bluuebunny/crossref_metadata_2025_split huggingface dataset:
Le traitement jurisprudentiel du trafic de migrants en droit comparé: Un désaveu des dispositions législatives
canadiennes
Authors: Jannard Louis-Philippe 
Published: June 2019

SommaireLe durcissement des politiques migratoires a diminué les possibilités légales de migration, créant ainsi un environnement propice au trafic de migrants. En 2002, le Canada a drastiquement augmenté les pénalités associées à ce phénomène. Ces dispositions sont inadéquates: elles cherchent moins à réprimer une activité criminelle présumée dangereuse qu’à dissuader l’immigration irrégulière. D’une part, les dispositions législatives s’inscrivent en faux avec le traitement jurisprudentiel du trafic de migrants au Canada, et ne correspondent ni aux lois ni à la jurisprudence étrangères: on surestime la gravité du crime. D’autre part, elles ne se conforment pas au droit international. En excluant la recherche d’un avantage financier de la 'définition canadienne de l’infraction, on privilégie la lutte à toute forme d’aide à la migration irrégulière, et non seulement au trafic de migrants.
Malaya/ Singapore/ Malaysia: Comments on State Competence, Succession and Continuity
Authors: Green L. C. 
Published: June 2019

The Constitutional and international history of Singapore and Malaya have been chequered and hectic since the days of the Japanese occupation. Perhaps the most startling were the years from 1963 to 1965, the period during which Singapore ceased being a Crown Colony to form with Malaya the Federation of Malaysia and, when that experiment failed, to become an independent sovereign state within the Commonwealth.It is the purpose of this paper to examine this history in order to extract those issues which are of interest from the point of view of state succession and the continuity of law, while at the same time paying attention to some of the problems of competence that occur in a federal state, especially one in which the component parts have only recently enjoyed independence.
Distinguishing Friend from Foe: Law and Policy in the Age of Battlefield Biometrics
Authors: Mitchell Alison 
Published: June 2019

SummaryIn the space of just over ten years, the collection and use of biometric data in the context of international military operations has gone from being virtually unheard of to being an everyday occurrence. The Canadian and US armed forces operating in Afghanistan, for example, have together collected the digital fingerprints, eye scans, and digital photographs of more than 2.5 million Afghans. The introduction of biometrics technology to warfare has undoubtedly increased the security of the armed forces that use it and made it easier for them to kill or capture their enemies. Its effectiveness, reliability, and convenience have all been praised. Due in part to its novelty, however, law and policy relating to the use of biometrics in conflict situations remain underdeveloped. This underdevelopment poses considerable risks for the already vulnerable populations who are being subjected to these programs, potentially including violations of their right to privacy, misuse of their personal data, or their misidentification as enemies or threats. This article weighs these benefits and risks associated with biometrics technology. It analyzes the extent to which law and policy already govern the collection and use of biometrics by armed forces at both the domestic and international levels. It explores why the United States and Canada — the two states whose armed forces appear to be the most heavily engaged in the collection of biometric data abroad — have adopted such different policies with respect to the use of biometrics. It explains why the current international legal and policy vacuum in relation to battlefield biometrics is unacceptable and concludes that the time to discuss best practices is now. Ten non-legally binding guidelines are proposed for consideration and potential adoption by states.
The Changing United Nations Constitutionalism. New Arenas and New Techniques for International Law-Making
Authors: McWhinney Edward 
Published: June 2019

The Advisory Opinion handed down by the World Court on July 20, 1962, concerning Certain Expenses of the United Nations has become a political cause célèbre in so far as the majority judicial position in it was backed up by the Western-sponsored action, in terms of Article 19 of the United Nations Charter, to deprive the Soviet Union and France of their vote in the General Assembly. The Advisory Opinion of the World Court has, however, its own intrinsic interest in terms of juristic method and of basic Soviet and Western differences in scientific approach to law. In his dissenting, judicial opinion in that case, the then President of the Court, the Polish jurist, Judge Winiarski, formulated principles of interpretation which reveal, very dramatically, the basic doctrinal differences between Soviet bloc and Western jurists as to the nature and character of the Charter. As President Winiarski commented:The Charter has set forth the purposes of the United Nations in very wide, and for that reason too indefinite, terms. But… it does not follow, far from it, that the Organisation is entitled to seek to achieve those purposes by no matter what means. The fact that an organ of the United Nations is seeking to achieve one of those purposes does not suffice to render its action lawful. The Charter, a multilateral treaty which was the result of prolonged and laborious negotiations, carefully created organs and determined their competence and means of action.
Exemption from the Jurisdiction of Canadian Courts
Authors: Castel J.-G. 
Published: June 2019

