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See detailK voprosou bidelenii fatsii zoubtchatogo moustié na materialakh pamyatnikov sredneï azii
Krivoshapkin, A.; Kolobova, K.; Pavlenok, K. et al

Scientific conference (2011)

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See detailK+ Production in a Cascade Model for High Energy Nucleus-Nucleus Collisions
Cugnon, Joseph ULiege; Lombard

in Nuclear Physics A (1984), 422

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See detailLe K-ABC utilisé avec des enfants trisomiques 21 : Un essai d’adaptation
Frenkel, Stéphanie ULiege; Bourdin, Béatrice; Vandromme, Luc

Conference (2001)

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See detailLe K-ABC utilisé avec des enfants trisomiques 21 : Un essai d’adaptation
Frenkel, Stéphanie ULiege; Bourdin, Béatrice; Vandromme, luc

in Vivicorsi, Bruno; Collet, R. (Eds.) Handicap, cognition et prise en charge individuelle : des aspects de la recherche au respect de la personne (2005)

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See detailK-excess, an unexploited method for discovering red quasars
Nakos, T.; Willis, J.; Andreon, S. et al

Conference (2006, May 19)

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See detailK-shell photoabsorption and photoionization of trace elements. I. Isoelectronic sequences with electron number 3 <= N <= 11
Palmeri, P.; Quinet, Pascal ULiege; Bautista, M.A. et al

in Astronomy and Astrophysics (2016), 589

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See detailK-shell photoabsorption and photoionization of trace elements: II. Isoelectronic sequences with electron number 12 ≤ N ≤ 18
Mendoza, C.; Bautista, M. A.; Palmeri, P. et al

in Astronomy and Astrophysics (2017), 604

Context. We are concerned with improving the diagnostic potential of the K lines and edges of elements with low cosmic abundances, namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn, that are ... [more ▼]

Context. We are concerned with improving the diagnostic potential of the K lines and edges of elements with low cosmic abundances, namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn, that are observed in the X-ray spectra of supernova remnants, galaxy clusters, and accreting black holes and neutron stars. Aims. Since accurate photoabsorption and photoionization cross sections are needed in their spectral models, they have been computed for isoelectronic sequences with electron number 12 ≤ N ≤ 18 using a multi-channel method. Methods. Target representations are obtained with the atomic structure code autostructure, and ground-state cross sections are computed with the Breit-Pauli R-matrix method (bprm) in intermediate coupling, including damping (radiative and Auger) effects. Results. Following the findings in our earlier work on sequences with 2 ≤ N ≤ 11, the contributions from channels associated with the 2s-hole [2s]μ target configurations and those containing 3d orbitals are studied in the Mg (N = 12) and Ar (N = 18) isoelectronic sequences. Cross sections for the latter ions are also calculated in the isolated-resonance approximation as implemented in autostructure and compared with bprm to test their accuracy. Conclusions. It is confirmed that the collisional channels associated with the [2s]μ target configurations must be taken into account owing to significant increases in the monotonic background cross section between the L and K edges. Target configurations with 3d orbitals give rise to fairly conspicuous unresolved transition arrays in the L-edge region, but to a much lesser extent in the K-edge that is our main concern; therefore, they have been neglected throughout owing to their computationally intractable channel inventory, thus allowing the computation of cross sections for all the ions with 12 ≤ N ≤ 18 in intermediate coupling with bprm. We find that the isolated-resonance approximations performs satisfactorily and will be our best choice to tackle the systems with ground configuration 3p63dm (3 ≤ m ≤ 8) in isoelectronic sequences with N > 20. © ESO 2017. [less ▲]

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See detailK-shell photoabsorption and photoionization of trace elements: III. Isoelectronic sequences with electron number 19 ≤ N ≤ 26
Mendoza, C.; Bautista, M. A.; Palmeri, P. et al

in Astronomy and Astrophysics (2018), 616

Context. This is the final report of a three-paper series on the K-shell photoabsorption and photoionization of trace elements (low cosmic abundance), namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu ... [more ▼]

Context. This is the final report of a three-paper series on the K-shell photoabsorption and photoionization of trace elements (low cosmic abundance), namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn. K lines and edges from such elements are observed in the X-ray spectra of supernova remnants, galaxy clusters, and accreting black holes and neutron stars, their diagnostic potential being limited by poor atomic data. Aims. We here complete the previously reported radiative datasets with new photoabsorption and photoionization cross sections for isoelectronic sequences with electron number 19 = N = 26. We also describe the access to and integrity and usability of the whole resulting atomic database. Methods. Target representations were obtained with the atomic structure code AUTOSTRUCTURE. Where possible, cross sections for ground-configuration states were computed with the Breit Pauli R-matrix method (BPRM) in either intermediate or LS coupling including damping (radiative and Auger) effects; otherwise and more generally, they were generated in the isolated-resonance approximation with AUTOSTRUCTURE. Results. Cross sections were computed with BPRM only for the K (N = 19) and Ca (N = 20) isoelectronic sequences, the latter in LS coupling. For the remaining sequences (21 = N = 26), AUTOSTRUCTURE was run in LS-coupling mode taking into account damping effects. Comparisons between these two methods for K-like Zn xii and Ca-like Zn xi show that to ensure reasonable accuracy, the LS calculations must be performed taking into account the non-fine-structure relativistic corrections. The original data structures of the BPRM and AUTOSTRUCTURE output files, namely photoabsorption and total and partial photoionization cross sections, are maintained but supplemented with files detailing the target (NT-electron system, where NT = N-1) representations and photon states (N-electron system). Conclusions. We conclude that because of the large target size, the photoionization of ions with N > 20 involving inner-shell excitations rapidly leads to untractable BPRM calculations, and is then more effectively treated in the isolated resonance approximation with AUTOSTRUCTURE. This latter approximation by no means involves small calculations as Auger damping must be explicitly specified in the intricate decay routes. © 2018 ESO. [less ▲]

