bluuebunny/crossref_metadata_2025_split huggingface dataset:
The New Canadian Declaration of Acceptance of the Compulsory Jurisdiction of the International Court of Justice
Authors: MacDonald R. St. J. 
Published: June 2019

On April 8, 1970, Prime Minister Pierre Elliott Trudeau informed the members of the Canadian House of Commons that the federal government had given notice of its intention to introduce two bills dealing with the protection of Canada’s marine environment and the living resources of the sea. He then made the following statement:I wish now to table a copy of a letter which Canada’s Ambassador to the United Nations has delivered to the Secretary General submitting a new reservation to Canada’s acceptance of the compulsory jurisdiction of the International Court of Justice. This reservation is intended to guard against any possible litigation of certain features of these two bills.
Canada’s Role in the International Commission for Supervision and Control in Cambodia
Authors: Dai Poeliu 
Published: June 2019

Commenting on canada’s participation in the activities of the International Commission for Supervision and Control in Cambodia, Mr. Paul Martin, the then Secretary of State for External Affairs, stated in the House of Commons on May 27, 1965 as follows:… Canada has been a member of the Commission for almost 11 years under two different Governments. I believe our record on the Commission is one that has commended itself to the people of Asia, and has commended itself to most people in Canada who have looked at this problem objectively. As Secretary of State for External Affairs I say, and I say with pride, that the officers of the Department and the officers of the Department of National Defence who have served on these commissions have rendered to Canada and as well as to the cause of peace, a distinct service.
The Judgment of the International Court of Justice in the Appeal Relating to the Jurisdiction of the ICAO Council
Authors: Fitzgerald Gerald F. 
Published: June 2019

On August 18, 1972, the International Court of Justice delivered its Judgment in the Appeal Relating to the Jurisdiction of the ICAO Council (India v. Pakistan) in which:(a) By thirteen votes to three, it rejected Pakistan’s objections on the question of its competence, and found that it had jurisdiction to entertain India’s appeal from a series of decisions of the ICAO Council which had found that the Council had jurisdiction to entertain the application and complaint made before the Council by Pakistan on March 3, 1971, the details of the application and complaint being given below.(b) By fourteen votes to two, it held the ICAO Council to be competent to entertain the above-mentioned application and complaint.
Canada and the Review of United Nations Peacekeeping Operations
Authors: Dai Poeliu 
Published: June 2019

Although the United Nations has undertaken more than a dozen peacekeeping operations, and Secretary-General Kurt Waldheim has affirmed that “peacekeeping constituted a principal, and perhaps the most vital, function of the UN,” there is no agreement on the definition of the political and jurisdical scope, or any uniform procedural basis, for such peacekeeping operations. As a matter of fact, the term peacekeeping does not even appear in the UN Charter.Most commentators, however, draw a sharp distinction between peacekeeping operations undertaken pursuant to chapter VI of the Charter on pacific settlement of disputes and enforcement action authorized by the Security Council under chapter VII. As one Swedish diplomat explained, peacekeeping operations are essentially voluntary, undertaken at the request or with the consent of the country in whose territory an operation is to take place, and do not impose any obligation on member states in regard to personnel, equipment or logistics.
On Desiderata for Star Catalogs for the Remainder of the Twentieth Century: A Report on Catalog Work Now in Progress at the U.S. Naval Observatory
Authors: Smith Clayton 
Published: June 2019

The results of observations of Southern Reference Stars (SRS) of all participants in the SRS program (1961–1973) have been received at the U.S. Naval Observatory. It is anticipated that compilation of the final SRS catalog of mean positions will be completed by the end of 1984.A supplementary list to the International Reference Star (IRS) catalog is described. It has been selected with a view to improving areal density and distribution in spectral type.A comparison of solutions for equator and equinox corrections and corrections to the assumed elements of the earth's orbit from daytime observations of the Sun, Mercury, and Venus and nighttime observations of Ceres, Pallas, Juno, and Vesta from Six-inch Transit Circle observations made during the W5-50 program (1963–1971) shows that a very significant part of the systematic daytime error has been removed. A problem remains for observations of the Sun, particularly in declination.
The Shape of the Moon
Authors: Runcorn S. K. , Hofmann S. 
Published: June 2019

