bluuebunny/crossref_metadata_2025_split huggingface dataset:
La reconnaissance du pilier culturel du développement durable: vers un nouveau mode de diffusion des valeurs culturelles au sein de l’ordre juridique mondial
Authors: Guèvremont Véronique 
Published: June 2019

SommairePar l’article 13 de la Convention de 2005 sur la protection et la promotion de la diversité des expressions culturelles, les parties se sont engagées à intégrer la culture dans leurs politiques de développement en vue de créer des conditions propices au développement durable. Si cette disposition marque une étape importante dans l’évolution du droit international de la culture et dans l’affinement de la notion de développement durable, ses effets juridiques sont toutefois susceptibles de se manifester à l’extérieur du champ d’application de la Convention. En effet, l’article 13 pourrait stimuler la prise en compte des valeurs culturelles dans l’interprétation des règles qui incorporent la notion de développement durable et faciliter une articulation harmonieuse — voire une synergie — entre des régimes juridiques distincts. Dans cette perspective, la référence à l’objectif de développement durable inscrite dans le préambule de l’Accord instituant l’Organisation mondiale du commerce semble par exemple offrir une avenue pour atténuer les tensions entre la poursuite des objectifs commerciaux et la prise en compte des preoccupations culturelles. De même, la mention du développement durable dans les normes climatiques peut favoriser une prise en compte des problématiques culturelles dans l’élaboration des stratégies d’adaptation. Comme le suggèrent ces exemples, le lien qui unit désormais la culture au développement durable pourrait donc exercer une influence tangible sur l’évolution de l’ordre juridique mondial.
Canada and the Two-China Formula at the United Nations
Authors: Dai Poeliu 
Published: June 2019

The canadian plan suggested to the 21st session of the General Assembly of the United Nations in 1966 for re-allocating China's seat in the world Organization was designed to bring about a breakthrough in resolving a question of great complexity that has beset that Organization for some 17 years. It has attracted world-wide attention and evoked various comments by both practitioners and students of international politics.Before analyzing the contents and denoting the legal and political implications of the plan, it is necessary to review briefly the background and the discussions of the question of China's representation at the 21st General Assembly.
Execution of Foreign Commercial Awards in Post-War Soviet Bilateral Treaty Practice
Authors: Ginsburgs George 
Published: June 2019

In 1945, H. J. Hilton, Jr., published an excellent article in the Department of State Bulletin entitled “Commercial Arbitration in the Treaties and Agreements of the U.S.S.R.” which assessed the Soviet record in this area up to the end of the Second World War. The purpose of the present study is to carry the inquiry forward to the present, concentrating, however, exclusively on the problem of execution of foreign commercial arbitral awards in Soviet bilateral treaty practice during this period.Before proceeding though, a quick review of the salient points of Mr. Hilton’s survey will furnish useful background information.First, in analyzing the corpus of Soviet treaties and agreements that feature statements concerning arbitration of commercial disputes, the author found that, while the relevant provisions ranged in detail from a single phrase to comprehensive conventions containing as many as 15 articles, the data did not reveal a pattern of historic evolution in the type of formulas regarding arbitration. In other words, although the Soviet regime passed through several phases of development between 1921, when such a reference initially appeared in a treaty signed by the R.S.F.S.R., and 1945, this did not entail technical changes reflecting specific policy shifts; the various approaches used recur throughout the span of observation without any determinable regularity and no correlation could be fixed between the choice of a particular solution and the prevailing conditions at home or abroad at a given juncture. The conclusion here, then, was that “the provisions referring to arbitration included in the treaties and agreements of the U.S.S.R. vary considerably in content; however, these variations cannot be established precisely by periods of time.”
Mediation, Conciliation and Adjudication in the Settlement of International Drainage Basin Disputes
Authors: Bourne C. B. 
Published: June 2019