I Persons against whom the jurisdiction cannot be enforcedThe first part of this note deals with the persons who claim immunity from the compulsory jurisdiction of Canadian courts.(1) The Foreign State, Sovereign or Head of Foreign State as a DefendantThe law relating to the immunity of foreign states and sovereigns or heads of foreign states from Canadian jurisdiction is to be found in the common law and has been stated and re-stated in leading cases such as The Parlement Belge, The Porto Alexandre, The Cristina, Dessaulles v. The Republic of Poland and Mehr v. The Republic of China et al. Lord Atkin reduced this law to two propositions:The first is that the courts of a country will not implead a foreign sovereign, that is, they will not by their process make him against his will a party to legal proceedings whether the proceedings involve process against his person or seek to recover from him specific property or damages.The second is that they will not by their process, whether the sovereign is a party to the proceedings or not, seize or detain property which is his or of which he is in possession or control.
Approaches to the Law of Armed Conflict
Authors: Morley Jeremy D. 
Published: June 2019

The international legal framework has traditionally been divided into a “state of war” and a “state of peace.” Most contemporary authorities still insist upon sharp and tidy categorization in this area, although some would prefer a three-fold or a multi-fold division, instead of the standard two-fold split. This whole approach has come under attack in recent years.A division into “states” of “war” and “peace” should theoretically produce simplicity and clarity. Instead, however, it leads to hopeless complications. This is clear as soon as any attempt is made to define the “state of war.”
Models of Rotating Neutron Stars in General Relativity
Authors: Bonazzola S. , Maschio G. 
Published: June 2019

We describe a numerical method of integration of Einstein's equations coupled with the hydrodynamic equations for a perfect fluid. We give, also, some preliminary results.We point out that the analogous problem was considered by Ostriker and Mark (1968) in the Newtonian case; by Thorne (1969) in General Relativity, in the weak angular velocity approximation; by Barden and Wagoner (1969) for disk configurations in the pressure vanishing case.
A Review of the Different Liquid Core Models Used for the Computation of the Dynamical Effects on Nutations and Earth Tides
Authors: Melchior P. 
Published: June 2019

Note: This short review was given during the Symposium at the request of a number of participants to serve as an elementary introduction to the discussion of the results obtained from different Earth models. It was not prepared in advance and is not an original contribution.The first approximation of the figure of a fluid planet is obtained by assuming hydrostatic equilibrium with respect to its gravitational self-attraction and the centrifugal force. When the speed of rotation is not too fast, the equipotential surfaces may be considered to an excellent approximation as ellipsoids of revolution. It is easy to show that these hydrostatic equipotential surfaces are surfaces of equal density (p).
Systematics of Bulge-to-Disk Ratios
Authors: Simien F. , de Vaucouleurs G. 
Published: June 2019

