bluuebunny/crossref_metadata_2025_split huggingface dataset:
“Nations Like Unto Yourselves”: An Inquiry into the Status of a General Principle of International Law on Animal Welfare
Authors: Sykes Katie 
Published: June 2019

SummaryThis article proposes that there is a general principle of international law concerning the humane treatment of animals. Preoccupation with “animal rights” has been associated with Western cultural imperialism masquerading as a universal ethic. Animal welfare is thus an instructive case study of what Jutta Brunnée and Stephen Toope have identified as the key challenge for international law, that of “construct[ing] normative institutions while admitting and upholding the diversity of peoples in international society.” This article applies the framework of interactional international law set out in Brunnée and Toope’s recent bookLegitimacy and Legality in International Law, while raising questions about the weight that their analysis accords to practice and their willingness to conclude that widely recognized principles to which states fail to adhere in practice lack legal force. The article also examines how laws prohibiting cruelty to animals have emerged precisely from an interactive cultural exchange between East and West, in particular, between England and India. It concludes that Brunnée and Toope’s framework, although it does not deal at any length with general principles of law (a source of international law in which practice plays a relatively minor role), is nevertheless a useful tool for understanding how a culturally contested principle fits into international law and ultimately supports the view that there is a general principle of international law concerning animal welfare.
Contribution of PAHs to the Interstellar Extinction Curve
Authors: Joblin C. , Leger A. , Martin P. , Defourneau D. 
Published: June 2019

Absorption spectra of some gaseous PAHs, either pure species or natural mixtures, have been obtained in the VUV-visible region and compared to the interstellar extinction curve.The assumption that free PAHs are ubiquitous in the ISM cannot be rejected by incompatibility between the interstellar extinction curve and the absorption spectra of such molecules. PAHs absorb in the FUV rise and may give an important contribution to the bump at 2200 Å. We have derived that about 15% of the cosmic carbon is involved in these molecules.
Dynamics of the Moon
Authors: Jeffreys Sir Harold 
Published: June 2019

Koziel's results on the librations have been rediscussed. Some serious departures from independence of the errors were detected and have been allowed for. The results areβ = 0.0006271 ± 0.0000010γ = 0.0002362 ± 0.0000082These do not differ much from Koziel's values but the uncertainties are larger. Both are consistent with results previously derived by comparison of results of different authors, and γ is consistent with a reinterpretation of a result of Yakovkin.The effect of elasticity is considered. It is shown that the elastic strain does not contribute to the librations but would affect the perturbations of a satellite. Allowance for this difference reduces Michael's estimate of 0.4015 for C/Ma2 to 0.4001 ± 0.0030, which would be consistent with either uniform density or with the value I found in 1936 after allowance for compressibility and a possible thin surface layer, namely 0.3971 ± 0.0007.
The Geomorphic Evolution of the Lunar Surface
Authors: Ronca L. B. 
Published: June 2019

Fundamental parameters of the geomorphology of a lunar surface are (i) the number and size distribution of craters, (ii) the degree of erosion of the craters and (iii) thickness and other characteristics of the regolith. These parameters are not independent of one another; as one changes through time, the other two will also change in a statistically predictable way.In the continuous degradation sequence, the relationship between the number of craters per unit area and the degree of erosion of the craters is continuous and monotonic. This sequence occurs in areas subjected to intermediate to small impacts, and eroded mainly by the impacts themselves plus other small-scale erosional processes. In areas subjected to large impacts and mare flooding the discontinuous degradation sequence is predominant.The relationship of the first two parameters, the number of craters and the degree of erosion, with the third parameter, the regolith, is not simple and is not yet understood. It appears, however, that the geomorphological stage is more important than the mare-versus-highland dichotomy of the lunar surface.The solution of the function relating craters of the continuous degradation sequence with degree of erosion was defined as the geomorphic index of the area. Studies of the geomorphic index of stratigraphic surfaces show that areas covered by considerable ballistic sediments have a geomorphic index which is not a monotonic function of time. On the other hand, areas covered almost exclusively by mare flooding show an index which is a monotonic function of the age of the flooding. As each mare surface shows a considerable range in indices, it is concluded that maria are covered by surfaces formed through a considerable length of time. By using Apollo 11 and 12 radiometric ages it is suggested that the time of mare flooding lasted on the order of one billion (109) years.The geomorphic index of highland surfaces shows a remarkable degree of order; i.e., the farther an area is inland from the mare shores, the higher will be the index. No explanation is given to this phenomenon, but is suggested that lunar erosion is not just a localized phenomenon centered on the locus of an impact, but has lateral trends of regional dimensions. Electrostatic transportation as suggested by Gold is a possible mechanism.
Introductory Remarks: The Apollo 14 Mission
Authors: Newell Homer E. 
Published: June 2019

