bluuebunny/crossref_metadata_2025_split huggingface dataset:
Outcome of Pectoralis Major Myomammary Flap for Post‐mastectomy Breast Reconstruction: Extended Experience
Authors: Denewer Adel , Setit Ahmed , Farouk Omar 
Published: May 2007

AbstractBackgroundIn the past decade there has been an enormously expanding interest among rural Egyptian patients, relatives, and treating oncologists in post‐mastectomy reconstruction as an integral part of patient care. We introduced our technique of pectoralis major myomammary cutaneous flap for single‐stage reconstruction of large breasts, nipple, and areola.MethodsThe new technique is based on performing modified radical mastectomy in the classic manner, and then using a pectoralis major myocutaneous pedicled flap from the other side in breast reconstruction. The flap is based on the pectoral branch of the thoracoacromial artery, and a sector from the medial part of the healthy breast with its overlying skin and a part of the nipple–areola complex is included with the flap. This technique was used in our center in one 118 patients, with very promising results.ResultsMajor flap necrosis was not observed in patients treated with this technique, and there were no local recurrences observed during the follow‐up period. Excellent cosmetic results were achieved in 49 of the 118 (41.5%) cases.ConclusionWe recommend this new technique as a single‐stage, simple solution for reconstruction of large breasts after mastectomy
Self-organised synthesis of Rh nanostructures with tunable chemical reactivity
Authors: Buatier de Mongeot F , Toma A , Molle A , Lizzit S , Petaccia L , Baraldi A 
Published: May 2007

Abstract
Nonequilibrium periodic nanostructures such as nanoscale ripples, mounds and rhomboidal pyramids formed on Rh(110) are particularly interesting as candidate model systems with enhanced catalytic reactivity, since they are endowed with steep facets running along nonequilibrium low-symmetry directions, exposing a high density of undercoordinated atoms. In this review we report on the formation of these novel nanostructured surfaces, a kinetic process which can be controlled by changing parameters such as temperature, sputtering ion flux and energy. The role of surface morphology with respect to chemical reactivity is investigated by analysing the carbon monoxide dissociation probability on the different nanostructured surfaces.
Rigid Endoscopes
Authors: MacDonald Ellen 
Published: May 2007

This is the third article on the care and maintenance of rigid endoscopic instruments. the first focused on prescribtive guidelines and rationale for handling, cleaning, and sterilizing rigid endoscopes.1 The second dealt with care and maintenance of telescopes, light cables, and light sources.2 This article examines care and maintenance of high frequency cables, resctoscope loops, sheaths, cannulas, forceps, and scissors.High‐Frequency Cables
Adult scoliosis: A personal experience
Authors: Reeder Jean M 
Published: May 2007

My thoughts were far from the road as I drove away from my appointment with an orthopedic surgeon. He had recommended a posterior spinal fusion to correct my scoliosis. I was confronted with the reality that my busy organized life as a wife and military nurse would be disrupted. Roles would be reversed. I would soon be a patient facing a major surgical procedure and lengthy recovery. I anticipated this experience with much anxiety. It offered, however, the potential for personal and professional growth. I focused on this as a coping mechanism and as a means to channel my increasing anxiety.As a result of my firsthand surgical experience, I was to find my perceptions about nursing care altered and my commitment to caring strengthened.
THE GENERALIZED HOMOLOGY OF PRODUCTS
Authors: HOVEY MARK 
Published: May 2007

Abstract.We construct a spectral sequence that computes the generalized homology E*(∏ Xα) of a product of spectra. The E2-term of this spectral sequence consists of the right derived functors of product in the category of E*E-comodules, and the spectral sequence always converges when E is the Johnson-Wilson theory E(n) and the Xα are Ln-local. We are able to prove some results about the E2-term of this spectral sequence; in particular, we show that the E(n)-homology of a product of E(n)-module spectra Xα is just the comodule product of the E(n)*Xα. This spectral sequence is relevant to the chromatic splitting conjecture.
RECURRENCE RELATIONS, DYNKIN DIAGRAMS AND PLÜCKER FORMULAE
Authors: BURNS JOHN M. , CLANCY MICHAEL J. 
Published: May 2007

