference viewed: 8 (0 ULg)
Peer Reviewed
See detailForbidden Lines in 6pk (j=1-5) configurations
Biémont, Emile ULg; Quinet, Pascal ULg

in Physica Scripta (1996), 54

Detailed reference viewed: 7 (1 ULg)
Peer Reviewed
See detailForbidden Lines in 6pk (k=1-5) configurations
Biémont, Emile ULg; Quinet, Pascal ULg

Conference (1995)

Detailed reference viewed: 6 (0 ULg)
Full Text
Peer Reviewed
See detailForbidden lines in a newly formed H II region
Manfroid, Jean ULg

in Astronomy and Astrophysics (1975), 43

The initial evolution of a spherically symmetric H II region forming around a star of 36 solar masses is calculated numerically using a program based on a finite-difference scheme extrapolated from those ... [more ▼]

The initial evolution of a spherically symmetric H II region forming around a star of 36 solar masses is calculated numerically using a program based on a finite-difference scheme extrapolated from those previously proposed for solving hydrodynamic problems involving shock waves. The helium abundance is assumed to be 10 per cent, and no account is taken of magnetic fields, turbulent motions, or interstellar grains. The evolution of the positions of the hydrogen and helium ionization fronts is plotted as a function of time, and the total spectra of the forbidden emission lines of C II, N II, N III, O II, O III, Ne II, and Ne III are computed at each time. The intensities of the 29 strongest lines at five different epochs are compared with a rough estimate of the total strength of H-beta. The temporal evolution of the nebula and the emission lines is described qualitatively. [less ▲]

Detailed reference viewed: 14 (0 ULg)
Full Text
See detailForbidden lines of CrII, Ni II, and Fe II
Swings, Polydore ULg

in Publications of the Astronomical Society of the Pacific [=PASP] (1944), 56

Detailed reference viewed: 8 (1 ULg)
Full Text
See detailForbidden lines of ionized nickel in the spectra of bright-line stars
Swings, Polydore ULg

in Publications of the Astronomical Society of the Pacific [=PASP] (1943), 55

Detailed reference viewed: 9 (0 ULg)
Full Text
Peer Reviewed
See detailForbidden oxygen lines at various nucleocentric distances in comets
Decock, Alice ULg; Jehin, Emmanuel ULg; Rousselot, P. et al

in Astronomy and Astrophysics (2015), 573

Aims: We study the formation of the [OI] lines - that is, 5577.339 Å (the green line), 6300.304 Å and 6363.776 Å (the two red lines) - in the coma of comets and determine the parent species of the oxygen ... [more ▼]

Aims: We study the formation of the [OI] lines - that is, 5577.339 Å (the green line), 6300.304 Å and 6363.776 Å (the two red lines) - in the coma of comets and determine the parent species of the oxygen atoms using the ratio of the green-to-red-doublet emission intensity, I[SUB]5577[/SUB]/(I[SUB]6300[/SUB] + I[SUB]6364[/SUB]), (hereafter the G/R ratio) and the line velocity widths. <BR /> Methods: We acquired high-resolution spectroscopic observations at the ESO Very Large Telescope of comets C/2002 T7 (LINEAR), 73P-C/Schwassmann-Wachmann 3, 8P/Tuttle, and 103P/Hartley 2 when they were close to Earth (<0.6 au). Using the observed spectra, which have a high spatial resolution (<60 km/pixel), we determined the intensities and widths of the three [OI] lines. We spatially extracted the spectra to achieve the best possible resolution of about 1-2'', that is, nucleocentric projected distances of 100 to 400 km depending on the geocentric distance of the comet. We decontaminated the [OI] green line from C[SUB]2[/SUB] lines blends that we identified. <BR /> Results: The observed G/R ratio in all four comets varies as a function of nucleocentric projected distance (between ~0.25 to ~0.05 within 1000 km). This is mainly due to the collisional quenching of O([SUP]1[/SUP]S) and O([SUP]1[/SUP]D) by water molecules in the inner coma. The observed green emission line width is about 2.5 km s[SUP]-1[/SUP] and decreases as the distance from the nucleus increases, which can be explained by the varying contribution of CO[SUB]2[/SUB] to the O([SUP]1[/SUP]S) production in the innermost coma. The photodissociation of CO[SUB]2[/SUB] molecules seem to produce O([SUP]1[/SUP]S) closer to the nucleus, while the water molecule forms all the O([SUP]1[/SUP]S) and O([SUP]1[/SUP]D) atoms beyond 10[SUP]3[/SUP] km. Thus we conclude that the main parent species producing O([SUP]1[/SUP]S) and O([SUP]1[/SUP]D) in the inner coma is not always the same. The observations have been interpreted in the framework of the previously described coupled-chemistry-emission model, and the upper limits of the relative abundances of CO[SUB]2[/SUB] were derived from the observed G/R ratios. Measuring the [OI] lines might provide a new way to determine the CO[SUB]2[/SUB] relative abundance in comets. Based on observations made with ESO Telescope at the La Silla Paranal Observatory under programs ID 073.C-0525, 277.C-5016, 080.C-0615 and 086.C-0958.Tables 3 and 4 are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201424403/olm">http://www.aanda.org</A> [less ▲]

