bluuebunny/crossref_metadata_2025_split huggingface dataset:
Canadian Mining Internationally and the UN Guiding Principles for Business and Human Rights
Authors: Seck Sara L. 
Published: June 2019

SummaryBetween 2005 and 2011, there was much debate, both within Canada and at the United Nations (UN), over what role home states should play in the regulation and adjudication of human rights harms associated with transnational corporate conduct. In Canada, this debate focused upon concerns related to global mining that led to a series of government, opposition and multi-stakeholder reports and proposals. These culminated in 2010 with the appointment of an Extractive Sector Corporate Social Responsibility Counsellor and the defeat of Bill C-300, An Act Respecting Corporate Accountability for the Activities of Mining, Oil or Gas in Developing Countries. Meanwhile, at the UN Human Rights Commission/Council, John G. Ruggie was appointed Special Representative to the UN Secretary-General on Business and Human Rights (SRSG). Ruggie’s work led to the 2008Protect, Respect and Remedy: A Framework for Business and Human Rightsand the 2011Guiding Principles for Business and Human Rights(the latter designed to “operationalize” the former). While both documents highlight state duties to protect against human rights violations by businesses and the need for access to remedies by victims, the role of home states in this regard was contested. This article compares the developments in Canada between 2005 and 2011 with the work of the SRSG in relation to the home state duty to protect human rights in the transnational corporate context. It also offers reflections on the implications of the inevitability of industry and industry lawyer participation for the development of home state legal obligations.
Les mesures conservatoires indiquées par la Cour internationale de Justice dans le cadre de conflits territoriaux et frontaliers: Développements récents
Authors: Ghantous Marie 
Published: June 2019

SommaireLe recours aux mesures conservatoires devant la Cour international de Justice (CIJ) a sensiblement augmenté mais une évolution significative a été notée dernièrement. Ces développements mettent en exergue la montée en puissance des juridictions internationals soit du fait de l’immobilisme du Conseil de sécurité, soit en raison d’un effet boule de neige de la multiplication en un temps record des juridictions pénales internationales après la chute du mur de Berlin et de l’effondrement de l’URSS. Destinées à l’origine à preserver les droits des parties et à conserver les preuves lors d’une procédure principale devant la CIJ, les mesures conservatoires sont devenues un véritable instrument au service de la paix et la sécurité internationales. Elles ont, en effet, la priorité sur toutes autres questions portées devant la CIJ et permettent ainsi de réagir rapidement dans les situations d’urgence. Les deux ordonnances en indication de mesures conservatoires prononcées en 2011 consolident d’une part la jurisprudence de la CIJ. Mais elles contribuent d’autre part à l’extension du champ d’application des mesures édictées, mettant ainsi la CIJ sur un pied d’égalité avec le Conseil de sécurité dans son rôle d’organe des Nations Unies (ONU) participant à la réalisation des objectifs de la Charte de l’ONU. Cette concurrence se manifeste au niveau du litige dont le Conseil ou la CIJ peuvent être saisis, mais elle peut se manifester également dans la nature des mesures que la CIJ va édicter et qui ont été dernièrement de nature militaire notamment à travers la création d’une zone démilitarisée, chose qui était traditionnellement du resort du Conseil de sécurité. Ce qui pose la question de la force obligatoire de ces ordonnances et de leur exécution mais aussi un risqué de détournement de procédure qui pourrait paradoxalement refroidir le désir des États de recourir à la Cour mondiale.
La conception soviétique du droit international
Authors: Patry André 
Published: June 2019

Dans un Discours prononcé le 25 janvier 1962 devant la Chambre de commerce américaine en France, l’ex-premier ministre Michel Debré mentionna qu’un délégué aux Nations Unies avait, quelques jours auparavant, tenu les propos suivants: “Le droit international est l’oeuvre des Européens. Les Européens sont colonialistes. Par conséquent, nous n’avons pas à connaître le droit international”.Il n’y a pas de doute que le droit international classique, celui qui fut à une époque récente le droit de la planète tout entière, est, pour l’essentiel, celui des nations chrétiennes. D’abord exclusivement européen, il était destiné à régir les rapports entre Etats dits “civilisés”. Au XVIIIe siècle, ce droit fut étendu à la Russie. Au siècle suivant, il fut jugé applicable à la Turquie (1856), puis au Japon (1895). Aux yeux des Européens, il y eut donc, à une certaine époque, à côté du jus gentium, un jus inter gentes, sorte de droit aristocratique liant entre eux les sujets chrétiens de l’ordre juridique international. Mais, dès les débuts du XXe siècle, ce droit européen était devenu universel, comme en témoignent les deux conférences de LaHaye.
Nuclear Forces in High Density Matter
Authors: McNaughton M. R. 
Published: June 2019