Abstract.We prove a generalisation of an observation of N. Iwahori concerning the coefficients of the extended Dynkin diagram of a complex simple Lie algebra. We relate the combinatorics of these coefficients to the orders of finite groups that act discontinuously on the Riemann sphere and to the Plücker formulae.
GROUP EXTENSIONS AND THE PRIMITIVE IDEAL SPACES OF TOEPLITZ ALGEBRAS
Authors: ADJI SRIWULAN , RAEBURN IAIN , ROSJANUARDI RIZKY 
Published: May 2007

Abstract.Let Γ be a totally ordered abelian group andIan order ideal in Γ. We prove a theorem which relates the structure of the Toeplitz algebraT(Γ) to the structure of the Toeplitz algebrasT(I) andT(Γ/I). We then describe the primitive ideal space of the Toeplitz algebraT(Γ) when the set Σ(Γ) of order ideals in Γ is well-ordered, and use this together with our structure theorem to deduce information about the ideal structure ofT(Γ) when 0→I→ Γ→ Γ/I→ 0 is a non-trivial group extension.
SOME PROPERTIES OF CLASS A(k) OPERATORS AND THEIR HYPONORMAL TRANSFORMS
Authors: MARY J. STELLA IRENE , PANAYAPPAN S. 
Published: May 2007

Abstract.In this paper we shall first show that if T is a class A(k) operator then its operator transform $\hat{T}$ is hyponormal. Secondly we prove some spectral properties of T via $\hat{T}$. Finally we show that T has property (β).
BOUNDED LINEAR OPERATORS ON SPACES IN NORMED DUALITY
Authors: BARNES BRUCE A. 
Published: May 2007

Abstract.LetTbe a bounded linear operator on a Banach spaceW, assumeWandYare in normed duality, and assume thatThas adjointT†relative toY. In this paper, conditions are given that imply that for all λ≠0, λ−Tand λ −T†maintain important standard operator relationships. For example, under the conditions given, λ −Thas closed range if, and only if, λ −T†has closed range.These general results are shown to apply to certain classes of integral operators acting on spaces of continuous functions.
Lichenostigma svandae, a new lichenicolous fungus on Acarospora cervina
Authors: VONDRÁK Jan , ŠOUN Jaroslav 
Published: May 2007

Abstract:The new species Lichenostigma svandae is described. It is known exclusively from Acarospora cervina, where it forms black stromatic hyphal strands and black sack-shaped ascomata on the host thallus surface. It is similar to L. elongatum and L. rouxii, but differs in a few characters. A short overview of the known Lichenostigma species is provided.
A second species of Lithographa with submuriform ascospores
Authors: FRYDAY Alan M. , COPPINS Brian J. 
Published: May 2007

Abstract:The new combination Lithographa skottsbergii (Zahlbr.) Fryday & Coppins is made for Enterostigma skottsbergii Zahlbr., described from the Juan Fernandez Islands off the coast of Chile. The species is known only from Chile but its geographical range is here extended to include maritime regions of south-west Chile. The distribution pattern of the Lithographa species with submuriform ascospores is also discussed.
New discoveries in Asian pannariaceous lichens
Authors: JØRGENSEN Per M. 
Published: May 2007

Abstract:New collections from inner China have revealed further species in the genus Fuscopannaria: two new species, Fuscopannaria cyanogranulosa P. M. Jørg. and Fuscopannaria obtegens P. M. Jørg. are described and Fuscopannaria subgemmascens Upreti & Divakar is reported as new to Sichuan. A key to the sorediate species of the region is provided. The first fertile specimen of Kroswia gemmascens has been discovered, much further west than previously known, showing the genus to be related most closely to Fuscopannaria despite its gelatinous, homoiomerous thallus. Some collections from the Mulu region in Borneo have added to our knowledge of the difficult lowland taxa of Parmeliella, two of which proved to be new: Parmeliella plumosella P. M. Jørg. and Parmeliella polydactyla P. M. Jørg. & Coppins, both being quite unusual in containing “violet” Nostoc as cyanobiont. There is a surprising number of Asian collections with brightly coloured medullas: red-orange material has been named several times and is correctly referred to as Parmeliella endomilta Vain. The specimens with a yellow medulla are named Parmeliella endolutea P. M. Jørg., nom. nov. A key to the brightly coloured species of Parmeliella concentrated in SE Asia is given. A new corticolous Protopannaria has been discovered in Sichuan, and is described as P. corticola P. M. Jørg.
Radiative transfer modeling of the Hanle effect in convective atmospheres
Authors: Bueno Javier Trujillo 
Published: May 2007