To set the context of our current exploration of the Moon, it is well to recall: Apollo 11 landed near the equator and was capable of affording the astronauts only a few hours on the lunar surface; Apollo 12 checked out pin-point landing which then permitted going to more difficult, nonequatorial sites; in Apollo 14 enlarged propellant tanks permitted some 42 kg of samples to be brought back. Three more Apollo missions follow Apollo 14. The Apollo missions, complemented by unmanned missions to the various planets, form a program to explore the solar system.Captain Scherer will elaborate on the significant increase in Apollo capability in the last three missions. Of note are the lunar heat flow experiments, the lunar surface gravimeter, and, for Apollo 15, the laser ranging retroreflector which will be three times the area of and four times as efficient as retroreflectors in the previous Apollo missions. In the lunar orbital equipment will be the sub-satellite with instruments for measuring various physical properties of the Moon and its environment. Also noteworthy is the lunar sounder, for Apollo 17, which will use radar for probing a large fraction of the lunar surface to considerable depth.Hardware changes will allow the astronauts to remain on the lunar surface for up to 66 hrs – an increase of 100%; thus the landed scientific payload may be doubled to approximately 550 kg. Increased range and efficiency of surface operations will result from improved suit mobility, an improved life support system, and a Lunar Roving Vehicle capable of up to 90 km traverses. Changes in the Command and Service Modules will allow for up to 16 days total flight duration.We will again welcome proposals for analysis of the new samples, but now that the initial exploratory work has been done we intend to be far less duplicative in choosing proposals to support. We are particularly pleased with the growing attention being given by the scientific societies to the results of lunar research.In the last talk of this series, Mr. Burke will describe some of the future possibilities that have been studied for exploration of the Moon and planets. We will particularly welcome suggestions as to how to improve the value of future missions.
Petrochemistry and Chemical Features of Lunar Glassy Spherules
Authors: Trigila R. 
Published: June 2019

The major elements of glassy spherules from samples 12001.73, 12057.60 and 12070.37 of lunar fines have been determined by electron probe analysis. The bulk chemistry of these spherules (which are between 200 μm and 62 μm in size) falls in most cases within the range of gabbro-peridotite and gabbro-anorthosite.In individual spherules, the grade of chemical homogeneity is highly variable and can be related to the possible presence of small inclusions or sometimes to slight concentration gradients evident near the peripheries of the particles. These features, together with the presence of vesicles of different size in association with strong alkali enrichment along the boundaries of such cavities can account for relationships between the chemistry of the particles and their genetic history.
The UV and optical reddening law to the Galactic Bulge and CNO abundances in Bulge planetary nebulae
Authors: Walton N.A. , Barlow M.J. , Clegg R.E.S. 
Published: June 2019

An analysis of the differential ultraviolet extinction towards four bulge planetary nebulae, based on the observed line ratio of He II 1640/4686Å, shows that the ultraviolet reddening law towards the bulge is much steeper than in the solar neighbourhood. An analysis of the optical reddening law for 42 bulge PN, based upon observed Balmer line ratios and Hβ to radio free-free flux ratios, is presented. The optical reddening law towards the bulge is steeper than in the local ISM, and thus the ratio of total to selective extinction, Rv = 2.29 (± 0.50), is lower than the standard solar neighbourhood value of Rv = 3.10.We present abundance determinations, in particular C/H and C/O ratios, for 11 Galactic bulge PN, based on spectrophotometry in the UV from IUE and in the optical from the Anglo-Australian Telescope. The derived abundances are compared with values for PN in the Galactic disk. The mean C/O ratio for bulge PN is significantly lower than that found for Galactic disk PNs. Additionally we present an abundance analysis of the very metal-poor halo population PN M2-29, which is located in the bulge.
Celestial Reference Frames: Definitions and Accuracies
Authors: Standish E M 
Published: June 2019