The main results of a new analysis of the spheroidal (I) and disk (II) components of 98 lenticular and spiral galaxies are :
(i)on the average, the magnitude difference between spheroid and total luminosity, ΔmI = BT(I) - BT, varies smoothly along the Hubble sequence from early lenticulars to late-type spirals (Fig. 1);(ii)the trend of ΔmI confirms the concept of the lenticular class as intermediate between E and S classes, not as a parallel sequence;(iii)the large scatter at any given type, σ(ΔmI) ≃ 0.7 mag, is still dominated by measuring and decomposition errors.(iv)The effective surface brightness of the spheroid, μce(I), corrected for galactic extinction AB, decreases by ~2 mag from early to late types, but with a large range (~ 3 mag) at T = const. (Fig. 2a).(v)The effective surface brightness of the disks, corrected for galactic extinction and inclination, μce(II) = μe(II)- AB + 3 log R2s, is almost independent of type, with <μce(II)> ≃ 23.5 for spirals. This implies a corrected central surface brightness μc(0) = μce −1.82 ≃ 21.7, in good agreement with the Freeman rule, but with a large scatter. However, the disks of lenticulars (T< 0) tend to be ~ 0.5 mag fainter than the disks of spirals (Fig. 2b).(vi)The linear effective radii of the spheroidal components are largest, <re (I)> ≳ 1 kpc, among the early type spirals, in agreement with the Hubble classification criterion. The spheroid of lenticulars and late-type spirals tend to be smaller, <re(I)> ≃ 0.5 kpc, but with a large scatter (Fig. 3a). There is no indication of systematic difference between ordinary (SA) and barred (SB) spirals.(vii)The linear effective radii of the disk components are largest <re (I)> ≳ 5 kpc, among intermediate type spirals. The disks of lenticular and late type spirals tend to be smaller (Fig. 3b).(viii)The mean absolute magnitudes of the disk and spheroidal components depend on type (Fig. 4). On the average the disks are brighter (MII ≃ −19.5) among types Sb-Sbc, spheroids (MI ⋍ −19) among types L+ to Sa, but, again, with a large scatter. Disks and spheroids are about equally bright (MI ⋍ MII ⋍ − 19) at stage SO/a (T = 0).
X-ray Observations of Crab-Like Supernova Remnants
Authors: Becker R. H. 
Published: June 2019

On the basis of extensive radio surveys of the galactic plane, approximately 140 sources of diffuse radio emission have been classified as supernova remnants (SNR). Using spectral index and spatial distribution as the primary selection criteria, these have been subdivided into two groups, “shell” and “Crab-like”. In each case, the radio emission is assumed to be of non-thermal origin. The two distinct morphologies arise from two distinct energy sources. For shell remnants, the energy is drawn from the reservoir of kinetic energy in the expanding shock front; in Crab-like remnants, the energy is drawn from the rotational kinetic energy of a central stellar remnant.These two classes of remnants differ significantly in their x-ray emission. With few exceptions, radio shell remnants emit thermal x-rays from shock heated gas which is itself distributed in a shell. Crab-like sources (as defined by their radio properties) emit synchrotron x-rays in a centrally-peaked spatial distribution. Presumably, the x-ray emission from these objects is an extension of the radio spectrum. Crab-like sources have a high probability of containing a compact (unresolved) source of x-ray emission which in analogy to the Crab Nebula, is identified as the central stellar remnant.The general absence of either compact x-ray sources or Crab-like diffuse nebulae within shell sources indicates that active pulsars are not usually formed in SN events which eventually form shell sources. However, there are several examples of remnants which share both shell and Crab-like characteristics so we cannot rule out an evolutionary connection between these two classes of SNR.
The Asiago Catalogue of Quasi Stellar Objects
Authors: di Serego Alighieri S. 
Published: June 2019

A catalogue containing the QSOs known with reasonable reliability from literature published before the end of 1981 has been compiled at the Asiago Observatory by C. Barbieri, M. Capaccioli, S. Cristiani, G. Nardon and A. Omizzolo, and will be published before the end of 1982 by the Memorie della Societá Astronomica Italiana.The present release is an enlarged and updated version of that published by Barbieri et al. (1975). It provides basic data (names, equatorial and galactic coordinates at 1950.0, photometry, redshifts and information on radio emission, variability, morphology, presence of absorption lines, X-ray emission and finding charts) for 2004 QSOs, together with references, individual notes and cross reference tables. Two separate lists contain X-ray data for 271 QSOs (X-ray luminosity, optical-X and optical-radio spectral indexes) and absorption line data for 243 QSOs (absorption systems with their redshift, identified ions and wavelengths, spectral range, resolution and dispertion of the spectra).The catalogue has been carefully checked for internal consistency and several discrepancies with the lists by Hewitt and Burbidge (1980) and by Véron and Véron (1975) have been resolved. The authors intend to provide a magnetic tape version of the catalogue to the Centre de Données Stellaires of the Strasbourg Observatory for distribution to the interested community.
Substructure in Clusters of Galaxies
Authors: Geller M. J. , Beers T. C. 
Published: June 2019