AbstractThis paper summarizes the results of a recent investigation on the Hanle effect in atomic and molecular lines, which indicates that there is a vast amount of “hidden” magnetic energy and (unsigned) magnetic flux in the internetwork regions of the quiet solar photosphere. This hidden magnetic energy, localized in the (intergranular) downflowing plasma of the solar photosphere, is carried mainly by tangled fields at sub-resolution scales with strengths between the equipartition field values and ∼1 kG, and is more than sufficient to compensate the radiative energy losses of the solar outer atmosphere.
Modelling of solar granulation
Authors: Muthsam H. J. , Löw-Baselli B. , Obertscheider Chr. , Langer M. , Lenz P. , Kupka F. 
Published: May 2007

AbstractWe present the essential features of the ANTARES code. ANTARES has been developed to perform the simulation of astrophysical flows in one, two, or three dimensions. Using, in particular, the option of grid refinement, we present results for solar granulation achieved at very high spatial resolution.
Observing convection in stellar atmospheres
Authors: Landstreet John D. 
Published: May 2007

AbstractConvection occurs in the visible photospheric layers of most stars having Te less than about 10000 K, and in some hotter stars. The solar granulation pattern is a symptom of this, as is the non-zero microturbulent velocity often required in abundance analysis to make both weak and strong lines yield the same abundance.In very sharp-lined stars, the presence of a non-thermal velocity field in the visible stellar atmosphere leads to several other effects which may be detected in spectral line profiles. These include radial velocities that vary systematically with equivalent width, distortions of the line profile as compared to a profile computed with a Voigt profile and rotational broadening (“macroturbulence”), and asymmetries with respect to the line centre (“bisector curvature”).Detection and interpretation of these effects, with the goal of obtaining empirical information about a velocity field present in the visible layers, requires comparison with calculated synthetic spectra which incorporate model velocity fields. Thus, this review will summarize some of the observational clues concerning photospheric velocity fields, as well as modelling aimed at interpreting these data.
Stellar fluxes as probes of convection in stellar atmospheres
Authors: Smalley Barry 
Published: May 2007

AbstractConvection and turbulence in stellar atmospheres have a significant effect on the emergent flux from late-type stars. The theoretical advancements in convection modelling over recent years have proved challenging for the observers to obtain measurements with sufficient precision and accuracy to allow discrimination between the various predictions. An overview of the current observational techniques used to evaluate various convection theories is presented, including photometry, spectrophotometry, and spectroscopy. The results from these techniques are discussed, along with their successes and limitations. The prospects for improved observations of stellar fluxes are also given.
On the relation between rotation, convection and activity in intermediate-mass giants
Authors: Gondoin P. 
Published: May 2007

AbstractI found evidence that the X-ray surface flux of intermediate-mass G and K giants is correlated with their rotation period and Rossby number. Confidence in the degree of correlation is significantly higher when stellar gravity is taken into account. An empirical relation is found that accounts for the X-ray luminosity evolution of single intermediate-mass giants and giants in close or long-period binary systems, such as RS CVn-type systems, as they evolve off the main sequence towards the top of red giant branch.
Microturbulent velocities and abundances for A and F dwarfs in open clusters
Authors: Gebran M. , Monier R. 
Published: May 2007

AbstractThe current status of microturbulent velocity and abundance determinations for A and F dwarfs in open clusters is reviewed. A programme to observe several tens of A and F dwarfs in open clusters of various ages was initiated several years ago. We have performed high resolution high signal-to-noise spectroscopy of stars well distributed in mass along the Main Sequence. Microturbulent velocities and abundances of several chemical elements have been derived iteratively by fitting grids of synthetic spectra calculated in LTE to the observed spectra. Curve of growths were used in a few instances as well. The results obtained are reviewed for Coma Berenices, the Pleiades, Alpha Persei and the Ursa Major moving group.The microturbulent velocities exhibit a broad maximum in the range A5V to about F0V as indicated in Smalley (2004).
Observations of convection in the giant planets: results from space missions
Authors: Ingersoll A. P. 
Published: May 2007

