bluuebunny/crossref_metadata_2025 huggingface dataset:
Exceeding the Limits of Territorial Bounds: The Helms-Burton Act
Authors: Fairley H. Scott
Published: June 2019

The author argues that the Helms-Burton Act violates general principles of international law. The analysis begins with a brief discussion of the extraterritorial purposes, structure, and operation of the act, followed by a survey of international responses to Helms-Burton by the principal trading partners of the United States: diplomatic protest, formalized dispute settlement under international trade agreements, retaliatory blocking leghlation, and multi-hteral scrutiny in and by international institutions. The author then turns to principles of jurisdiction with a view to demonstrating that Helms-Burton does not meet the applicable thresholds to support either the private right to sue for trafficking in confiscated property under Title III of the act or the governmental exclusion of designated aliens from admission to the United States under Title IV. In this regard, substantive international law arguments in relation to extraterritoriality and nationality, remoteness, the effects doctrine, human rights, and the reasonable expectations of other nations are also considered.
On Expelling Nigeria from the Commonwealth
Authors: Carmody Chi
Published: June 2019

In November 1995, the execution of Nigerian writer Ken Saro-Wiwa led to Nigeria’s suspension from the Commonwealth and the possibility of its expuhion from membership. The absence of an expulsion clause for the Commonwealth led to the question whether the association has the inherent power to expel and whether any such power of expuhion is limited by international law. A review of treaties, customary international law, and commentary suggests that the Commonwealth can expel a member by use of implied power. Other factors, however, militate against Nigeria’s expuhion. Once expelled, Nigeria would be free to behave as it saw fit. Expuhion could aho divide the Commonwealth and make other members think twice about their membership obligations. The author concludes that expuhion from the Commonwealth must be a last resort.
Federalism, Biculturalism, and International Law
Authors: McWhinney Edward
Published: June 2019

The Contemporary “Great Debate” over the future of Canadian Confederation, whatever else it may have done, has at least shattered a number of comfortable old maxims as to the inevitable course and development of federal constitutions. “Bryce’s law” — or the asserted axiom that federalism is simply a transitory step on the way to political unity — has been exposed for what it really is, a generalization based too easily upon the experience of the essentially “Anglo-Saxon,” English-speaking federal systems with which Lord Bryce happened to be acquainted at the time he was writing. Even Dicey’s triadic critique long accepted as a truism in Empire and Commonwealth legal circles — that federalism inevitably means weak government, conservatism, and legalism — may be seriously doubted, as to its first two points at least, in the light of the strongly centripetal governmental trends in the main federal systems in modern times, and the concomitant association of that centralizing trend with political concepts of social and economic planning and community determination and direction of financial policy. It may be, as a French-Canadian jurist contended at a conference on Federalism held in Toronto in November 1964, that those English-speaking Canadian jurists who, in the 1930’s and the 1940’s, preached both the desirability and also the inexorability of the march to Ottawa were “plucking the Socialist fruit from the tree before it was fully ripe.” We are, in any case, indebted to French Canada for reminding us that theories of historical inevitability, when applied to social phenomena, must inevitably tend to break down if they ignore the crucial variable of the human factor. For while complex political-legal relationships and interactions often seem to be shaped and conditioned by intractable social and economic forces, in the end the dynamic element in the community power process must still be the free will of the main actors or participants in it. This is in essence William James’s point that truth is not an abstract quality inherent in an idea but something that happens to it in the unfolding of events. In constitutional law, what may have seemed right and proper and, if you wish,truefor Canada in the 1930’s and the 1940’s may not necessarily be so today.
Compliance Committees and Recent Multilateral Environmental Agreements: The Canadian Experience with Their Negotiation and Operation
Authors: Adsett Hugh , Daniel Anne , Husain Masud , McDorman Ted L.
Published: June 2019

In order to enhance and encourage compliance with obligations in multilateral environmental agreements (MEAs), states have agreed to the creation of compliance committees for all of the recent MEAs. Canada has been a strong supporter of the compliance committee experiment and an active participant in the negotiation and operation of numerous MEA compliance committees. This article does three things. First, it examines the international legal nature of the MEA compliance committees. Second, the key issues of the structure of the committees are explored. Finally, the article look at the development and operation of compliance committees pursuant to: the Montreal Protocol; the LRTAP Convention; the Espoo Convention; the Basel Convention; the Cartagena Protocol; the Rotterdam Convention; the Stockholm Convention; and the Protocol to the London Dumping Convention.
Radiation Warfare: A Review of the Legality of Depleted Uranium Weaponry
Authors: Hulme Karen
Published: June 2019

Criticized by many as the new “weapon of mass destruction,” lauded by some as the “weapon of choice in combat,” the use of depleted uranium ammunition in warfare raises many legal questions. Designed as a point weapon to penetrate armoured targets, scientific studies prove that depleted uranium has both chemically and radioactively toxic characteristics. Clearly, every weapon of war will have some affect on human health and the environment, but the laws of armed conflict have evolved to place limits on the level of harm viewed as permissible and legal. Does this “weapon of choice,” therefore, breach the international laws of armed conflict?