When States Disagree about the way in which the waters of an international drainage basin should be utilized, they should try first to resolve their differences by consultation and negotiation. This is what they usually do and, for the most part, do successfully. Sometimes, however, their negotiations do not lead to agreement. They then face the question whether or not they should involve the aid of third-parties in resolving their problem. In the words of Article 33 of the Charter of the United Nations, must they “seek a solution by … mediation, conciliation, arbitration, judicial settlement, resort to regional agencies or arrangements, or other peaceful means of their own choice”?It is proposed to examine here the obligation of states to resort to mediation, conciliation and adjudication when they cannot otherwise settle a dispute about the development of an international drainage basin that they share.
The Convention on the Law Applicable to Traffic Accidents
Authors: Fischer Hugo 
Published: June 2019

On October 26, 1968, the delegates to the Eleventh Session of The Hague Conference on Private International Law decided to submit, for consideration by their respective governments, a draft Convention on the law applicable to traffic accidents. Article 14 of the Convention permits ratification by a country which, like Canada, has a non-unified legal system, if the Convention has been extended to at least one of its jurisdictions. The Convention aims at uniformity in a branch of the law where, until now, to quote an eminent jurist, “case-to-case decisions [did] not add up to a system of justice.”Under Canadian constitutional law the implementation of the Convention requires provincial legislation. At the invitation of the government of Canada a delegate of the Conference of Commissioners on Uniformity of Legislation in Canada participated at the session in The Hague as a member of the Canadian delegation.
Towards an International Convention on the Registration of Space Objects: The Gestation Process
Authors: Dalfen Charles 
Published: June 2019

Under most legal jurisdictions, motorized vehicles operating on land, in the air and on water are subject to registration. The effective management of traffic, the enforcement of standards of safety and the imputation of liability for damage all require that the parties responsible for the conduct of particular vehicles be identifiable. This identification function is normally provided for by means of a registration system.Typically, a registration system comprises two elements — characteristic markings on each vehicle operating within the jurisdiction, and a register which lists the vehicles by their markings along with the parties legally responsible for them. The system is underpinned by obligations on the responsible persons — usually the owners — to register and mark their vehicles, and on the state to maintain appropriate registers.As between jurisdictions there are frequently bilateral and sometimes multilateral agreements providing for reciprocal access to these registers under certain conditions.
Organisation des Etats américains, Comité juridique interaméricain : 5ième Séminaire de Droit international, Rio de Janeiro, 6 août - 1er septembre 1978
Authors: Hubert Jean-Paul 
Published: June 2019

Le comite juridique interaméricain (CJI) de l’Organisation des Etats américains a tenu son 5ième Séminaire de Droit international à Rio de Janeiro entre les 6 août et 1er septembre 1978. Le CJI a justement son siège à Rio.Le CJI admet deux catégories de participants à son Séminaire annuel: des boursiers, dont la candidature doit être soumise à l’OEA par les gouvernements des états-membres, et des auditeurs libres, admis par le Directeur du cours sur demande formulée auprès du Secrétariat général de l’OEA à Washington. Il n’y a pas de frais d’inscription. Pour la session de 1978, 27 bourses avaient été accordées, à des représentants de 19 pays de l’hémisphère. De plus, 17 auditeurs en provenance de 5 pays (dont le Canada) avaient reçu autorisation de participer.
Plasma Interactions in the Crab Nebula
Authors: Kahn F. D. 
Published: June 2019

Alfvén waves can be carried by the thermal plasma in the Crab Nebula. Each such wave perturbs the relativistic plasma present, in particular it strongly affects those particles which are in resonance with it. For a wave travelling parallel to the magnetic field the resonances are quite simple, but a wave travelling obliquely can give rise to multiple resonances, and can therefore couple together particles with quite different energies.It is shown that the interaction with the relativistic plasma leads to an amplification of the Alfvén waves when the mean velocity of relativistic plasma relative to the thermal plasma exceeds the Alfvén speed. The rise time for the instability is quite short, and the waves, once excited, are highly effective in redistributing the directions of motion of the relativistic particles. The relativistic plasma therefore cannot stream freely through the thermal plasma. On the other hand the disturbances will never quite die out in the Crab Nebula as long as the Crab pulsar keeps injecting fresh plasma, and thus keeps producing new inhomogeneities in the relativistic plasma density.
Physical mechanisms of mixing in stellar interiors
Authors: Schatzman Evry 
Published: June 2019