The conditions for superfluidity or ferromagnetism in neutron stars are presented and discussed (but not derived). It is suggested that present estimates relating to these are in error and that the predictions made contradict at least one of three sets of nuclear physics data cited in the text. This is due to neglecting the action of the exclusion principle.A comparatively simple method for calculating the strength of nuclear forces in the presence of many-body effects is outlined. Some preliminary results are presented together with projected future developments.
Binary evolution and observational constraints
Authors: de Loore C. 
Published: June 2019

The evolution of close binaries is discussed in connection with problems concerning mass and angular momentum losses. Theoretical and observational evidence for outflow of matter, leaving the system during evolution is given: statistics on total masses and mass ratios, effects of the accretion of the mass gaining component, the presence of streams, disks, rings, circumstellar envelopes, period changes, abundance changes in the atmosphere.The effects of outflowing matter on the evolution is outlined, and estimates of the fraction of matter expelled by the loser, and leaving the system, are given. The various time scales involved with evolution and observation are compared. Examples of non conservative evolution are discussed.Problems related to contact phases, on mass and energy losses, in connection with entropy changes are briefly analysed. For advanced stages the disruption probabilities for supernova explosions are examined. A global picture is given for the evolution of massive close binaries, from ZAMS, through WR phases, X-ray phases, leading to runaway pulsars or to a binary pulsar and later to a millisecond pulsar.
Catalogue of Clusters that are Members of Superclusters
Authors: Kalinkov M. , Stavrev K. , Kuneva I. 
Published: June 2019

An attempt is made to establish the membership of Abell clusters in superclusters of galaxies. The relation
is used to calibrate the distances to the clusters of galaxies with two redshift estimates. One is m10, the magnitude of the ten-ranked galaxy, and the other is the “mean population,” P, defined by:
where p = 40, 65, 105 … galaxies for richness groups 0, 1, 2 …, and r is the apparent radius in degrees given by:
The first iteration for redshift, z1, is obtained from m10 alone:
The standard deviation for Eq. (1) is 0.105, the number of clusters with known velocities is 342 and the correlation coefficient between observed and fitted values is 0.921. With zi from Eq. (1), we define Cartesian galactic coordinates Xi = Rih−1 cosBi cosLi, Yi = Rih−1 cosBi sinLi, Zi = Rih−1 sinBi for each Abell cluster, i = 1, …, 2712, where Ri is the distance to the cluster (Mpc), and Ho = 100 h km s−1 Mpc−1.
The Sun's Rotation Rate as Inferred from Magnetic Field Data
Authors: Stenflo J.O. 
Published: June 2019

The pattern of solar magnetic fields has been used as a tracer to determine how the sun's rotation rate varies with latitude and time. Two distinctly different rotation laws emerge from such an analysis, one agreeing with the surface Doppler rotation rate, the other corresponding to much more rigid rotation with a small polar spin-up. Detailed analysis shows that this second law cannot be explained in terms of flux redistribution on the solar surface, but that it represents the rotation properties of the sources of magnetic flux, which are likely to be located at the bottom of the convection zone.The rotational phase velocity of the source pattern is found to be constant with time, which suggests that the depth at which the magnetic flux is stored and amplified inside the sun does not vary with the solar cycle, and that the phase velocity also represents the plasma velocity.
Wolf-Rayet Populations in Dwarf Galaxies
Authors: Smith Lindsey F. 
Published: June 2019