Rich galaxy clusters containing multiple condensations are common. This subclustering affects many cluster properties and provides insight into cluster evolution.“Clumpy” clusters of galaxies are interesting, in part, because N-body simulations indicate that multi-component substructure occurs before complete collapse and virialization (White 1976). Interesting systems can be identified both from x-ray surface brightness maps (Forman et al. 1981) and from contour maps based on galaxy counts (Geller and Beers 1982).
Evidence of Intrinsic Correlation Between the Luminosity and the Velocity Dispersion in Galaxy Groups
Authors: Mezzetti M. , Giuricin G. , Mardirossian F. 
Published: June 2019

By using the two samples of galaxy groups reselected by Rood and Dickel (1979, Astroph. J. 233, 418), we have investigated the significance of the correlations between the virial parameters of groups. Taking into account observational selection effects present in the two samples, together with statistical and observational uncertainties, we show that only an intrinsic correlation between the luminosity L and velocity dispersion V is necessarily required in order to explain all the observed correlations. There is no serious ground to state that the virial radius correlates with both velocity dispersion and luminosity. We also show that the observed slope of the Log L - Log V relation is considerably smaller than the true slope, while the contrary holds for the Log M/L - Log V relation.An analysis similar to that described above, carried on the recent catalogue of nearby groups of galaxies prepared by Huchra and Geller (1982, Astroph. J. 257, 423), seems to reveal that also the intrinsic correlations between L and R, and R and V are significant for this new sample.
Neighboring Superclusters and Their Environs
Authors: Einasto J. , Miller R. H. 
Published: June 2019

Recently finished redshift surveys make it possible to study the large-scale environment of superclusters and their mutual relationship.Figure 1 shows the distribution of nearby clusters in the sky in supergalactic coordinates at two redshift intervals. Nearby clusters in the distance interval 75 to 150 Mpc form a belt around us which is close to the supergalactic equator; its inclination is only 20°. The following superclusters belong to this belt: Ursa Major-Lynx (Giovanelli and Haynes 1982), Coma, Hydra-Centaurus, Pavo-Corona Australes, and Perseus-Pisces. Coordinates and redshifts for a number of previously unknown southern clusters have been derived by Dr. H. Corwin and Dr. M. Tarenghi (Einasto et al. 1982).
Interstellar Extinction in the Magellanic Clouds
Authors: Nandy K. 
Published: June 2019

The extinction properties of interstellar dust in the Large and Small Magellanic Clouds have been systematically investigated, using recent UV observations of early type Cloud members along with complementary visible data. The extinction curves differ systematically from the standard Galactic curve. The latter shows a broad absorption feature centred near 2200Å in virtually all sight lines but this is absent or only weakly present in the SMC; also the SMC extinction in the far UV is the largest known relative to EB-V. Dust in the LMC appears to be intermediate in extinction properties between the SMC and normal Galactic material. However, exceptions from the average extinction curves have been found in both Clouds.Model computations show that the range of grain sizes and their number distribution law may not be significantly different in the Clouds and the Galaxy; the difference in extinction laws can be accounted for by varying the graphite contribution relative to silicate.
Observing, Modeling, and Understanding Stellar Granulation
Authors: Dravins Dainis 
Published: June 2019