Detailed reference viewed: 13 (2 ULg)
Full Text
Peer Reviewed
See detailForbidden oxygen lines in comets at various heliocentric distances
Decock, Alice ULg; Jehin, Emmanuel ULg; Hutsemekers, Damien ULg et al

in Astronomy and Astrophysics (2013), 555

We present a study of the three forbidden oxygen lines [OI] located in the optical region - i.e., 5577.339 Å (the green line), 6300.304 Å and 6363.776 Å (the two red lines) - in order to better understand ... [more ▼]

We present a study of the three forbidden oxygen lines [OI] located in the optical region - i.e., 5577.339 Å (the green line), 6300.304 Å and 6363.776 Å (the two red lines) - in order to better understand the production of these atoms in cometary atmospheres. The analysis is based on 48 high-resolution and high signal-to-noise spectra collected with UVES at the ESO VLT between 2003 and 2011 referring to 12 comets of different origins observed at various heliocentric distances. The flux ratio of the green line to the sum of the two red lines is evaluated to determine the parent species of the oxygen atoms by comparison with theoretical models. This analysis confirms that, at about 1 AU, H[SUB]2[/SUB]O is the main parent molecule producing oxygen atoms. At heliocentric distances >2.5 AU, this ratio changes rapidly, an indication that other molecules are starting to contribute. The most abundant species after H[SUB]2[/SUB]O in the coma, CO and CO[SUB]2[/SUB], are good candidates, and the ratio is used to estimate their abundances. We found that the CO[SUB]2[/SUB] abundance relative to H[SUB]2[/SUB]O in comet C/2001 Q4 (NEAT) observed at 4 AU can be as high as ~70%. The intrinsic widths of the oxygen lines were also measured. The green line is on average about 1 km s[SUP]-1[/SUP] broader than the red lines, while the theory predicts that the red lines are broader. This might be due to the nature of the excitation source or to a contribution of CO[SUB]2[/SUB] as the parent molecule of the 5577.339 Å line. At 4 AU, we found that the width of the green and red lines in comet C/2001 Q4 are the same, which could be explained if CO[SUB]2[/SUB] becomes the main contributor to the three [OI] lines at high heliocentric distances. Based on observations made with ESO Telescope at the La Silla Paranal Observatory under programs ID 268.C-5570, 270.C-5043, 073.C-0525, 274.C-5015, 075.C-0355, 080.C-0615, 280.C-5053, 086.C-0958, and 087.C-0929. [less ▲]

Detailed reference viewed: 13 (1 ULg)
See detailForbidden transitions in Fe II
Quinet, Pascal ULg; Le Dourneu, M; Zeippen, C J

in Proceedings of the 5th International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas (1996)

Detailed reference viewed: 16 (0 ULg)
Peer Reviewed
See detailForbidden transitions of Astrophysical Interest in the 5pk (k=1-5) Configurations
Biémont, Emile ULg; Hansen, J. E.; Quinet, Pascal ULg et al

in Astronomy and Astrophysics. Supplement Series (1995), 111

Detailed reference viewed: 13 (1 ULg)
Peer Reviewed
See detailForbidding Bodies: Avatars of the Phisical in the Work of Janet Frame
Delrez, Marc ULg

Conference (2002, April 23)

Detailed reference viewed: 12 (0 ULg)
Full Text
Peer Reviewed
See detailForbidding Bodies: Avatars of the Physical in the Work of Janet Frame
Delrez, Marc ULg

in World Literature Written in English (2004), 38(2), 70-79

Detailed reference viewed: 38 (8 ULg)
Full Text
Peer Reviewed
See detailLa force du mi-dit : Figures de style dans le roman de Lawrence Scott, Witchbroom
Pagnoulle, Christine ULg

in Palimpsestes (2005), 16

Beyond some obvious comparisons, the article traces the function of some embedded metaphors, and the kind of problem they may raise in a translation.

Detailed reference viewed: 31 (4 ULg)
See detailForce Limiting at CSL premises
Grodent, Christophe ULg; Cucchiaro, Antonio ULg; ronchain, philippe

(2001, June)

Detailed reference viewed: 19 (6 ULg)
Full Text
Peer Reviewed
See detailForce musculaire isocinétique du couple quadriceps / ischio-jambiers des joueurs de rugby professionnels
Julia, Marc; Pereira, B.; Morand, D. et al

in Résumés des communications orales SFTS (2012, October)

Detailed reference viewed: 148 (7 ULg)
Full Text
Peer Reviewed
See detailLa force persuasive de l'Idéo-graphie
Leclercq, Bruno ULg

Conference (2010, April 17)

Detailed reference viewed: 18 (0 ULg)
Full Text
Peer Reviewed
See detailForce plate : Gold standard ?
Balligand, Marc ULg

in Proceedings of the 20th ECVS Congress (2011)

Detailed reference viewed: 15 (0 ULg)
Full Text
Peer Reviewed
See detail- La force probante de la preuve irrégulièrement recueillie : Antigone aurait-elle perdu son âme ?
Jacobs, Ann ULg

in Saint-Pau, Jean Christophe; Bergeaud, Aurélie (Eds.) La preuve pénale – Problèmes contemporains en droit comparé (2012)

Jurisprudence belge en matière de preuve illégale et irrégulière.

Detailed reference viewed: 65 (1 ULg)