The determination of the heights of points on the lunar surface by Earth based astronomy using the geometrical librations, although individually of low accuracy, still provides our best method of obtaining the global shape of the Moon. The intrinsic scatter of the results arises from the effects of ‘seeing’ and simple statistical analysis is required to derive valid conclusions about the shape. Baldwin's method of fitting ellipsoidal surfaces to the points on the maria and uplands, separately by the method of least squares proves to be a valuable tool.Analyses of the ACIC points and of the Pic du Midi studies of G. A. Mills show that good first descriptions of the global shape of the Moon for both the maria and uplands are triaxial ellipsoids with their long axes within 10° of the Earth direction, the major axis of the maria being about 1.3 km smaller than that of the uplands. Of particular significance is that the ellipticity of these surfaces is about 2½ times greater than the dynamical ellipticity; thus the non-hydrostatic figure of the Moon is not simply the result of distortion from a uniform Moon during its early history. The angular variation in density within the Moon cannot be simply a phenomena within the crust but must extend to a great depth. Convection could provide an explanation.The departures of the lunar surface from the idealised ellipsoids are also of interest. The circular maria are systematically depressed relative to the maria ellipsoid: can the mascons have adjusted isostatically since their formation? Systematic differences in height between the western and eastern southern uplands are also noted.
On the Interaction Between Tectonic Processes of the Earth and the Moon
Authors: Kozyrev N. A. 
Published: June 2019

At present seismographs are operating on the Moon as well, installed there owing to the successful Apollo missions. However these data are insufficient for detailed statistic investigations. That is why in case of the Moon we are to use indirect indications of its activity, such as the data on transient light phenomena from the catalogues by Miss B. Middlehurst. Among the great number of earthquakes there were chosen only the strong earthquakes (magnitude 6.5) with focuses deeper than 70 km. According to these characteristics 630 earthquakes were selected from 1904 to 1967. In the Middlehurst catalogue during the same period about 370 transient events on the Moon are registrated. A distribution of lunar events on the days of an anomalistic month gives evidence of the influence of the Earth's tidal forces (the Middlehurst effect). It appears that the distribution of earthquakes gives a similar curve. Thus the tidal interaction of the Earth and the Moon establishes certain synchronism in tectonic activity of these planets. The further statistic analysis reveals some more causal relation between the processes of the Earth and the Moon. Strongly pronounced maximum of lunar events is observed with the interval of 2–3 days after the earthquakes and the maximum of earthquakes – with quite the same interval after the lunar events. The peaks of these maxima exceed the mean number of events by a factor 3. The Moon Earth system is the astronomical example of a direct interaction of the processes in the neighbouring celestial bodies.The corresponding experiments, made at the Pulkovo Observatory, confirm the possibility of immediate interactions of irreversible processes due to the change of physical properties of time. Thus we can form a chronology of orogenesis on the Moon judging from the data on the history of the Earth. Tectonic processes of the Earth and the Moon seem to be in such a close interaction as if the Moon were in direct contact with the Earth, i.e. in other words, were its seventh continent. These conclusions give evidence of the extreme importance of regular seismic observations on the Moon.
Luminescence Excitation by Protons and Electrons, Applied to Apollo Lunar Samples
Authors: Geake J. E. , Walker G. , Mills A. A. 
Published: June 2019

A proton accelerator, modified for work on lunar samples, is described; 60 keV protons at about 1 μA cm−2 are used. Luminescence emission spectra in the visible and near IR regions are shown for lunar samples from Apollo 11 and 12, and preliminary results are given for Apollo 14 samples. Lunar samples are compared with terrestrial and meteoritic materials. Plagioclase is found to be the most efficient luminescent material present in the lunar samples, and the activator for its dominant green peak is found to be Mn2+.Apparatus is described for taking colour photographs of the luminescence emission from rock chips under 6 keV electron excitation. Most of the lunar samples investigated show only plagioclase emission, but one breccia shows a wide variety of colours from different luminescent constituents.
Recent Observations and Superluminal Monitoring of the Quasar 3C 395
Authors: Simon R. S. , Johnston K. J. , Spencer J. H. 
Published: June 2019