AbstractThe giant planets are fluid objects; their solid cores occupy much less than half of their volumes. The largest planet, Jupiter, is over ten times the size of Earth. The giant planet atmospheres are powered in roughly equal parts by sunlight and by internal heat, which is left over from planetary formation. In most cases, the winds are measured by tracking clouds relative to the internal magnetic fields. Saturn is the exception, since the internal field is axisymmetric and therefore provides no evidence of rotation. In all four giant planets, the winds blow mainly in the east-west (zonal) direction, and the coloured cloud bands are aligned with the winds. The patterns are organized by rotation and not by the energy sources, since the sun at zenith moves from one pole to the other during the course of a year on Uranus, and yet the winds do not change. Although the power per unit area - the sum of absorbed sunlight and internal heat - is 20 times greater at Jupiter than at Neptune, the winds at Neptune are stronger. In fact Jupiter has the weakest winds of all the giant planets, although it is closest to the sun. Besides the zonal winds, the giant planets have long-lived vortices that have the same sign of vorticity as the latitude bands in which they sit. These large vortices exhibit a variety of behaviours, including oscillation in shape, position, and orientation, merging and splitting, and filament ejection. The anticyclones have a compact, oval shape; the cyclones are more elongated and diffuse. The cyclones contain lightning, which is a sign of moist convection. The cyclones therefore have a more disturbed appearance, since the convective storms are vigorous and chaotic. The convective storms are more frequent on Jupiter, but they are apparently more energetic on Saturn. The convective storms maintain a Reynolds stress that pumps momentum into the zonal jets in what is known as an inverse energy cascade. The depth to which the zonal winds extend is largely unknown. The winds could be confined to the outer 1 percent of the planets radii, or they could extend down into the fluid interiors, where the electrical conductivity and magnetic field become important.
Convection in brown dwarfs
Authors: Mohanty Subhanjoy , Baraffe Isabelle , Chabrier Gilles 
Published: May 2007

AbstractWe briefly review the crucial effect that convection plays in the evolution, interior and atmospheric physics of brown dwarfs. In particular, we discuss: (1) the role of convection in the interior structure and evolution of brown dwarfs (BDs); (2) the importance of convection in the atmospheres of ultra-cool objects, at both high and low gravities (i.e., in both young and old BDs); and (3) the role of convection/turbulence in the formation and settling of dust grains, and non-equilibrium chemistry, in BD atmospheres.
Convection during the formation of gaseous giants and stars
Authors: Wuchterl Günther 
Published: May 2007

AbstractConvection theories for star and planet formation studies have to be (1) simple, to allow a self-consistent solution with other relevant processes, (2) time-dependent, because convection often starts in collapse-flows, and (3) robust, i.e. physically well-behaved under a wide range of conditions ranging from the quiet protoplanetary nebula to supercritical protostellar accretion-shocks with Mach-numbers of a few hundred. I describe how the equations of radiation fluid-dynamics can be augmented by a one-equation convection model in order to construct a system of equations that contains the Sun, brown dwarfs and planets as well as their nearly isothermal parent-clouds. The system of equations is calibrated to the Sun and tested by the solar convection zone and the pulsations of RR-Lyrae stars. I discuss the following applications: (1) star formation as the collapse of Bonnor-Ebert spheres of masses ranging from the stellar domain to the brown dwarf region, (2) the approach to the main sequence, (3) companion mass determinations for direct imaging searches for exoplanets, with GQ Lupi as an example, and (4) the formation of Pegasi-planets, and the “large core” exoplanet, HD 149 026, in particular.
Chemical composition of dust clouds in turbulent brown dwarf atmospheres
Authors: Helling Christiane 
Published: May 2007