The determination of a specific catalogue or ephemeris reference frame is a highly over-determined problem, depending on the particular selection of which coordinates, which objects and at what time(s) the determination is made. The consistency which various determinations exhibit is dependent upon the accuracy of the catalogue or ephemeris itself. This paper discusses the accuracies of the three most prominent celestial reference frames: stellar catalogues, the lunar and planetary ephemerides and the radio source catalogues.The FK4 stellar catalogue contains known systematic errors amounting to a few tenths of an arcsecond; the FK5 will yield nearly an order of magnitude improvement; HIPPARCOS and Space Telescope expectby the mid 1990's optical interferometry should approachwithin a couple of years, tens of micro(!)arcseconds after a couple of decades. Present-day lunar and planetary ephemerides have accuracies at the level offor the moon and inner four planets;for the outer planets. Further observational data will permit continued improvement. Radio source catalogues now show internal consistency of
The Second Byurakan Spectral Sky Survey, Quasistellar Objects and Seyfert Galaxies
Authors: Stepanian J.A. , Erastova L.K. , Lipovetsky V.A. , Shapovalova A.I. 
Published: June 2019

Survey of surveys, and the place of the Second Byurakan Survey (SBS) among them is shortly discussed. Deep low-dispersion surveys cover > 10000 sq.degrees, but they managed to study only 15% of this area relatively well.For 450 SBS objects the slit spectra were obtained on 6 m telescope of SAO. The nature of 120 QS0s,40 Sy galaxies and more than 200 ELG are confirmed. The results of the slit spectroscopy in six SBS fields covering commonly the area of ∼100 sq.degrees are presented.All surveys, except Byurakan Surveys are extremely poor with Sy galaxies, that is their distinction from other surveys. Weak (16<m<18m5) SBS Sy galaxies sufficiently well filled in the interval between QSOs and Sy galaxies, the efficiency of selection does not much depend on redshifts. There is quite good pass from Sy galaxies to QSOs.
Numerical Simulations of Encounters of Hard Binaries
Authors: Mikkola Seppo 
Published: June 2019

Results from numerical integrations of random binary-binary encounters have been used to obtain various cross-sections and outcome distributions for the four-body scattering. The initial orbital elements were chosen randomly except the Kepler-energies for which various selected values were used. Rough estimates for mass effects were obtained by simulating encounters of binaries with unequal component masses.We developed a semi-analytical theory for obtaining the types and energies of the outcome configurations. The theory contains some adjustable parameters, the values of which we deduced by comparing the theory and experiments.The energy transfer rate by collisions (=outcome is not two binaries) dominates over that due to fly-by's by an order of magnitude, provided that the binaries are hard. The formation of a hierarchical three-body system is fairly common. In a collision of energetically similar very hard binaries the probability is about 20 percent, while it is greater than 50 percent if the binding energies differ by a factor of more than four.
Monte Carlo Simulations of the 2+1 Dimensional Fokker-Planck Equation: Spherical Star Clusters Containing Massive, Central Black Holes
Authors: Shapiro Stuart L. 
Published: June 2019