Until recently, the compact structure in 3C 395 could be described as follows (Simon et al. 1987):
(1)A bright, unresolved, flat spectrum core to the northwest. The core brightened by about 0.4 Jy between 1983.3 and 1985.4, from 0.6 Jy to 1.0 Jy.(2)A moderately resolved component 15.8+/−0.2 mas to the southwest along P.A.I 18o. The position of this component relative to the core has changed by less than 0.2 mas in 6 years and the flux density of this component has remained roughly constant.(3)A component which was moving rapidly away from the core towards component (2) with a proper motion of 0.64+/−0.1 mas yr−1. For 3C 395 (z=0.635), this implies (v/c)∼20c for Ho =100 km/s/Mpc and qo =0.5.
Shock Models of Time Variability and Superluminal Motion in Compact Extragalactic Radio Sources
Authors: Hughes Philip A. , Aller Hugh D. , Aller Margo F. 
Published: June 2019

Following the success of a simple shock model for outbursts in BL Lacertae and 3C 279 (see Aller, Aller & Hughes, this meeting) we have constructed computer codes to study in detail the radiation from shocked, relativistic jets. These codes compute the transfer of synchrotron radiation, accounting for polarized emission and absorption, rotation, and mode conversion for a turbulent collimated flow with one or more shocks propagating parallel to the jet axis. We present results for a flow that evolves adiabatically, with the turbulence represented by a random component to the magnetic field within each computational cell, and with the shocks prescribed analytically following Königl (Phys. Fluids, 23, 1083, 1980). From the evolution of the total and polarized fluxes as a function of frequency, and from the corresponding projection of the source structure on the plane of the sky, we see that this type of model
a.is capable o f explaining the variability of compact radio sources - see Aller, Aller & Hughes, this meeting,b.highlights the care needed when interpreting VLBI maps, in that
i)the component separations are frequency dependent (see Fig. 1)ii)the ‘core’ is not always the brightest component (see Fig. 1)iii)the Doppler boosting factor of the shocked flow is not directly related to the Lorentz factor derived from the apparent superluminal motion of a componentiv)a multiplicity of components can give rise to both apparent contractions and accelerations,c.clearly shows the link between time variability of compact sources and evolving VLBI structure, and suggests that both may be understood in terms of weak shocks that tap a small fraction of a jet's flow energy,d.enables us to probe the physical conditions of the flow and the ambient material.
Earth Rotation from the IRIS Project
Authors: Robertson D. S. , Carter W. E. , Fallon F. W. 
Published: June 2019

Project IRIS (International Radio Interferometric Surveying) was set up under the IAG and COSPAR to provide an operational system that would employ Very-Long-Baseline Interferometry (VLBI) techniques to monitor variations in the rotation of the Earth. Currently the IRIS-A network, with stations at Westford, MA, Ft. Davis, TX, Richmond, FL, and Wettzell, FRG, conducts 24-hour observing sessions every five days to produce determinations of pole position, UT1, and nutation in addition to other parameters of geophysical and astrometric interest. The resulting Earth orientation parameters (EOP) have been shown to have an accuracy of 1 to 2 milliseconds of arc in pole position, and 0.05 to 0.1 milliseconds of time in UT1. In order to observe the relatively large higher frequency variations in UT1, daily 45-minute observing sessions are conducted using the single baseline between Westford and Wettzell. Intercomparison of the UT1 values from the daily and the 5-day series indicates that the accuracy of the daily values is better than 0.1 millisecond of time.The longer term objectives of the IRIS project include improving the monitoring of Earth orientation by increasing the sampling rate and accuracy of the observations. In April, 1987, the IRIS-P network, with stations in Kashima, Japan, Fairbanks, AK, Ft, Davis, TX, and Richmond, FL began monthly 24-hour observing sessions, and a second series of daily UT1 observing sessions was begun using the stations in Richmond and Bologna, Italy. The additional networks will provide redundancy that will improve the reliability of the system and allow the accuracy of the EOP values to be estimated.The IRIS UT1 time series provides, for the first time, sufficient accuracy and temporal resolution to look for the few percent increase in k/C caused by the anelastic response of the mantle. Initial results presented here suggest that improved methods of accounting for the dynamics of the oceans and atmosphere may be required before the intertwined variations in UT1 can be fully separated.
Atmospheric Effects on Earth Rotation and Polar Motion
Authors: Salstein David A. 
Published: June 2019