The Wolf-Rayet (WR) feature at 4650 A is observed in about 10% of the dwarf galaxies with high surface brightness knots. The intensity of the feature implies the presence of tens to thousands of WR stars. Hbeta fluxes imply correspondingly large numbers of O stars. The easily observed intensity ratio WRbump/Hbeta is a measure of the WR/O star numbers.The metallicity of dwarf galaxies ranges from Z = Zo/30 to Zo/2, or O/H” = log(O/H)+12 = 7.4 to 8.6. WRbump/Hbeta correlates with O/H′ and O/H″ > 7.9 appears to be a necessary condition for the presence of the WR feature. Giant HII regions in ordinary galaxies extend to higher than solar metallicities and, in extreme cases, WR/O ≈ 1 are implied.The subtypes present in giant HII regions in nearby galaxies appear to be exclusively late type WN and, occasionally, early type WC. Spectra of most BCD galaxies are compatible with a similar population. However, some high metallicity giant HII regions in large galaxies appear to have stronger NIII4640 relative to HeII4686 than occurs in WN subtypes in the Galaxy and the Magellanic Clouds.The data needed for more detailed analysis of dwarf galaxy observations is collected.
Distribution de l'énergie dans le spectre ultraviolet de quelques étoiles
Authors: Chalonge D. , Divan L. , Hua C. T. 
Published: June 2019

AbstractPreliminary results of recent direct comparisons between some early type O, B standards (and also α Lyr) and a terrestrial source previously compared to a black body are given for the ultraviolet range. It appears that the previously-used gradients ɸuv must be corrected on the average by +0.10.
Choosing Filters to Make CCD Photometry Transformable to Other Detectors
Authors: Young Andrew T. 
Published: June 2019

Transforming CCD data is difficult. Until recently, the general transformation problem was so poorly understood that there were no established design criteria. Now, the Hilbert-space approach to photometry tells us to match the standard passbands in the least-squares sense.Unfortunately, the spectral responsivities of CCDs vary much more than do conventional detectors, and must be known to design filters. Each individual chip generally requires its own set of filters, if results are to be better than second-rate. Even so, spatial variations in spectral response limit the accuracy that can be reached, unless color terms are determined for individual pixels. Such CCD calibration problems involve the generally neglected optical properties of CCDs and the systems in which they are used.Large observatories will have to establish calibration laboratories, and to abandon the common practice of moving “standard” filter sets from one instrument to another. Smaller institutions will need to purchase the services of such calibration laboratories if they are to produce accurate CCD photometry. These are major changes in the way astronomers are accustomed to working; but such changes are necessary to stem the backlash developing against CCD photometry.
Spectral Anomalies in the Hyades and Pleiades and in Field Stars with Active Chromospheres
Authors: Rose James A. 
Published: June 2019

Widened photographic image-tube spectra at 50 Å mm−1 dispersion have been obtained for a large number of late-type field dwarfs and giants with well-determined atmospheric parameters and for 35 Hyades dwarfs and 31 Pleiades dwarfs. The spectra have a resolution of 2.5 Å and cover the wavelength range λλ3400–4500 Å. A new quantitative three-dimensional spectral classification system is derived for late-type stars and is calibrated using the sample of field dwarfs and giants with known atmospheric parameters. Diagnostic indices are defined by comparing the counts in the bottoms of two neighboring absorption lines or by comparing the counts in two neighboring pseudocontinuum peaks.It is found that the Hyades and Pleiades dwarfs and field dwarfs with strong Ca II H and K emission reversals exhibit well-defined anomalies in their diagnostic indices when compared with normal field dwarfs. These results are summarized in Rose (1984). In LaBonte and Rose (1984), it is shown, from spectra of solar magnetic plages, that all spectral and photometric peculiarities of the Hyades discovered to date, including the original “Hyades anomaly” (Crawford 1969; Strömgren et al. 1982), are manifestations of plage activity.
About the Photometric Calibration of IUE High Resolution Spectra: Quantification of the Order Overlap for the SWP Camera
Authors: Bianchi Luciana , Bohlin Ralph 
Published: June 2019

In order to quantify the errors in the IUE line profiles caused by the order overlap, we have compared line depths in IUE and Copernicus spectra. The excess line depth in IUE spectra suggests that the amount of order overlap is about 32% at 1150Å and decreases to zero at about 1400Å, for spectra extracted with the recent version of IUESISPS (the IUE standard extraction software). The transfer of a spectral feature from one order to the next is below the 5% level.Based on these results, a correction technique is described.
Some Differences Between Geometrical and Dynamical Figures of the Moon
Authors: Gavrilov I. V. 
Published: June 2019