Although the subject of media frenzy in the immediate aftermath of the 1999 Kosovo conflict, the use of depleted uranium ammunition in Iraq 2003 raised little media attention. How could the use of such a controversial weapon in 1991 go largely unnoticed just four years later? Does this lack of global condemnation necessarily lead to the conclusion that the “dictates of the public conscience” have evolved in regard to the use of this previously controversial weapon of war? This article seeks to analyze the legality of the use of depleted uranium ammunition — the main question being whether the existing laws of armed conflict are already sufficient to address any human and environmental concerns.
Determining the Existence of Countervailable Subsidies in the Context of the Canada-United States Softwood Lumber Dispute: 1982–2005
Authors: Sandford Iain
Published: June 2019

This article examines the history of countervailing duty determinations with respect to softwood lumber between 1982 and 2005. The piece is divided into two main areas of analysis. First, the article chronicles and reviews certain key determinations made throughout the history of softwood lumber countervailing duty proceedings. It examines, in particular, certain recurring themes as well as issues that shed light on some of the interesting jurisprudential questions that arise out of the case study. Second, having completed this review, the note turns to distill some lessons from the experience to date. These lessons focus on the light shed by the lengthy history of the softwood lumber dispute upon the nature of subsidies disciplines in international trade. They also focus on what the softwood lumber dispute reveals about the relationship between different judicial actors at the international level. The article closes with some reflections on the limits of international dispute settlement tools in highly contentious and politicized cases.
Les zones de pêche de Terre-Neuve et du Labrador à la lumière de l’évolution du Droit international
Authors: Morin Jagques-Yvan
Published: June 2019

Depuis Que La Seconds Conférence Sur le droit de la mer, tenue à Genève en 1960, a échoué dans sa tentative de fixer de manière uniforme la largeur de la mer territoriale et de la zone de pêche des Etats, la situation a évolué sans cesse dans le sens de l’extension des compétences étatiques vers la haute mer.

Avant 1960, plus de vingt pays revendiquaient déjà des eaux territoriales ou une zone de pêche de douze milles marins, et quelquefois davantage. A ces Etats sont venus s’ajouter au moins une quinzaine d’autres qui ont étendu leur mer territoriale à douze milles, tandis que 25 environ ont opté pour une zone de pêche de douze milles, tout en conservant des eaux territoriales plus exiguës. Parmi ces derniers, il convient de mentionner en particulier les signataires de la Convention européenne sur les pêcheries, du 9 mars 1964, qui consacre au profit de l’Etat riverain l’établissement d’une zone de pêche de six milles, ainsi que d’une zone additionnelle de même largeur où l’exclusivisme est tempéré par certains droits réservés aux co-contractants, quelle que soit, par ailleurs, la largeur de la mer territoriale de chacune des parties. Si l’on considère que 28 Etats ne possèdent pas de littoral et que, d’autre part, 9 pays ont étendu leurs compétences au-delà de douze milles, on constate que les deux tiers des Etats côtiers (environ 72 sur 107) acceptent maintenant et même soutiennent la tendance à l’extension des zones de pêche exclusives — quand ils ne vont pas jusqu’à élargir tout simplement leurs eaux territoriales.
International Regional Organizations and their Travel Documents
Authors: Turack Daniel G.
Published: June 2019

Functional independence of international institutions is a sine qua non to their effective operation. Current international law reveals that international organizations have a legal capacity and certain privileges and immunities bestowed upon them by their member states to ensure their independence and that of their staffs. One vital component of functional independence is the freedom of travel for all members of the international staff. In examining the features of freedom of travel necessary for international organizations to discharge their responsibilities effectively, C. W. Jenks wrote:

The freedom of movement which is necessary comprises more than the absence of any special restrictions; it includes the usual facilities for official travel, such as diplomatic or other special visas, priorities where these are necessary, exemption from immigration regulations and formalities, and similar measures; taken cumulatively these facilities involve a considerable saving of time and energy and are therefore an important element in securing the expeditious and unhindered travel necessary to the prompt discharge of international responsibilities.
On Consensus
Authors: D’Amato Anthony
Published: June 2019

Two Phenomena Have Converged in recent years to account for the current interest among international lawyers in the concept of the “consensus” of states. The first is the recognition in jurisprudence that all law, and particularly the international legal system with its lack of centrally organized sanctions, is founded on inductively verifiable psychology and not in deductive principles purportedly derived from God, nature, or reason. If international law is nothing more or less than what states (national decisionmakers and their counsel) think it is, then do not particular rules of international law owe their existence and transmutations to the flow of international consensus?
An Historical Introduction to the Teaching of International Law in Canada
Authors: MacDonald R. St. J.
Published: June 2019

The purpose of this paper is to describe from an historical point of view the main developments in the teaching of international law in Canadian law schools from the time when the subject was first taught, in the mid-nineteenth century, to the early years of the present decade.