The variability in the earth's rotation rate not due to known solid body tides is dominated on time scales of about four years and less by variations in global atmospheric angular momentum (M), as derived from the zonal wind distribution. Among features seen in the length of day (Δl.o.d.) record produced by atmospheric forcing are the strong seasonal cycle, quasi-periodic fluctuations around 40–50 days, and an interannual signal forced by a strong Pacific warming event, known as the El Niño. Momentum variations associated with these time scales arise in different latitudinal regions. Furthermore, winds in the stratosphere make a particularly important contribution to seasonal variability.Other related topics discussed here are (i) comparisons of the M series from wind fields produced at different weather centers, (ii) the torques that dynamically link the atmosphere and earth, and (iii) longer-term non-atmospheric effects that can be seen upon removal of the atmospheric signal. An interesting application for climatological purposes is the use of historical earth rotation series as a proxy for atmospheric wind variability prior to the era of upper-air data. Lastly, results pertaining to the role of atmospheric pressure systems in exciting rapid polar motion are presented.
The Mark IIIA Correlator System
Authors: Whitney Alan R. 
Published: June 2019

The Mark IIIA correlator system, developed at Haystack Observatory, is a second-generation version of the original Mark III correlator which adds significant new capabilities, such as double-speed operation, longer integration periods, and improved internal modelling. One Mark IIIA correlator is currently operational at the U.S. Naval Observatory in Washington, D.C., and another is being readied to replace the Mark III correlator at Haystack.The Mark IIIA correlator can simultaneously process up to 10 baselines of 24-MHz BW data from 5 stations. Experiments including more than 5 stations may be processed with multiple passes through the correlator. The architecture of the correlator allows a future expansion to a maximum of 16 stations. Due to a simple modular design and the low cost of required computer-support equipment, expansion is straightforward and relatively economical.Both astronomy and geodetic data processing are supported by the Mark IIIA system, including spectral line and pulsar gating. In addition, recent work has led to support of space-based VLBI observations; this capability was critical in supporting the first successful space-based VLBI astronomy observations between ground-based antennas and an orbiting satellite in August 1986.
Multivariate Statistical Analysis of the Sample of AGN
Authors: Petrosian A. R. , Karapetian M. Sh. 
Published: June 2019

Radio, FIR, spectral and X-ray data by 11 parameters for the AGNs samples of Sy1, Sy1.5, Sy2 types and LINERs are compiled. All samples are processed by the multivariate statistical methods including factor and discriminant analysises. The following results are obtained:
–LINERs by principal factors, determining NLR and the central engine are clearly separated from the Seyfert galaxies.–All types of the Seyfert galaxies in all have the same NLR.–Intermediate Seyfert type is real. These AGNs are much more similar to Sy1 type objects than to Sy2.
Narrow Line Region in NGC 4151 Nucleus
Authors: Pronik V. I. 
Published: June 2019

The well-known correlations of forbidden lines FWHM with the critical density for collisional de-excitation and with the ionization potential mean, that:
i.the noticeable part of forbidden lines emission must arise in a gas of a rather high density n ∼ ncii.the gas velocity, the density and the degree of ionization they all increase toward the centre of the nucleus.
The Dynamics of 47 Tucanae
Authors: Da Costa G. S. , Freeman K. C. 
Published: June 2019