The different mechanisms by which mixing can take place in stellar interiors are considered : the classical Rayleigh-Benard instability with penetrative convection and over-shooting, semi-convection, gravitationnal and radiative settling, turbulent mixing. The latter mechanism is thoroughly described, from the driving force of turbulent mixing to its influence on stellar structure, stellar evolution and the analysis of the corresponding observationnal data.Turbulent mixing has to be considered each time the building up of a concentration gradient takes place, either by gravitationnal or radiative settling or by nuclear reactions. Turbulent mixing, as a first approximation, can be described by an isotropic diffusion coefficient. The process is then governed by a diffusion equation. The behaviour of the solution of the diffusion equation needs some explanation in order to be well understood.A number of examples concerning surface abundances of chemical elements are given (3He, 7Li, Be, 12C, 13C, 14N), as well as a discussion of the solar neutrinos problem.The building up of a µ-barrier, which stops the turbulence allows stellar evolution towards the giant branch and explains nitrogen abundance at the surface of giants of the first ascending branch.Turbulent mixing is also of some importance for the transfer of angular momentum and has to be taken into account for explaining the abundance of the elements in Wolf-Rayet stars.
On the Equation of Precession and Nutation of the Dynamically Unbalanced Earth
Authors: Erzhanov Zh. S. , Kolybaev A. A. , Egorov Al. K. 
Published: June 2019

In contrast to the deduction of the equations of precession and nutation adopted as a standard by the IAU, the authors develop a rigorous theory of the rotation of the Earth taking into account the inequality of the equatorial moments of inertia of the Earth and retaining small terms usually neglected to simplify an approximate solution.The equation is expressed in terms of the so-called Beletsky-Chernousko's variables used in astrodynamics.
Particle Acceleration and Radio Emission of the Supernovae Remnants at Different Stages of their Evolution
Authors: Fedorenko V. N. 
Published: June 2019

In this Paper, I consider physical processes, governing relativistic electrons in SNRs.
a)SNRs at the age t > 102 yr. I argue that the shock wave acceleration faces some difficulties. Then I show that the temporal evolution of the SNRs radio emission can be accounted for without involving the acceleration.b)SNRs at the age t < 102 yr. I associate the lack of radio emission at this stage (Brown and Marscher, 1978) with the weakness of the magnetic field.c)I infer that the most efficient particle acceleration and radio emission of the SNRs should occur at the stage t ~ 102 yr.
Spectrophotometry of the Optical Emission from RCW103
Authors: Ruiz Maria Teresa 
Published: June 2019

Spectra for five different positions in RCW103 were obtained with the 1.5m and 4m telescopes of CTIO equiped with a SIT Vidicon detector.From the observed Hα/Hβ ratio we found a variation of about 1.5 magnitudes in reddening for different filaments. The minimum value of Av found was 4.4 magnitudes implying a distance of 6.5 kpc.Temperatures of about 105 K and densities of 70 cm−3 were found. Nitrogen is overabundant at least by a factor 3.
CTB80: Cosmic Collision?
Authors: Salter C. J. , Mantovani F. , Tomasi P. 
Published: June 2019

High resolution maps of the Galactic radio source CTB80 at three different frequencies are presented. A new interpretation in terms of a cosmic collision between two SNRs of different age is suggested.CTB80 is one of the most mystifying Galactic Objects yet discovered and has recently attracted considerable attention from X-ray, optical and radio astronomers (see for example: Becker et al. (1981), Angerhofer et al. (1980, 1981), Velusamy et al. (1976), van den Bergh (1980).The present observations of the radio continuum emission of the extended feature at 408 MHz, 1720 MHz and 4750 MHz and the linearly polarized emission at 1720 MHz and 4750 MHz (Figs 1,2,3) throw new light on the morphological, spectral and polarization properties of the whole source.
Supernova Remnants with Central Pulsars
Authors: Seward Frederick D. 
Published: June 2019