The geometrical shape of the Moon is determined from measurements of absolute heights of the lunar surface, while its dynamical shape is described by means of the Moon's gravity field parameters. All these data are derived from observations of the lunar artificial satellites (‘Luna-10’, ‘Orbiters 1-4’) and astronomical measurements.In the paper differences of the lunar geometrical and dynamical figures are analysed. It is shown, that the homogeneous model of the Moon is not capable of explaining these differences. It is found, that the lunar centre of gravity situated about 0.9 km to the north, and 1.1 km nearer to the Earth, than the centre of its geometrical figure.
Formation of Lunar Glassy Spherules: A Dynamical Model
Authors: Carusi A. , Coradini A. , Fulchignoni M. , Magni G. 
Published: June 2019

Glassy spherules ranging from 200μto 62μin size have been separated from lunar dust samples No. 12001.73, 12057.60, 12070.37. Most of them are regular in size (spherical, ellipsoidic, dumbbell, teardrop, etc.); some are irregularly shaped.A tentative dynamical model of the evolution of a rotating melted spherical drop of homogeneous glassy material has been built in order to explain the observed forms. We suppose such fluid to be originated from the impact of meteoroids on the lunar surface. The energy balance between the projectile (meteoroid) and the target (lunar surface) has been calculated supposing that the impact gives rise to strong shock waves in both bodies.Equations of the model have been solved numerically and a good agreement between these results and the experimental data regarding small spherules has been obtained.
The Valence States of 3d: Transition Elements in Apollo 11 and 12 Rocks
Authors: Cohen Alvin J. 
Published: June 2019

The absorption spectra of Apollo 11 fine-grained rocks, 10017 and 10022 are due entirely to pyroxene minerals. Spectral bands due to Fe3+, Fe2+, Cr3+ and Ti4+ and Ti3+ are detected. Single crystals of olivine in rocks 12021 and 12018 show bands due to Fe3+, Fe2+, Cr3+, Ti3+, Mn3+, and Mn2+. Pyroxenes in the same rocks exhibit band maxima of the same cationic species as in the olivines. Spectral shifts are noted due to anisotrophy of the crystal structures.Heating sections 10017, 10022, and 12018 from the rock interiors at 200–225°C for 2 h caused large decreases in the spectral intensity of Fe3+, Cr3+ and Ti3+, indicating the following reaction:Fe3+ + Cr3+ + Ti3+ → Fe2+ + Cr2+ + Ti4+This suggests that Fe3+, Cr3+ and (a portion of) Ti3+ are not in equilibrium. It is most probable that they were produced subsequent to the formation of the rocks by a combination of secondary ionization processes following cosmic ray bombardment and by trace radioactivity present in the rocks.An orange glass, 150 μ in diam and 50 μ thick contained in brecciated rock, 10048.44, exhibited 15 identifiable absorption bands related to Fe2+, Cr3+, Ti3+, Mn3+ or Mn2+ ions.Plagioclase in 12021.65 has perfect transmission over the region studied. The limit of Fe3+ is in the order of < 1 ppm and Fe2+, 1000 ppm or less in this plagioclase single crystal of dimensions 0.6 mm × 0.2 mm × 30 μ.
Infrared Emission from Dust in Supernovae and Supernova Remnants
Authors: Dwek Eli 
Published: June 2019

The need to replenish the reservoir of interstellar dust grains that are continuously being destroyed in the interstellar medium, and the presence of isotopic anomalies in meteorites, suggest that supernovae may be important sources of interstellar dust. Infrared observations of supernovae or their unmixed ejecta may provide the first direct evidence for newly-formed grains in this environment. The recently discovered supernova, SN 1987A, currently offers the best prospects for observing the actual process of dust formation in a supernova.In contrast, supernova remnants constitute the most important grain destruction mechanism in the galaxy. Interstellar dust swept up by the expanding blast wave is predominantly heated and destroyed by collisions with a shocked x-ray emitting plasma. Infrared observations of remnants can therefore provide valuable information on the interaction between dust particles and a hot gas. This interaction can best be studied in supernova remnants detected with the Infrared Astronomical Satellite (IRAS). This paper reviews what we have learned so far on the subjects of grain formation and destruction by studying the infrared emission from supernovae and supernova remnants.
Anisotropy of the Microwave Background and Biased Galaxy Formation
Authors: Kaiser Nick 
Published: June 2019