The paper is divided into five parts, dealing respectively with the law schools of Quebec, the Maritime provinces, Ontario, the Prairie provinces, and the Pacific coast. A chronological account is given of the teaching of international law in each law school, describing first the teachers, their backgrounds, personalities, attitudes to international law and other interests, and, second, the courses taught, texts and casebooks used, and the importance placed on international law in the general curriculum, as indicated by the time devoted to it, whether it was elective or compulsory, and the year in which it was taught. For the most part, the discussion is restricted to the law schools in the various universities. Although it would be interesting to consider the parallel development of international law teaching in other disciplines, such as political science, the subject is so vast that some limit must be imposed on it.
The Labour Conventions Case Revisited
Authors: La Forest Gerard V.
Published: June 2019

So much has been written about theLabour Conventionscase that one hesitates to add to the flow of ink. But the bulk of these writings simply reflects the diametrically opposed views about the correctness of the decision on both technical and practical grounds. Most commentators from English Canada have bewailed the decision in this case that power to implement treaties in Canada is divided between the federal parliament and provincial legislatures according to the usual division of legislative power. On the other hand, French Canadians overwhelmingly support the decision. Recent literature has concentrated on techniques that can be employed to secure federal-provincial co-operation in effecting international action. Still, little notice has been taken of gradually evolving doctrine in the Supreme Court of Canada that should facilitate the exercise of Canada’s sovereign status in the international sphere, whatever the ultimate fate of theLabour Conventionscase. The purpose of this article is to examine the nature of this evolution and to suggest possible paths for future developments.
The Role of The United Nations Environment Program (UNEP) in the Development of International Environmental Law
Authors: Bacon T. C.
Published: June 2019

Little or no attention was given to the development of international environmental law prior to the Stockholm Conference of 1972. Nor was it intended that the Conference should consider legal questions: it was to be merely a technical, scientific meeting. During preparations for it, however, a change in character occurred, and the Conference became a politically oriented endeavour designed to make policy decisions on global environmental problems. This change permitted the Twenty-seven Power Preparatory Committee responsible for the preparation for the Conference to concentrate on broad policy considerations. In this context, a real concern for the future of international environmental law was evident.
Rotational Characteristics of Coronal Holes
Authors: Wagner William J.
Published: June 2019

From May 1972 to October 1973, daily measures were obtained of EUV coronal hole areas appearing at the central meridian. Autocorrelations of these coronal hole area time series provide synodic rotation periods which indicate an almost rigid rotation by such features for lag lengths as short as one rotation. The rotation periods of coronal holes at high latitudes best compare with inferred interplanetary field rotation periods.
Observations of Magnetic Fields on Late-Type Stars
Authors: Marcy Geoffrey W.
Published: June 2019

The “Robinson” method for measuring magnetic fields on solar- and late-type stars is reviewed. The results of such measurements for a sample of 29 G and K main-sequence stars are presented. The area covering-factors of magnetic regions are greater in the K dwarfs than in the G dwarfs, but no spectral-type dependence is found for the field strengths, contrary to expectations of some flux-tube models. The dependence of Ca II H and K emission on magnetic fields and Teff is consistent with theoretical expectations for “slow-mode” mhd wave-generation rates, but inconsistent with those of other mhd modes. Coronal soft X-ray fluxes correlate well with the magnetic fields, and it is argued that Alfvén waves are the likely energy-transport mechanism. Surface magnetic fluxes vary with rotation as , depending on spectral type.
The Mount Wilson Program for Stellar Activity Cycles
Authors: Vaughan Arthur H.
Published: June 2019

The present review will focus upon the incidence, form, and characteristic timescale of long-term chromospheric variations that, from the work of O.C. Wilson and his successors, can be descerned in records of CaII H and K emission now extending over 16 years, and the relation, if any, between properties of activity cycles and stellar mass, age, and rate of rotation, in the light of current evidence.
Magnetic Braking and Angular Momenta of Protostars
Authors: Mouschovias Telemachos Ch.
Published: June 2019

A contracting, typical, isothermal interstellar cloud or fragment, magnetically linked to the surrounding medium, loses angular momentum so efficiently that it remains in nearly synchronous galactocentric orbit as long as the field is frozen in the matter. At a high enough density ndec, the field decouples from the matter due to ambipolar diffusion. Thereafter angular momentum is essentially conserved and, consequently, there is a one-to-one correspondence between ndec and the angular momenta of binary and single stars that can ultimately form. Although the calculated rotational velocities (typically, 100 km/sec) are not yet refined enough to account for peculiarities among different spectral classes which may be due to phenomena following protostar formation, they are encouragingly consistent with observations.
Outlook for Ground-Based and Space Observations
Authors: Vaiana G.S.
Published: June 2019

The presentations given at this Symposium have made clear that we are witnessing an exciting period in the study of solar activity, and in the ancillary study of magnetic field dynamics in solar-type stars: the new space observations obtained within the past four years, together with the renaissance in ground-based observations, have occasioned a burgeoning in our phenomenological understanding of stellar activity in its manifold facets, and have encouraged a substantially greater interest in the problem of magnetically-coupled activity in stars by the theoreticians. This excitement must not distract us from the realization that in this branch of our science, much of the impetus towards new research has come, and very likely will continue to come, from observations; with this fact in mind, I would like to address the possible evolution of our experimental science in response to the new observational and theoretical results.
Stochastic Starformation and Bubbles in the Large Magellanic Cloud
Authors: Feitzinger J. V.
Published: June 2019

Nearly all places in the LMC where ring nebulae or shell structures in the neutral or ionized interstellar medium are observed, an OB association and/or WR-stars can be located (Braunsfurth, Feitzinger, 1983). Several mechanisms have been propsoed to generate shell or bubble structures: stellar winds, supernovae explosions, evolving HII regions, sequential starformation, collapsing hydrogen clouds interacting with stellar winds and radiation pressure. Ordered motions resulting in a shell or bubble structure are the result of almost any point like energy injection into the interstellar medium. Therefore all the mechanisms result in similar morphological structures, thus similar shapes can have heterogeneous origins.
Kinematics and Dynamics of the Magellanic Clouds
Authors: Freeman K. C.
Published: June 2019

Why are the kinematics and dynamics of the Magellanic Clouds worth studying ? Some of the reasons are:

1.