AbstractBrown dwarf atmospheres are largely convective. These convective gas flows collide and feed back a whole spectrum of turbulent fluctuations into the atmospheric fluid field. Resulting non-static density and temperature fields influence the local chemistry concerning gas phase and dust formation. Numerical simulations are used to show the large and inhomogeneous changes of the gas phase chemistry in a turbulent dust forming cloud region of a brown dwarf atmosphere. The relaxation time scale of the gas phase composition towards steady state is considerably longer than for the dust component.
A finite-difference convective model for Jupiter's equatorial jet
Authors: Chan Kwing L. 
Published: May 2007

AbstractWe present results of a numerical model for studying the dynamics of Jupiter's equatorial jet. The computed domain is a piece of spherical shell around the equator. The bulk of the region is convective, with a thin radiative layer at the top. The shell is spinning fast, with a Coriolis number = ΩL/V on the order of 50. A prominent super-rotating equatorial jet is generated, and secondary alternating jets appear in the higher latitudes. The roles of terms in the zonal momentum equation are analyzed. Since both the Reynolds number and the Taylor number are large, the viscous terms are small. The zonal momentum balance is primarily between the Coriolis and the Reynolds stress terms.
Stellar convection with nuclear burning
Authors: Arnett David , Meakin Casey , Young Patrick A. 
Published: May 2007

AbstractCareful choice of of method, problem, and zoning has allowed us to do three-dimensional (3D) simulations of thermally relaxed, nearly adiabatic convection (with nuclear burning). The simulations are run long enough so that a robust statistical state is found. We find that 2D simulations are biased relative to 3D simulations: 2D shows larger velocities and less mixing than their 3D counterparts. Detailed theoretical analysis of these numerical experiments allows us to begin to build a simple theoretical model of turbulent convection in stars, which may be used in 1D calculations of stellar evolution. Implications for stellar evolution, will be discussed. Oxygen shell burning simulations in 3D, and multishell burning of C, Ne, O, and Si in 2D will be presented, as will aspherical distortion in supernovae progenitors (Meakin and Arnett, 2006a). Contact will be made with convective driving of waves, convective zone growth by entrainment, the velocity scale and the geometric parameters in mixing length theory, and the solar Ne abundance problem. Explicit comparisons of compressible and anelastic methods at modest Mach numbers (M≈ 0.01 to 0.1), as well as solutions of the nonradial wave equations, are presented here. Additional detail is presented in the poster by Meakin.
On supersonic convection in stellar atmospheres
Authors: Xiong D. R. , Deng L. 
Published: May 2007

AbstractIt follows from the local mixing length theory that the convection in the atmospheres of yellow and red giants and super-giants become supersonic. In this work we studied the physical reality of such phenomenon and its possible consequences on the structure and evolution of stars involving such situations. The main conclusion is that the supersonic nature of convection as predicted by the local mixing length theory has been overestimated. If supersonic convection is not an artifact in all situations, it is the case at least for all yellow giants and super-giants. We believe that such an artifact is due to the imperfect of the mixing length theory. Owing to the fact that convective energy transport in the atmospheres of yellow giants and super-giants is quite negligible, these artifacts have very limited consequences on the structure and evolution of these stars. However, it is not the case for red giants and super-giants whose properties can be seriously affected by this overestimation. Our investigation shows that the theoretical red phases of stars under consideration are somewhat too blue as predicted with the usual mixing length theory. To this aim, full hydrodynamic simulation is needed in order to clear the doubts on the existence of supersonic convection in these red objects.
Abundances in extremely metal-poor stars: comparison of the trends of abundance ratios in giants and turnoff stars
Authors: Spite Monique , Bonifacio Piercarlo , Cayrel Roger , Spite François , Hill Vanessa , Andersen Johannes , Barbuy Beatriz , Beers Timothy , Depagne Eric , François Patrick , Molaro Paolo , Nordström Birgitta , Plez Bertrand , Primas Francesca 
Published: May 2007

AbstractWe show that in a sample of Extremely Metal-Poor (EMP) giants (<[Fe/H]>=−3.1) all the stars with a luminosity higher than logL/L⊙ ≈ 2.6 present the characteristics of a mixing of the surface with the H-burning layer: low abundance of carbon and high abundance of nitrogen. In these “mixed stars” the lithium abundance and the ratio 12C/13C are very low. Some of these stars are also Na or/and Al rich.