Fluctuations in the microwave background will have been imprinted atz≃ 1000, when the photons and the plasma decoupled. On angular scales greater than a few degrees these fluctuations provide a clear view of any primordial density perturbations, and therefore a clean test of theories which invoke such fluctuations from which to form the structure we see in the universe. On smaller angular scales the predictions are less certain: reionization of the gas may modify the spectrum of the primordial fluctuations, and secondary fluctuations may be generated.Here I shall review some recent theoretical developments. A brief survey is made of the currently popular theories for the primordial perturbations, with emphasis on the predictions for large scale anisotropy. One major uncetainty in the predictions arises from the normalisation of the fluctuations to e.g. galaxy clustering, and much attention is given to the question of ‘biased’ galaxy formation. The effect of reionization on the primordial fluctuations is discussed, as is the anisotropy generated from scattering off hot gas in clusters, groups and galaxies.
The Tycho Survey Of Stars Brighter than Eleventh
Authors: Egret Daniel , Høg Erik 
Published: June 2019

The real-time attitude of the HIPPARCOS satellite (see Turon, this symposium) is monitored by a star mapper viewing a 40 arcmin. Wide band of the sky, ahead of the main field of view, through a system of four vertical and four inclined slits (fig. 1). The resulting on-board precision will be 1 arcsec. rms and on-ground attitude reconstitution will later improve this value to 0.1 arcsec. rms.The TYCHO project (approved by ESA in 1981) consisted in introducing dichroic beam splitters and a pair of redundant photomultipliers (with a bandpass close to Johnson B and V) into the science payload. This configuration will give a complete survey of the sky down to 11th magnitude in B, during the two and a half years of the mission. The data reduction is prepared by a scientific consortium (TDAC) which will be described in more details in section 4. The work related to the TYCHO Input Catalogue is described in section 2. An overview of the data reduction process is given as section 3, and aspects of the TYCHO outputs are discussed in section 5.
The Twin-Nucleus Merging Galaxy MKN 266
Authors: Hutchings J.B. , Neff S.G. , van Gorkom J.H. 
Published: June 2019

We present results of observations of the double-nucleus galaxy Markarian 266 (NGC 5256) from 3 principal sources. These are
1:CCD imaging with the Canada-France-Hawaii telescope in broad and narrow bands. These indicate that the galaxy has extended, complex, faint outer plumes which indicate that a recent merger has occurred. The narrow-band images reveal remarkable knotty structure of the [O III] emitting gas, extending over the whole central part of the galaxy. This is not seen in Hα (see figure 1).2:21cm imaging with the VLA, covering velocity space near that of the optical nuclei. The continuum image reveals resolved triple structure, with the two outer peaks coincident with the optical nuclei. The 21cm velocity profiles indicate the presence of considerable H I absorption near the optical emission line velocities.3:Spatially resolved optical spectroscopy with the DAO 1.8m telescope. These data reveal the details of the [O III] velocity field and some of the physical parameters of the gas. The complexity and extended nature of the gas explains some conflicting redshift measurements in the literature. Together with the imaging data, we derive estimates of nuclear reddening and luminosity.
Numerical planetary and lunar ephemerides: present status, precision and accuracies
Authors: Standish E. Myles 
Published: June 2019

The Ephemeris Development Program has been in existence for nearly 20 years at JPL, providing high precision present-day knowledge of the positions of the moon and major planets. The resultant ephemerides are used extensively in the navigation of spacecraft and in the reduction of astrometric observations. They also provide a key element in the testing of various theories of gravitation and a means for the determination of various relevant astronomical constants. The ephemerides and the process of creating them are both shown to be viable tools for the measurement of various gravitational effects which govern the motions of the objects in the solar system.This paper gives an outline of the least-squares adjustment of the ephemerides to the observations, the present physical (dynamical) model, the present observations to which the ephemerides are fit, the expected accuracies of various ephemeris elements, recent and future observations and features of the solar system which are poorly determined (and thereby place limits upon the accuracies). Recent comparisons with similar work at the Center for Astrophysics (formerly at MIT) are serving as valuable independent checks on formulations and procedures used at each institution; they also lend insight toward what are the realistic accuracies being attained. The export procedure, by which an outside user may obtain and use the JPL ephemerides, is described.