The Clouds are the closest examples of Magellanic systems. These asymmetric systems give some interesting dynamical problems. Because the Clouds are so close, a unique amount of information can be obtained on the kinematics of objects of all ages. This should be very helpful for understanding the dynamics.

2.

The Clouds and the Galaxy are interacting. This produces complex kinematics of the gas in and between the Clouds, and also the Magellanic Stream. Again, very detailed information can be derived. We would like to know enough about the gas dynamics of interacting galaxies, to be able to explain the kinematics produced by this interaction.

3.

The interaction will affect the star formation and chemical evolution in the Clouds. As new results are obtained on the star formation history and the chemical evolution, it is important to follow in parallel the dynamical history of the system, to see if the dynamics, star formation and chemical evolution can be tied together.
The Magellanic Stream and its Related Problems
Authors: Fujimoto M. , Murai T.
Published: June 2019

A brief survey is made of recent 21-cm and optical observations of the Magellanic Stream(MS). The space orientation of the Magellanic Clouds is touched upon in relation to modelling the MS. After summarizing a variety of models for the MS, we show that if our Galaxy is massive with a huge dark halo, a tidal model is most suitable for reproducing its characteristic structure and high-negative radial velocity. Past orbits of the Large and the Small Magellanic Cloud (LMC and SMC) are determined uniquely for the last 2×109 yr, if we postulate that the LMC and SMC are bound together for 1010 yr: Highly-noncircular motion of the SMC around the LMC could give a clue to understand some peculiar features associated with the Magellanic Clouds.
HI Surveys of the Magellanic System
Authors: Mathewson D. S. , Ford V. L.
Published: June 2019

The global distribution of HI in the Magellanic System is shown in Figure 1. The gas covers some 1500 square degrees of sky and has a mass of 1.8 × 109 M⊙. There are four main components: the LMC, the SMC, the inter-Cloud region and the Magellanic Stream. The integrated HI of the first three components is mapped in Figure 2 with the Parkes 64-m radio telescope which has a resolution of 15 arc min. The previous surveys of McGee and Milton (1966), Hindman (1967), Mathewson et al. (1979) have been combined with a recent survey by Mathewson et al. (1983) of the outer regions of the System to give this large-scale picture of the gas distribution. The last two surveys were made with a velocity resolution of 4.12 km s−1 and a minimum detectable signal of 0.2 K. The long spurs extending from the LMC and SMC and the bridge joining the two galaxies with prominent spurs pointing to the Magellanic Stream are all compelling evidence for tidal interaction between the LMC and SMC (Mathewson 1976a, Murai and Fujimoto 1980). The detailed velocity field of the HI is given in Mathewson et al. (1983). Its large-scale features are shown in Figure 5 of Mathewson et al. (1979) which indicate that the radial velocities of the inter-Cloud region form a velocity continuum with those of the LMC and SMC. This plus the continuity of the general velocity gradient across the entire Magellanic System strongly suggest that the two galaxies are bound.
Magnitude absolue moyenne des RR Lyrae
Authors: Heck A.
Published: June 2019

By a method based on the principle of maximum likelihood, we obtained for a sample of 102 RR Lyrae stars and σMpg = 0.5 ± 0.2. We could not confirm the results of Clube and Jones (1971). The study of the correlations between , the period, the abundance parameter ΔS and the light variation amplitude showed that on ground of the present data, no significant correlation can be established.
The Search for Unwanted Signals: Systematic Trends in Proper Motions of Fundamental Stars
Authors: Brosche P. , Schwan H.
Published: June 2019

An investigation of the N30 along the same lines as that of the FK4 (Brosche and Schwan 1981) reveals quite similar non-standard systematic motions. Some consequences are indicated for the determination of cluster parallaxes, of secular parallaxes and of the galactic rotation. In general, we stress the necessity of always searching for every signal in the data - including those ones which are not understood and hence not ‘wanted’.
Preliminary Precise Radio/Optical Positions of Selected Stars
Authors: Florkowski D. R. , Johnston K. J. , de Vegt C. , Wade C. M.
Published: June 2019

Positions of the radio emission associated with stars were determined along with precise optical positions of the stars. The high precision obtained shows that radio star observations are a practical means of determining the relationship between the optical and radio reference frames.
Internal Refraction in Meridian Circles
Authors: Høg E.
Published: June 2019