The recent discovery of a central pulsing X-ray source makes MSH 15–52 the third SNR to contain a radio pulsar surrounded by diffuse X-ray emission. The pulsar periods are all increasing with time and the consequent loss of rotational kinetic energy is enough, in each remnant, to power a synchrotron nebula with the observed luminosity and volume.After a review of the properties of the Crab Nebula it will be shown that both Vela X and MSH 15–52 have the same relationship between central pulsar and diffuse emission. Using empirical rules derived from these SNR, it is demonstrated that other plerionic remnants have similar characteristics. Two accretion-powered central sources can be distinguished from radio pulsars in SNR by the relatively high X-ray luminosity of the central source compared to that of possible synchrotron diffuse emission.
Luminous Supernova Remnant Candidates in M82 and The Physical Properties of The Variable Radio Source 41.9+58
Authors: Kronberg P. P. , Biermann P. 
Published: June 2019

Large numbers (∼30) of supernova remnant candidates have been revealed in new VLA maps of the inner 600 pc of M82 with subarcsecond resolution. The flux density decrease of the bright source 41.9+58 in the M82 nuclear region is found to be occurring with an approximately constant spectral index of −0.9 at ν≳3 GHz, and the low frequency turnover has moved from ∼700 MHz in 1974–1975 to <400 MHz in 1979–81.A model of 41.9+58 is proposed in which it is, at least initially confined by its own hot (∼108K) pre-SN ejecta, and its relativistic particles are accelerated by a pulsar at its centre.
Properties of Galaxies in Low Density Regions
Authors: Brosch N. 
Published: June 2019

Isolated galaxies seem to have more nuclear activity and less disk activity than nonisolated objects. This is interpreted as an expression of the mass-profile in their halos.The discovery of voids in the three-dimensional distribution of galaxies has rapidly been followed by claims that in at least one such void some objects, like Markarian and emission-line galaxies, are present. Why are only active galaxies found in these voids? Should we also expect the opposite to be true, namely that active galaxies ought to be found more often in voids, or in regions of the Universe with lower-than-average density? There are indications that this seems to be the case, as Gisler (1978) found that emission-line galaxies, Markarians and possibly Seyferts avoid environments of dense clusters. Differences between “field” and “cluster” populations are probably due more to the enhanced local density of galaxies than to the nature of the overall environment.
Chemical Composition in the Envelopes of Different WR Subtypes
Authors: Nugis T. 
Published: June 2019

Valuable model-independent information about the chemical composition of WR stars can be obtained by using lines of different ions arising at transitions between highly excited energy levels. We determine the abundances of He, H, C, N, O using theoretical line intensities obtained by solving statistical equilibrium equations for level populations for different subtype WR envelope conditions.The chemical composition of WR stars strongly differs from the mean cosmic composition. In the case of WN stars nuclear processed CNO products of H-burning are revealed in the envelopes and He-burning products in the WC envelopes.The abundance of oxygen in WC stars differs from the predictions of recent evolutionary calculations which account for the new 12C(α,γ) 16O reaction rate.
Radio Observations of Massive OB Stars
Authors: Howarth Ian D. , Brown Alexander 
Published: June 2019

The mass-loss rates of O stars and B supergiants are of interest because of their influence on the evolution of these massive stars (among other matters). In principle, the ‘safest’ (i.e. most model-independent) method of determining M is to measure the free-free emission from stellar winds at radio wavelengths. This method is complicated, however, by the existence of poorly understood non-thermal emission in some stars, and by the possibility of hydrogen recombination in the winds of B supergiants.We are in the process of carrying out a VLA survey of OB stars, initially at 3.5cm, to a flux limit of ~0.1mJy. Because all our targets should have thermal emission at detectable levels (based on mass-loss rates from Howarth & Prinja 1989 and terminal velocities from Prinja, Barlow & Howarth 1990), the survey is yielding an unbiassed estimate of the frequency of non-thermal emission. The improved sensitivity of our survey over earlier work defines the log M – log L relationship much more precisely than was previously possible, over a large range in luminosities; and allows us to make definitive statements on recombination in B supergiant winds. Our sample includes the first radio detections of an OC star, of a massive X-ray binary, and of thermal emission from a main-sequence star.
Photometric Determination of Mass Loss Rates and Orbital Inclinations for WR Binaries
Authors: Lamontagne R. , Robert C. , Grandchamps A. , Lapierre N. , Moffat A. , Drissen L. , Shara M.M. 
Published: June 2019