The dynamical behavior of a relaxed star cluster containing a massive, central black hole poses a challenging problem for the theorist and intriguing possibilities for the observer. The historical development of the subject is sketched and the salient features of the physical solution and its observational consequences are summarized.The full dynamical problem of a relaxed, self-gravitating, large N-body system containing a massive central black hole has all the necessary ingredients to excite the most dispassionate many-body, computational physicist: it is a time-dependent, multidimensional, nonlinear problem which must be solved over widely disparate length and time scales simultaneously. The problem has been tackled at various levels of approximation over the years. A new 2+1 dimensional Monte Carlo simulation code has been developed in appreciable generality to solve the time-dependent Fokker-Planck equation in E-J space for this problem. The code incorporates such features as (1) a particle “cloning and renormalization” scheme to provide a statistically reliable population of test particles in low density regions of phase space and (2) a time-step “adjustment” algorithm to ensure integration on local relaxation timescales without having to follow typical particles on orbital trajectories. However, critical regions in phase space (e.g. disruption “loss-cone” trajectories) can still be followed on orbital timescales. Numerical results obtained with this Monte Carlo scheme for the dynamical structure and evolution of globular star clusters and dense galactic nuclei containing massive black holes are reviewed.Recent dynamical integrations of the Einstein field equations for spherical, collisionless (Vlasov) systems in General Relativity suggest a possible origin for the supermassive black holes believed to power quasars and active galactic nuclei. This scenario is discussed briefly.
The precision of modern theories of Galilean satellites as derived with their comparison with photographic observations made with the 26″ refractor at Pulkovo Observatory
Authors: Kisseleva T. P. , Glebova N. I. , Malkova A. G. 
Published: June 2019

The regular photographic observations of Galilean satellites has been made with 26″ refractor at Pulkovo since 1975. The relative positions of satellites are obtained by means of “scaletrail” technique. During 1975–1979 over 600 observations of Galilean satellites were carried out. The observed positions were compared with the ephemeris based on Sampson's and Lieske's E-1 theories, the corresponding computations being made at the Institute for Theoretical Astronomy. The standard deviations of one observed relative position “Satellite minus Jupiter” don't exceed ±0″.10. The comparison of Sampson's theory with observations showed some systematic error which can be considered as an error in longitude of about 1 min. Lieske's theory E-1 showed a better agreement with the observations, the absolute deviations not exceeding 0″.3.A construction of highly precision theories of motion of planet's satellites and of Galilean satellites, in particular, demands appropriately accurate observations (the error not exceeding 0″.10). At present such observations of satellites can be obtained with the help of long-foci telescopes (focal length of about 10 m), using rigorous technique of astrometric reduction.
Extended X-Ray Emission from Early-Type Galaxies: Comparison with Optical
Authors: Trinchieri G. , Fabbiano G. 
Published: June 2019

In this poster we display the results from a detailed analysis of the distribution of the X-ray emission in early type galaxies. Two major results have come out of the analysis so far:
a)The surface brightness radial profiles of isolated elliptical and SO galaxies are smoothly decreasing functions of radius out to a Rmax (similar to the optical radius). Outside Rmax a flattening in the slope is observed, although the exact shape of the profiles at large radii, where the data are poorest, cannot be determined at present.b)For R«Rmax, the X-ray and optical surface brightness profiles are similar (the nuclear region could be an exception). At larger radii, the X-ray profile could be flatter (NGC 4649 and NGC 4472 northern sector) or steeper (NGC 4472 southern sector) than the optical profile, or have a similar shape (NGC 4636).It is likely that the different profiles reflect the action of slightly different environments and/or a different ambient density around each galaxy, combined with the “history” of each galaxy. The tail in NGC 4472 could be the result of the motion of this galaxy in a dense intracluster medium. The X-ray deficiency in NGC 4649 could be due to either ram pressure stripping or the action of wind in the outer regions of the galaxy.
Detecting Cold Dark Matter Candidates
Authors: Drukier A. K. , Freese K. , Spergel D. N. 
Published: June 2019