Tube refraction of the order 0″.3 inside a meridian circle is a source of systematic errors that has not been noticed before. Natural convection due to cooling at night or heating during day will create primarily vertical temperature gradients in the air. This is shown by experiments at a collimator where typically 1 K/m was found inside the tube even when the gradient outside the tube was much smaller. A method of tangential ventilation of the tube was used to eliminate the gradients. It is shown that the resulting effect on seeing or image motion will be to the better when the ventilation system is properly designed, and the design for a conventional meridian circle and for a Glass Meridian Circle is discussed.
ISO and Laboratory Astrophysics
Authors: Allamandola L. J.
Published: June 2019

ISO, the Infrared Space Observatory is capable of measuring spectra across most of the mid-infrared, the region from 4000 to 500 cm−1 (2.5-20 μm). Of these 3500 cm−1, about 670 have been inaccessible to astronomers due to strong atmospheric absorptions and about 750 cm−1 require an airborne platform, making access limited. ISO will provide high quality spectra in the 19% of the celestial mid-infrared which has never been studied and dramatically increase the number of spectra in the 21% with limited access. Thus ISO has the potential to nearly double our knowledge of the mid-IR spectroscopic properties of the cosmos. This knowledge, in turn, will revolutionize our understanding of its chemical make-up because of the mid-infrared's powerful compositional diagnostic capabilities.
Astrophysical Problems Involving Carbon Re-appraised
Authors: Hare J P , Kroto H W
Published: June 2019

The molecule C60, Buckminsterfullerene, was discovered1-3during laboratory experiments motivated by problems associated with processes involving carbon in stars and space4,5. Astronomical puzzles also lay behind the experiments which led to the molecule's extraction and structure confirmation6-8. Although the resulting breakthrough has opened up exciting new avenues of chemistry, physics and materials science here on earth9the original astrophysical questions still remain and are even more tantalising now than they were before. Some of the puzzles are here re-addressed in the light of the new understanding which the fullerene discovery has brought. Indeed we shall look at the questions through magenta coloured spectacles and note that there are new and even more intriguing parallels between the behaviour of carbon on earth and space. The article contains a brief account of the processes responsible for the synthesis of carbon in stars and its dissemination throughout the Galaxy as this information is deemed necessary to gain an intrinsic understanding of the amazing role carbon plays in nature.
The D/H Ratio in Molecular Clouds
Authors: Tielens A.G.G.M.
Published: June 2019

This paper summarizes our understanding of the dominant D-reservoirs in molecular clouds and suggests possible direct determinations of the D-abundance. It is concluded that rotational HD lines from shock regions provide the best way to determine the gas phase D-abundance. In cold dense cores, the dominant gas phase D-reservoir is likely to be atomic D, because of expected inefficient HD formation on grain surfaces. The gas phase D-abundance derived from observations of dense cores is ≍5 × 10-6/n4 (with n4 the total density in units of 104 cm−3). A large fraction of the D (≍50%) may be locked up in deuterated molecules in grain mantles. A small fraction (≍2%) may be locked up in the photolyzed residues of such grain mantles. PAHs will also be deuterated (PADs), containing ≍1% of the D. Finally, it is likely that all of these processes have contributed to the D-enrichment observed in solar system materials.
Search for the 4430 Å DIB in the Spectrum of Coronene
Authors: Ehrenfreund P. , D'Hendecourt L. , Verstraete L. , Leger A. , Schmidt W.
Published: June 2019

Polycyclic Aromatic Hydrocarbon (PAH) molecules have been proposed as candidates to explain the Diffuse Interstellar Bands (DIBs). We have performed laboratory measurements of coronene, using rare gas matrix isolation techniques and UV photolysis. Our aim was to search for a possible identification of the 4430 Å DIB, but also to provide data almost free from environmental band shifts and broadening, which can be used for astronomical identification of the species.
What Species Remain to be Seen?
Authors: Turner B. E.
Published: June 2019

We review what species remain to be seen for several types of astrochemistry: Thermochemical Equilibrium (TE) in circumstellar envelopes (CSEs); photo- and ion-molecule chemistry in CSEs; ion-molecule chemistry in cold interstellar clouds; grain chemistry (passive, catalytic, disruptive); and shock chemistry. In CSEs, a rich Si gas-phase chemistry is now recognized, and two predicted species (SiN, SiH2) have been seen. Others are predicted. In the ISM, a global picture of refractory-element chemistry predicts that compounds of Mg, Na, Fe, and possibly Al occur with detectable gas-phase abundance. Predicted species require laboratory synthesis and spectroscopy. Reactions of hydrocarbon ions with neutral species dominate the formation of the families CnH, HCnN, H2Cn, and CnO in both interstellar (TMC-1) and circumstellar (IRC10216) cases, and readily explain the favored values of n in each case as well as predicting which higher-n species remain to be seen. Confirmation of H3O+ (interstellar) is discussed.
Evolutionary Models of Interstellar Chemistry
Authors: Prasad Sheo S.
Published: June 2019