Numerical simulations of the three-dimensional structure and time evolution of stellar surface convection are now possible, at least for solar-type stars. Using the output from such simulations as sets of spatially and temporally varying model atmospheres, synthetic granulation images and spectral line profiles are computed, and compared to observations. Thus obtained disk-integrated data agree with observed lineshapes and bisector patterns in different stars, and also permit stellar rotation to be determined. Such simulations represent the first generation of models that are free from the classical ad hoc parameters of ‘mixing-length’, ‘micro-’ or ‘macro-turbulence’, parameters which in the past have characterized and limited stellar astrophysics.To infer the surface structure also in more exotic stars, simpler and parametrized models must still be used to interpret observed line asymmetries. Such models suggest that rapidly rising ‘granules’ cover only a small surface fraction on early-type stars, a situation opposite to that in solar-type ones, and one likely to affect magnetic fields and stellar activity. Theoretical challenges for the future include detailed modeling also of early-type, giant, and other non-solar type stars of different rotational velocities; the hydrodynamics of entire stellar envelopes (including the interaction with global oscillations); and the interaction with magnetic fields (including their generation). Greatly increased computing power will be needed for such detailed modeling throughout the Herzsprung-Russell diagram, possibly requiring custom-designed computers.Signatures of stellar granulation are primarily observed as asymmetries and wavelength shifts in photospheric absorption lines. Observational challenges include achieving sufficient spectral resolution to fully resolve such asymmetries; identifying granulation signatures throughout the HR-diagram (including the blended spectra of cool stars); observing how line asymmetries for a given spectral type depend on stellar rotational velocity, measuring wavelength shifts between groups of different lines in the same star, and between different stars; monitoring lineshift variations during stellar activity cycles; and ultimately high-resolution spectroscopy of spatially resolved granulation structures across stellar disks. The latter will require active optics on future very large telescopes, or the use of long-baseline optical interferometers.
The Impact of Polarimetry on Wolf-Rayet Star Models
Authors: Schulte-Ladbeck Regina E. 
Published: June 2019

Recent observational efforts have presented new results concerning (linear) polarization variations as a function of time as well as wavelength that have considerable impact on WR star models:Polarimetry throughout orbital phase has provided inclinations of double-line spectroscopic binaries containing WR stars with O star companions, thus improving our understanding of the masses and evolution of WR binaries (Schulte-Ladbeck 1989, A.J. 97, 1471). New binary-model calculations were presented at the meeting and continuing comparison with observations should prove productive.
From LBV Binary to WR+OB Binary
Authors: Vanbeveren D. 
Published: June 2019

The LBV phase is generally identified with the hydrogen shell burning phase of a star with initial mass larger than 40-50 M⊙ (see also Humphreys, this volume) and therefore in binaries with ZAMS component masses larger than 40-50 M⊙ and periods larger than 4-7 days the primary may experience a LBV mass loss phase before it reaches its critical equipotential surface (the Roche lobe). I then define the ‘LBV scenario’ of massive close binaries as follows:when a binary component (initial mass larger than 40-50 M⊙) reaches the LBV phase prior to its Roche lobe overflow phase (RLOF), a stellar wind mass loss phase sets in at rates comparable to the rates encounterd during a RLOF process and which are large enough in order to prohibit the occurence of a RLOF.Evolutionary models are computed for close binaries with initial primary masses larger than 50 M⊙ and mass ratios ranging between 0.2 and 1. Special attention is given at the predicted spectral type of the secondary component. In order to determine the mass of the primary at the end of its LBV phase, I have used the following general theorem holding for the most massive stars, i.e.a hydrogen shell burning mass loser with mass larger than 50 M⊙ in a massive close binary restores thermal equilibrium (and becomes a WR star) when helium starts burning in its core and when its atmospherical hydrogen abundance has dropped to Xatm = 0.2-0.3 (by weight).
Absolute Magnitude Determinations from Hydrogen-Line Photometry
Authors: Crawford D. L. 
Published: June 2019

The history and status of Balmer hydrogen-line photometry are briefly reviewed, and problems associated with calibrations in general are commented on.The calibration work at Kitt Peak is described in some detail for B, A, and F type stars. The data used, the determination of intrinsic colours and colour excesses, photometric classification, and the relation of our indices to other people's are reviewed. With this background, the procedure used in establishing the absolute magnitude — Hβ calibration is given, and the preliminary calibration is presented. Finally, the work remaining to be done before the calibration is final is noted, and a comparison is given to Blaauw's zero-age main sequence calibration.