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See detailK-shell photoionization and photoabsorption of Ne, Mg, Si, S, Ar and Ca
Witthoeft, M; Bautista, M A; Mendoza, C et al

in Astrophysical Journal Supplement Series (2009), 182

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See detailK-shell photoionization of highly-charged iron ions under high-density astrophysical plasma conditions
Deprince, J.; Bautista, M.A.; Fritzsche, S. et al

Poster (2019)

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See detailK-shell photoionization of Na-like to Cl)like ions of Mg, Si, S, Ar and Ca
Witthoeft, M; Garcia, J; Kallman, T R et al

in Astrophysical Journal Supplement Series (2011), 192

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See detailK-shell photoionization of Nickel ions using R-matrix
Witthoeft, M C; Bautista, M A; Garcia, J et al

in Astrophysical Journal Supplement Series (2011), 196

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See detailK-type geomagnetic index nowcast with data quality control
Stankov, Stanimir; Stegen, Koen; Warnant, René ULiege

in Annals of Geophysics (2011), 54(3), 285-295

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See detailThe K1 beta-lactamase of Klebsiella pneumoniae.
Joris, Bernard ULiege; De Meester, F; Galleni, Moreno ULiege et al

in Biochemical Journal (1987), 243(2), 561-7

beta-Lactamase K1 was purified from Klebsiella pneumoniae SC10436. It is very similar to the enzyme produced by Klebsiella aerogenes 1082E and described by Emanuel, Gagnon & Waley [Biochem. J. (1986) 234 ... [more ▼]

beta-Lactamase K1 was purified from Klebsiella pneumoniae SC10436. It is very similar to the enzyme produced by Klebsiella aerogenes 1082E and described by Emanuel, Gagnon & Waley [Biochem. J. (1986) 234, 343-347]. An active-site peptide was isolated after labelling of the enzyme with tritiated beta-iodopenicillanate. A cysteine residue was found just before the active-site serine residue. This result could explain the properties of the enzyme after modification by thiol-blocking reagents. The sequence of the active-site peptide clearly established the enzyme as a class A beta-lactamase. [less ▲]

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See detailThe K2-ESPRINT Project I: Discovery of the Disintegrating Rocky Planet K2-22b with a Cometary Head and Leading Tail
Sanchis-Ojeda, R.; Rappaport, S.; Pallé, E. et al

in Astrophysical Journal (2015), 812(2), 112

We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from ∼0% to 1.3%, are suggestive of ... [more ▼]

We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from ∼0% to 1.3%, are suggestive of a planet that is disintegrating via the emission of dusty effluents. We characterize the host star as an M-dwarf with Teff ≃ 3800 K. We have obtained ground-based transit measurements with several 1-m class telescopes and with the GTC. These observations (1) improve the transit ephemeris; (2) confirm the variable nature of the transit depths; (3) indicate variations in the transit shapes; and (4) demonstrate clearly that at least on one occasion the transit depths were significantly wavelength dependent. The latter three effects tend to indicate extinction of starlight by dust rather than by any combination of solid bodies. The K2 observations yield a folded light curve with lower time resolution but with substantially better statistical precision compared with the ground-based observations. We detect a significant “bump” just after the transit egress, and a less significant bump just prior to transit ingress. We interpret these bumps in the context of a planet that is not only likely streaming a dust tail behind it, but also has a more prominent leading dust trail that precedes it. This effect is modeled in terms of dust grains that can escape to beyond the planet's Hill sphere and effectively undergo “Roche lobe overflow,” even though the planet's surface is likely underfilling its Roche lobe by a factor of 2. [less ▲]

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See detailKaberdoes
Vromans, Joseph ULiege

in Nederlands Van Nu (1993), 41(5),

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See detail"Kadenzen des ganzen Körpers" - Das Sich-Bewegen des Musikers.
Viehöver, Vera ULiege; Wunsch, Stephan

in Görling, Reinhold; Skrandies, Timo; Trinkaus, Stephan (Eds.) Geste - Bewegungen zwischen Film und Tanz (2009)

Detailed reference viewed: 108 (4 ULiège)
See detailKaffee, Cognac, Marmelade: Verfahrenstechnik im Alltagsleben
Pfennig, Andreas ULiege

Conference (2004, October 11)

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