Observations made at Las Campanas Observatory and at the Anglo-Australian Observatory have been used to determine line-of-sight velocities with an average accuracy of 3 kms−1 for 135 member stars in the globular cluster 47 Tucanae. The velocities were derived from cross-correlation techniques applied to 30 A/mm spectra obtained with digital sky-subtracting detectors. The spectra themselves have been used to analyze the cyanogen anomalies on the red giant branch in this cluster (Norris et al., 1984). When combined with the velocities published by the CORAVEL group (Mayor et al., 1983), these observations yield velocities for 212 stars with projected distances from the cluster center ranging from 3 to 68 core radii. After radial binning and analysis these observations yield the following results:(i) The inner parts of the cluster show appreciable differential rotation with a maximum projected rotation velocity of approximately 6 kms−1 in the region 6–18 core radii. However, at larger radii the rotation declines rapidly and is essentially zero for radii greater than 30 core radii. This result is illustrated in Figure 1. To within the errors of the determinations, the position angle of the maximum rotation and that of the major axis of the stellar density distribution coincide.(ii) In contrast to M3 (Gunn and Griffin 1979), “thermal equilibrium” multimass models (c.f. Da Costa and Freeman 1976) can ONLY reproduce the observed velocity dispersion values by including a substantial amount of “dark matter”; i.e. unlike M3, there is “missing mass” in 47 Tuc. In order to retain a fit to the surface brightness profile of the cluster, this “dark mass” (which provides perhaps 30 to 40 percent of the total cluster mass) cannot have a distribution much different from that of the cluster giants if it is in the form of stars and “thermal equilibrium” is maintained. In this case the obvious candidates for the dark matter are the white dwarf remnants of the stars more massive than the current turnoff mass, though many more such remnants are required than the number expected from extrapolating the present mass function. The difference between M3 and 47 Tuc in this case then implies that the 47 Tuc initial mass function had many more massive stars than did that for M3. The work of Freeman (1977), who demonstrated large IMF variations in the 8 − 1.5 solar mass range in young Magellanic Cloud clusters, provides observational support for this interpretation.
An attempt to determine the structure of the solar core from observed g-mode frequencies
Authors: Kosovichev A.G. 
Published: June 2019

The purpose of this investigation is to estimate how well the structure of the solar core might be inferred by inverting g-mode frequencies.Delache and Scherrer (1983), Isaak et al. (1984), Severny et al. (1984) reported detection and identification of solar g modes. Although the results seem not to be complete it is helpful to invert the available data in order to understand what new information on the structure of the solar core can be obtained from g-mode frequencies.
Spherically Symmetric Kinematic Modelling of Planetary Nebulae
Authors: Diesch C. , Grewing M. 
Published: June 2019

High resolution two-dimensional long slit spectra of NGC 7009, NGC 3242, IC 2448 and TC 1 in the Hα(6565 Å), OIII(5007 Å) and NII(6584 Å) emission lines have been used as input to determine radial velocity gradients in PNe by fitting calculated high resolution spatially resolved spectral structures of single emission lines. Contributions to the Doppler structure of emission lines taken into account are the global expansion of the PN shell and thermal line broadening due to temperatures of some 104 K. This model is based on two parametrized empirically chosen spherical symmetric functions:
1.A empirical two parameter density function ρ(r).2.A linear radial velocity component function ν(r).
The detection of new methanol masers in the 5−1 — 40E Line
Authors: Kalenskii Sergei V. , Slysh Vyacheslav I. , Val'tts Irina E. , Winnberg Anders , Johansson Lars E. B. 
Published: June 2019

Fifty-one objects in the 5−1 − 40E methanol line at 84.5 GHz was detected during a survey of Class I maser sources. Narrow maser features were found in 17 of these. Broad quasi-thermal lines were detected towards other sources. One of the objects with narrow features, the young bipolar outflow L 1157 was also observed in the 80 − 71A+ line at 95.2 GHz; a narrow line was detected at this frequency. Analysis showed that the broad lines are usually inverted. The quasi-thermal profiles imply that the line opacities are not larger than several units. These results confirm the plausibility of models in which compact Class I masers appear in extended sources as a result of an appropriate velocity field.Measurements of linear polarization at 84.5 GHz in 13 sources were made. No polarization was found except a tentative detection of a weak polarization in M 8E.