Evolutionary chemical models are ultimately unavoidable for a full understanding of interstellar clouds. They include not only the chemical processes but also the dynamical processes by which the modeled object came to be the way it is. From an evolutionary perspective, dark cores may be ephemeral objects and dynamical equilibrium an exception rather than norm. Evolutionary models have numerous advantages over “classical” fixed condition equilibrium models. They have the potential to provide more elegant explanations for the observed inter-cloud and intra-cloud chemical differences. The problem of the depletion of gas phase molecules by condensation onto the grain may also be less serious in evolutionary models. Hence, these models should be actively developed.
Molecular Line Observations Towards W58 and GL490
Authors: Roh D.G. , Kim H.R. , Minh Y.C. , Auh B.R. , Koo B.C.
Published: June 2019

We observed 3 mm transitions of several interstellar molecules toward star-forming regions in W58 and GL490 using the 14 m Daeduk Radio Telescope (Korea). We derive molecular abundances for the“broad” components observed with a high spectral resolution, which could represent the abundances of outflowing materials.
Panel Discussion: The CO/H2 Abundance Ratio
Authors: Van Dishoeck E.F. , Glassgold A.E. , Guélin M. , Jaffe D.T. , Neufeld D.A. , Tielens A.G.G.M. , Walmsley C.M.
Published: June 2019

The observational and theoretical information on the CO/H2 abundance in a variety of astrophysical regions including diffuse clouds, dense star-forming regions, shocked gas and circumstellar envelopes is discussed and reviewed.
Spectral Synthesis of Cool Components of Symbiotic Stars
Authors: Pereira Claudio B. , Codina Landaberry Sayd
Published: June 2019

We analyzed the optical spectra of cool component of symbiotic star SY Mus by means of spectral synthesis technique in order to derive the atomic abundances using the Minneart formulae for computing the atmospheric opacities. We obtained a satisfactory agreement between the observed and computed spectra and the resulting abundances were consistent to the solar abundances.
Cometary Chemistry
Authors: A'Hearn Michael F.
Published: June 2019

The key problem in cometary chemistry is to observe abundances of species in the coma and to reassemble those species into the species that are present in the nucleus. The limitations are primarily due to poorly constrained models and the lack of uniqueness in reassembling parent species from the fragments when not all of the fragments are observable. These problems will be illustrated with several examples.
Type II Clathrate Hydrate Formation in Cometary Ice Analogs in Vacuo
Authors: Blake D. F. , Allamandola L. , Sandford S. , Hudgins D. , Freund F.
Published: June 2019

Clathrate Hydrates can be formed under high vacuum conditions by annealing vapor-deposited amorphous ices of the appropriate composition. When astrophysically significant H2O:CH3OH ices are deposited and annealed, Type II Clathrate Hydrates are formed which can hold up to 6 mole % large guest molecules such as methanol and 12 mole % small guest molecules such as CO2 and CO. The solid state transformation of amorphous mixed molecular ice into crystalline clathrate hydrate and its sublimation at higher temperatures may serve to explain heretofore anomalous mechanical and gas release properties observed in cometary ices and laboratory ice analog experiments.
Gas Production Rates in Comets
Authors: De Almeida A.A.
Published: June 2019

Emission fluxes of CN, C2and C3carbon- bearing molecular species observed in the coma of comets Bennett (1969i ≡ 1970II), West (1975n = 1976VI), P/Halley (1982i), Hartley-Good (1985l) and Bradfield (1987s) are analysed in the framework of Haser model. CN, C2and C3production rates are determined using recently derived fluorescence efficiencies. The dependence of CN, C2and C3production rates on the heliocentric distance and the possible correlations among these radicals is studied and briefly discussed.
Solar System - Interstellar Medium: A Chemical Memory of the Origins
Authors: Despois D.
Published: June 2019

The growing body of data on solar system objects and interstellar space provides us with new tests of the connection between the two. We emphasize here the role played by the study of comets through the properties of the dust, the chemical composition of volatiles and the elemental abundances. These data inform us on cometary matter formation, and hence on conditions in the protosolar nebula. Under the adopted scenario of formation in a cold environment, with little further processing, cometary abundances are even new constraints to interstellar (gas and solid phase) abundances. Several points specific to the chemical modelling of the collapsing cloud and of the protosolar nebula are listed.
Formation of Comets: Constraints From the Abundance of Hydrogen Sulfide and Other Sulfur Species
Authors: Despois D. , Crovisier J. , Bockelee-Morvan D. , Colom P.
Published: June 2019

Recent determinations of H2S and other sulfur compounds abundances in comets and in Orion KL bring new tests of the origin of cometary matter.
A Diagnostic Spectral Indicator of the Exposure Age of an Asteroidal Surface
Authors: Nuth Joseph A.
Published: June 2019

The energy of the SiH vibrational fundamental has been shown be extremely sensitive to the oxidation state of the silicon to which the hydrogen is bound, ranging from 4.4 microns in highly oxidized silicate grains to 4.74 microns in silicon carbide (Moore, Tanabé and Nuth, Ap. J. (Lett.) 373, L31-L34, 1991). Yin, Ghose and Adler (Appl. Spectrosc. 26, 355-7, 1972) have shown that the process of ion-sputtering a metal oxide results in chemical reduction, due to the high sputtering yield and volatility of oxygen relative to the metal. These authors have shown that solar wind ion-sputtering of lunar soils could provide an explanation for the observed solar wind darkening of the lunar surface. We hypothesize that a similar ion-reduction process could occur on asteroidal surfaces exposed to the solar wind. A second consequence of solar wind exposure would be the implantation of hydrogen ions into the asteroidal surface. Stein (J. Elec. Mat. 4, 159-174, 1975) has shown that hydrogen-ions implanted into silicon exhibit infrared absorptions between 4.5 and 5.5 microns: similar features should result from the ion-implantation of hydrogen ions into partially reduced silicate minerals and glasses. The position of such features would be indicative of the local chemical environment of the silicon atom to which the hydrogen was bound.
Long Term Evolution of the Solar System
Authors: Wisdom Jack
Published: June 2019

