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Distribution by Scientific Domains

Physics and Astronomy	50%

Selected Abstracts

Modified regional self-interaction corrected time-dependent density functional theory for core excited-state calculations

JOURNAL OF COMPUTATIONAL CHEMISTRY, Issue 16 2009
Ayako Nakata
Abstract A modified regional self-interaction correction (mRSIC) method is proposed for obtaining accurate core-excitation energies in time-dependent density functional theory (TDDFT) calculations. The mRSIC method is an improvement of the RSIC method (Tsuneda et al. J Comput Chem 2003, 24, 1592). It takes into account the energy contributions from 2s and higher atomic orbitals that the RSIC method neglects. Furthermore, mRSIC improves the poor description for the nuclear-electron cusp of Gaussian basis functions. The mRSIC method was combined with a long-range correction (LC) scheme, which has been proved to give accurate valence-, Rydberg-, and charge transfer (CT)-excitation energies. In so doing, it dramatically improved the accuracy of the calculated core-excitation energies and did not affect the already accurate values of valence-, Rydberg-, and CT-excitation energies produced by the LC functionals. These results mean that the combined scheme is accurate for all excitation energy forms. © 2009 Wiley Periodicals, Inc. J Comput Chem 2009 [source]

Intracluster light and the extended stellar envelopes of cD galaxies: an analytical description

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 4 2007
Marc S. Seigar
ABSTRACT We have analysed deep R -band images, down to a limiting surface brightness of 26.5 R-mag arcsec,2 (equivalent to ,28 B-mag arcsec,2), of five cD galaxies to determine the shape of the surface brightness profiles of their extended stellar envelopes. Both de Vaucouleurs R1/4 and Sérsic R1/n models, on their own, provide a poor description of the surface brightness profiles of cD galaxies. This is due to the presence of outer stellar envelopes, thought to have accumulated over the merger history of the central cluster galaxy and also from the tidal stripping of galaxies at larger cluster radii. We therefore simultaneously fit two Sérsic functions to measure the shape of the inner and outer components of the cD galaxies. We show that, for three out of our five galaxies, the surface brightness profiles are best fitted by an inner Sérsic model, with indices n, 1 ,6, and an outer exponential component. For these systems, the galaxy-to-envelope size ratio is 0.1,0.4 and the contribution of the stellar envelope to the total R -band light (i.e. galaxy + envelope) is around 60,80 per cent (based on extrapolation to a 300 kpc radius). The exceptions are NGC 6173, for which our surface brightness profile modelling is consistent with just a single component (i.e. no envelope) and NGC 4874 which appears to have an envelope with a de Vaucouleurs, rather than exponential, profile. [source]

Management and outcomes of facial paralysis from intratemporal blunt trauma: A systematic review,,

THE LARYNGOSCOPE, Issue 7 2010
John J. Nash MD
Abstract Objectives/Hypothesis: To systematically review the existing literature on outcomes and management of facial paralysis resulting from intratemporal blunt trauma. Study Design: Systematic review of the literature. Methods: Thirty-five articles met our inclusion criteria. Outcome variables analyzed included severity of paralysis, time of onset of paralysis, surgical or nonsurgical management, steroid use, and final facial nerve function. Results: All studies were classified as level 4 evidence as defined by the Oxford Centre for Evidence-Based Medicine. There was marked variation in the quality of the studies with inconsistent outcome measures, diagnostic testing, and follow-up, thus ruling out a formal meta-analysis. In an exploratory pooling of data, 612 cases had sufficient follow-up and facial movement grading for some evaluation of trends. In 189 patients who were followed observationally, 66% achieved an outcome equivalent to House-Brackmann (HB) I, 25% achieving HB II-V, and two patients an HB VI score. Among 83 patients treated with steroids, 67% achieved HB I, 30% HB II-V, and no patients with HB VI. In 340 patients treated surgically, 23% achieved HB I postoperatively, 58% were graded as HB II-V, and 9% with HB grade VI postoperatively. No patient presenting with partial paralysis had an HB VI outcome. Conclusions: The role of surgery versus nonsurgical interventions for this clinical entity remains inconclusive. Level 4 evidence studies predominate and are further hindered by poor description of outcome measures and incomplete data reporting. Exploratory pooling of data without formal meta-analysis suggests the need to compare any intervention to the natural course of healing, which overall appears to be favorable. Laryngoscope, 2010 [source]

Nearby stars of the Galactic disk and halo.

ASTRONOMISCHE NACHRICHTEN, Issue 1 2004

Abstract High-resolution spectroscopic observations of about 150 nearby stars or star systems are presented and discussed. The study of these and another 100 objects of the previous papers of this series implies that the Galaxy became reality 13 or 14 Gyr ago with the implementation of a massive, rotationally-supported population of thick-disk stars. The very high star formation rate in that phase gave rise to a rapid metal enrichment and an expulsion of gas in supernovae-driven Galactic winds, but was followed by a star formation gap for no less than three billion years at the Sun's galactocentric distance. In a second phase, then, the thin disk , our "familiar Milky Way" , came on stage. Nowadays it traces the bright side of the Galaxy, but it is also embedded in a huge coffin of dead thick-disk stars that account for a large amount of baryonic dark matter. As opposed to this, cold-dark-matter-dominated cosmologies that suggest a more gradual hierarchical buildup through mergers of minor structures, though popular, are a poor description for the Milky Way Galaxy , and by inference many other spirals as well , if, as the sample implies, the fossil records of its long-lived stars do not stick to this paradigm. Apart from this general picture that emerges with reference to the entire sample stars, a good deal of the present work is however also concerned with detailed discussions of many individual objects. Among the most interesting we mention the blue straggler or merger candidates HD 165401 and HD 137763/HD 137778, the likely accretion of a giant planet or brown dwarf on 59 Vir in its recent history, and HD 63433 that proves to be a young solar analog at , , 200 Myr. Likewise, the secondary to HR 4867, formerly suspected non-single from the Hipparcos astrometry, is directly detectable in the highresolution spectroscopic tracings, whereas the visual binary , Cet is instead at least triple, and presumably even quadruple. With respect to the nearby young stars a complete account of the UrsaMajor Association is presented, and we provide as well plain evidence for another, the "Hercules-Lyra Association", the likely existence of which was only realized in recent years. On account of its rotation, chemistry, and age we do confirm that the Sun is very typical among its G-type neighbors; as to its kinematics, it appears however not unlikely that the Sun's known low peculiar space velocity could indeed be the cause for the weak paleontological record of mass extinctions and major impact events on our parent planet during the most recent Galactic plane passage of the solar system. Although the significance of this correlation certainly remains a matter of debate for years to come, we point in this context to the principal importance of the thick disk for a complete census with respect to the local surface and volume densities. Other important effects that can be ascribed to this dark stellar population comprise (i) the observed plateau in the shape of the luminosity function of the local FGK stars, (ii) a small though systematic effect on the basic solar motion, (iii) a reassessment of the term "asymmetrical drift velocity" for the remainder (i.e. the thin disk) of the stellar objects, (iv) its ability to account for the bulk of the recently discovered high-velocity blue white dwarfs, (v) its major contribution to the Sun's ,220 km s,1 rotational velocity around the Galactic center, and (vi) the significant flattening that it imposes on the Milky Way's rotation curve. Finally we note a high multiplicity fraction in the small but volume-complete local sample of stars of this ancient population. This in turn is highly suggestive for a star formation scenario wherein the few existing single stellar objects might only arise from either late mergers or the dynamical ejection of former triple or higher level star systems. (© 2004 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source]