We consider the use of superheated superconducting colloids as detectors of weakly interacting galactic halo candidate particles (e.g. photinos, massive neutrinos, and scalar neutrinos). These low temperature detectors are sensitive to the deposition of a few hundreds of eV's. The recoil of a dark matter particle off of a superheated superconducting grain in the detector causes the grain to make a transition to the normal state. Their low energy threshold makes this class of detectors ideal for detecting massive weakly interacting halo particles.We discuss realistic models for the detector and for the galactic halo. We show that the expected count rate (≈103 count/day for scalar and massive neutrinos) exceeds the expected background by several orders of magnitude. For photinos, we expect ≈1 count/day, more than 100 times the predicted background rate. We find that if the detector temperature is maintained at 50 mK and the system noise is reduced below 5 × 10−4 flux quanta, particles with mass as low as 2 GeV can be detected. We show that the earth's motion around the Sun can produce a significant annual modulation in the signal.
Several Statistical Properties of Galaxies with UV Excess
Authors: Kazarian M.A. 
Published: June 2019

The number of galaxies with UV excess relative to normal galaxies is determined and other statistical characteristics of galaxies with UV excess are also presented.V.A. Ambartsumian's idea of the activity of galaxy nuclei, suggested 30 years ago, has played a great role in the development of extragalactic astronomy. He showed that the evolution of galaxies depended on the activity of their nuclei. According to Ambartsumian (1958) the nuclei of galaxies are active if explosions take place in them. These explosions lead to large radio fluxes and in general to the wide range of phenomena normally associated with nuclear activity.The spectra of active galaxies show ultraviolet (UV) excess and emission lines of hydrogen and other elements. In other words, the UV excess and emission lines which are observed in the spectra of galaxies are the consequence of active processes.
An extremely high ‘Q’ueue value applied to seismological meetings
Authors:   Anonymous (perhaps Hunger and Tooth)
Published: June 2019

Recent observations of the mysterious astronomical body IAU 123 indicate that the ‘Q’ueue value for astronomy symposia can approach 100–120, with very rapid growth and slow exponential decay. Number density fluctuations, with a frequency of 11.56 μHz and extreme phase coherence have been detected outside the main cafeteria. The long period and high ‘Q’ suggest that this may be represented by a g-mode of low radial order.A stabilized Fabry-Perot etalon has been used to measure the low-level motions, with propagation velocities of order 0.01 cm s−1. Although this is well below the local Alfvén speed, there can still arise significant shock effects (e.g. upon discovery of liver loaf as the main course).The observed cafeteria oscillation spectrum is still incomplete. For instance, if ice cream were offered at the end of the line, we would expect to detect the well-known ‘a la’-mode predicted by Baskin and Robbins.We hope that future studies of astronomical Q's may lead to a better understanding of solar-type astronomers' resonant cavities.
The Molecular Features in the Optical Spectra of the Proto-Planetary Nebulae
Authors: Hu J.Y. 
Published: June 2019

An AGB star evolves into the proto-planetary nebula(PPN) phase, when the stellar surface temperature is hotter than 5000K(Schonberner, 1983). But the remnant of AGB dust/gas envelope is still thick in the early stages of PPN evolution. The observed optical spectrum of PPN is a spectrum of central star(T∗ hotter than 5000K, the spectral type earlier than G5) overlaped with molecular features formed by molecules in the envelope. The features are changing during the envelope turns to optical thin. Based on our systematic observations of IRAS selected PPN candidates(Hu et al. 1990) we found that molecular features in the spectra evolve as following:
1.When object just exposes from dust shell, the column density of molecules in the envelope is very high. The molecular absorption bands are dominant in the spectra, which are resemble to the M supergiant. There are 6 objects from our 62 PPN candidates sample in this stage.2.When column density of molecules decreases, the spectra mainly show F-(or G-)type supergiant features from photosphere and partly also from envelope (especially the neutral atomic lines). But we still can detect the molecular bands such as C2, CN in the spectra of carbon-rich objects(3 objects in our sample, IRAS23304+6147, 20000+3239 and 19477+2401), TiO of oxygenrich object(one object, IRAS20406+2953), and ZrO and LaO of S-type transit object(one object, IRAS19454+2920).3.The evelope becomes optical thin and molecules absorb photons from central star then radiate by fluorescence process. In the spectrum apear the molecular emission bands resemble to the cometary spectra. A well known object in which spectrum C2 Swan bands in emission is CRL 2688(Crampton et al. 1975). We found another object, IRAS14429-4539, in the sample showing similar features.