The mapping method of Wisdom (1982) has been generalized to encompass all n-body problems with a dominant central mass (Wisdom and Holman, 1991). The new mapping method is presented as well as a number of initial applications. These include billion year integrations of the outer planets, a number of 100 million year integrations of the whole solar system, and a systematic survey of test particle stability in the outer solar system.
The Evolution of Jupiter Family Comets over 2000 Years
Authors: Tancredi G. , Rickman H.
Published: June 2019

The orbital evolution of the whole sample sample of short-period comets was computed by numerical integrations for a time interval of 2000 yr centered on the present epoch. This data base is intended to serve in various studies involving the statistics of orbital evolution and correlation with physical parameters or discovery circumstances. We present some results concerning the following aspects: the evolution of the orbital elements and their past-future asymmetry, statistics on the discovery of comets and on the encounters of comets with Jupiter.
Engineering Potential for Lunar Missions After Apollo
Authors: Burke James D.
Published: June 2019

With results of past and present lunar exploration programs in hand, it is now possible to outline the next logical steps in the exploration and use of the Moon. This paper describes first, a set of mission objectives and engineering capabilities considered desirable and feasible for projects following soon after Apollo, and second, some objectives for the farther future.
Lunar Mare Ridges, Rings and Volcanic Ring Complexes
Authors: Strom Robert G.
Published: June 2019

Mare ridges often consist of two separate but related features: (1) a broad gentle arch overlain by (2) a sharper, more contorted ridge. Often these sharper, secondary ridges have flowed into craters in the adjacent terrain indicating they are extrusions. Major flows in Mare Imbrium appear to have issued from several prominent mare ridges. These flows show color differences which may be related to their abundance of titanium. The association of flows with mare ridges, the broad arching linked with many ridges and the coincidence of linear ridges with the directions of major fracture patterns in the highlands indicates that arched mare ridges are dike, sill or laccolithic-type intrusions along major fractures. In many cases these intrusions appear to have broken through the surface to form short flows and bulbous lava extrusions. Mare ridges unassociated with arching are probably lava extrusions only.

Mare ridges often take the form of rings indicating that they developed along ring fractures. Several linear mare ridges and mare ridge rings have bright hills situated along them and are considered to be post-mare volcanic hills of more siliceous composition than the maria. Evidence suggests that many of the ring structures are post-mare volcanic ring complexes formed over large igneous masses.
On the Origin of Central Peaks in the Crater Formations Filled by Melt After Impacts
Authors: Křivský L.
Published: June 2019

An attempt is made at explaining the successive origin of the central peaks and terrace ring-wall in the crater formations filled with melt after impacts.
The Thermoluminescence of Lunar Samples
Authors: Garlick G. F. J. , Robinson Irene
Published: June 2019

Studies of thermoluminescence emission from lunar samples show that at lunar day surface temperatures and even at 18°C the trapped electron responsible are decaying to their ground states by a non-thermal process. Data from various workers show similar characteristics with respect to this process. They show that thermoluminescence cannot be used as a technique for dating lunar samples (or terrestrial plagioclases) over any significant geological period. A quantitative model for the non-thermal process is proposed.
Summary Introduction
Authors: Deutsch A.
Published: June 2019

Gas can be observed to flow from a wide variety of stars into the interstellar medium, and to do so in a fascinating variety of ways. In some flows, the temperature exceeds a million degrees; in others, it cannot be distinguished from zero. Flow velocities range from 5 000 km/s down to one or two km/s at the limit of detection. The particle densities in some flows are at least 109 times larger than in others. The rates of mass-loss span the range from zero to probably more than 1026 g/s.
Kinematics and dynamics of OH/IR stars
Authors: Dejonghe H.
Published: June 2019

The available kinematical data on OH/IR stars is discussed, and dynamical models for the OH/IR stars are presented.
Bulge K and M giants
Authors: Terndrup Donald M.
Published: June 2019

Several independent studies of the abundances and kinematics of K and M giants in the inner Galaxy (R < 2 kpc) are assembled to trace out this region's global properties. The mean metal abundance is [M/H] ≈ +0.3 at R = 0.5 kpc, and declines by about 1.2 dex out to R = 2 kpc. The line-of-sight velocity dispersion at R = 0.5 kpc is σr ≈ 115 km sec—1 for all population tracers, and declines by d log σr/d log R = —0.4. It now seems fairly clear that only the most metal-poor K giants become RR Lyrae variables, while the more metal-rich ones become late M stars. There is some evidence that the most metal-rich stars are in a flatter, more rapidly rotating system. Metal abundance ratios for a few K giants suggest that the inner Galaxy may have formed rapidly.
The Bulge of the Milky Way and cosmic rays
Authors: Jansen F. , Wenzel K.-P. , Sullivan D.O' , Thompson A.
Published: June 2019