Most Wolf-Rayet binaries show phase-dependent light variations with a broad dip occurring at phase zero, when the WR star passes closest to the observer. When the orbital period is long, or the inclination is low, this dip is buried in the noise. When eclipses of the stars occur, another dip is seen when the companion passes closest to the observer; in this case, both dips are relatively deep and sharp (e.g. V444 Cygni, HD5980).In the cases when only one dip at phase zero is seen, a simple model is derived. This involves electron scattering of companion starlight as the orbit makes it systematically traverse different amounts of the WR wind, assumed to be spherically symmetric and to follow a monotonic velocity-radius law. The shape and amplitude of the dip yield estimates of M and i (hence M when combined with M sin3i from spectroscopic orbits).
The Mass of WR Progenitors
Authors: Vanbeveren D. 
Published: June 2019

A search through literature reveals four methods in order to derive the mass of WR progenitors, i.e.a. WR stars must be descendant from the most massive stars which share their galactic distribution,b. the computation of detailed evolutionary models of massive close binaries up to the WR phase, able to explain the observational constraints of these WR binaries,c. comparing the very narrow mass-luminosity relation of massive core helium burning stars predicted by evolution and estimated bolometric luminosities of WR members of stellar aggregates,d. the minimum mass of the progenitor of a WR member of a cluster equals the mass of the most luminous star (or the star with the earliest spectral type) in the cluster.
Summary of Symposium
Authors: Conti Peter S. 
Published: June 2019

“It is a significant fact that the emission and absorption lines of Wolf-Rayet spectra cannot be regarded as being formed in one body of gas at one representative temperature and pressure” (Underhill 1968)“I think it fair to say that the demonstration of… diversity has brought the Wolf-Rayet stars from being a curiosity to being an important part of the ‘main stream’ evolution of all massive stars” (Smith 1982)
MOCAM: A 4k × 4k CCD Mosaic for the Canada-France-Hawaii Telescope Prime Focus
Authors: Cuillandre J. C. , Melliers Y. , Murowinski R. , Crampton D. , Luppino G. , Arsenault R. 
Published: June 2019

MOCAM is a wide field CCD camera, currently nearing completion, which will be offered to the Canada-France-Hawaii Telescope (CFHT) user community in 1995. The project is a collaboration between the CFHT, the Dominion Astronomical Observatory (DAO, Canada), the Institut des Sciences de l'Univers (INSU, France), Laboratoire d'Astrophysique de Toulouse (LAT, France) and the University of Hawaii (UH). In the interests of producing a reliable and effective camera in the shortest time, it was decided to use existing technologies rather than innovative ones. Two-edge buttable 2048 × 2048 15 μm pixel CCDs were obtained from the LORAL aerospace foundry, based on a mask designed by J. Geary at Smithsonian Astrophysical Observatory (SAO). They are mounted in a dewar designed by G. Luppino (UH); the focal plane mounting keeps the mosaic flat to within two pixels and the CCDs are aligned to within two pixels. A mechanical interface designed and fabricated by the DAO holds a 150 mm shutter and a filter wheel which has a positioning repeatability better than five μm.The four CCDs are operated in parallel by a San Diego GenIII controller adapted by LAT. The mosaic is read out in seven minutes and a single 33 Mb FITS file is generated to enable convenient on-line preprocessing. The user will control the system through a single CFHT Pegasus environment session. The camera field is 14′ × 14′ with a 0.″2 pixel sampling and the readout noise is less than seven electrons. The scientific goals of the initiators of the project are studies of distant clusters, deep galaxy counts and quasars surveys.