The propagation of cosmic ray protons and anti–protons from the inner Galaxy via the galactic halo to the Sun supplies a good agreement with the observed cosmic ray gradient and is in the order of the measured anti-proton flux. Ultra heavy cosmic ray nuclei may have the same origin.
Rapid gas fueling in a barred potential by self-gravitational instability
Authors: Wada Keiichi , Habe Asao
Published: June 2019

Recent IRAS surveys have revealed that large infrared luminosities are originated from active star forming regions in galaxies (Soifer et al. 1986). Such starburst regions are frequently located in galactic central regions and CO observations indicate that these regions contain a large amount of molecular gas (e.g. Ishizuki et al. 1990). However, the triggering mechanism for starbursts and the mechanism of the high mass supply rate of gas into a galactic center are still unclear.
SIO maser survey of the Bulge IRAS sources
Authors: Izumiura H. , Ono T. , Yamamura I. , Okumura K. , Onaka T. , Deguchi S. , Ukita N. , Hashimoto O. , Nakada Y.
Published: June 2019

SiO maser emission from the Bulge IRAS sources has been searched by the v=1, J=1−0 and v=2, J=1—0 transitions to investigate the kinematics of the Galactic Bulge, resulting in a sample of 124 line-of-sight velocities. The rotation velocity, velocity dispersion, and velocity offset at l = 0° for the sample are found to be , and —18.2±9.7 km s−1, respectively (80% confidence interval). Furthermore we find trends for the rotation velocity and velocity dispersion to decrease with distance from the galactic plane. These trends are supported by a larger sample constructed by incorporating other available velocity data on the Bulge IRAS sources. The rotation velocity and velocity dispersion are expressed as 15.6—1.23x|b(deg)| km s−1 deg−1 and 101−3.6x |b(deg)| km s−1, respectively. The implications of the observed quantities are discussed.
Kinematics of the Galactic Bulge: the velocity ellipsoid
Authors: Minniti Dante
Published: June 2019

We investigate the shape of the velocity ellipsoid in the Galactic bulge by combining radial velocities and proper motions. We find that the velocity ellipsoid is nearly isotropic.
Star clusters as tracers of galactic subsystems
Authors: Barbuy B. , Bica E. , Ortolani S.
Published: June 2019

We have obtained CCD BVRI colour-magnitude diagrams for a series of disk globular clusters, improving parameters and detecting a new one: Lyngå 7. Using the magnitude difference between turn-off and horizontal branch Δ(TO-HB) as an age discriminator, and their spatial distribution we compare old disk open clusters, young halo globular clusters, and metal-rich disk globular clusters, obtaining clues to the Galaxy formation process.
Dynamics of OH/IR Stars in the Inner Galactic Bulge
Authors: Winnberg Anders , Lindqvist Michael , Habing Harm J.
Published: June 2019

Using the VLA at 1612 MHz Lindqvist et al. (1992a) have found 134 OH/IR stars close to the Galactic Centre (GC). These stars plus 15 from Habing et al. (1983) have been used as probes of the gravitational potential to derive the mass distribution in the inner galactic bulge between ≈ 5 to ≈ 100 pc from the GC (Lindqvist et al., 1992b). In this paper we present a progress report of a dynamical model which we have applied to the data.
Point-axial mass distribution in the external Galactic Bulge
Authors: Sanz-Subirana J. , Juan-Zornoza J.M.
Published: June 2019

The main purpose in this work is to present some analytical results about the spatial distribution of the stars in the Galactic Bulge. These results have been obtained by considering that the stellar system verifies the collisionless Boltzman equation and the ellipsoidal hypothesis (non-axisymmetrical) for the distribution of peculiar velocities of the stars.
Measurements of Interstellar Extinction
Authors: Massa D. , Savage Blair D.
Published: June 2019

The results of interstellar extinction measurements from the near IR to the far-UV are reviewed. The average interstellar extinction curve for the diffuse cloud medium exhibits a nearly linear rise (in 1/λ) from 1 μm−1 to the 2.25 μm−1 “knee” in extinction where the slope changes. In the UV there is a pronounced extinction bump near 4.6 μm−1 (2175 å) followed by a broad minimum and a steep rise in extinction to the shortest wavelengths for which measurements exist. For wavelengths shortward of about 5500 å, the interstellar extinction curve exhibits considerable variation in shape from one sight line to another. In addition to strength variations, the width (FWHM) of the 2175 å extinction bump has been observed to vary by more than a factor of two from 360 to 770 å with the average width being 480 å. In contrast, the central position of the feature only varies from 2110 å to 2195 å with the average central position being 2175 å. The most extreme variations in extinction are found at far-UV wavelengths where E(λ – V)/E(B – V) has been found to range from 3 to 12.5 at 1250 A. In the last few years significant progress has been made in determining various empirical relationships among extinction parameters in the different wavelength regimes and in determining how extinction curve shape changes are influenced by the interstellar environment in which the dust resides. Those relationships are discussed.