bluuebunny/crossref_metadata_2025 huggingface dataset:
Torsion of elliptical composite beams with auxetic phase
Authors: Strek Tomasz , Jopek Hubert , Fraska Agnieszka
Published: March 2016

The torsion of a prismatic beam has been a classic problem of structural mechanics since the famous works of Saint‐Venant. In this paper, an analysis is extended on a composite beam with elliptical cross‐section. We consider a beam in which the elliptical cross‐section is split into sectors in which two materials, one of which is auxetic, are distributed alternately. The influence of auxetic phase on the total elastic strain energy is analyzed as well as geometrical parameters representing both the shape of the cross‐section, and the arrangements of sectors. An unexpected behavior of a beam with strong auxetic phase is presented as, in the case of selected parameters, the beam with elliptical cross‐section is more rigid than the beam with a circular one.
Analysis of the thermal and temporal stability of Ta and Ti thin films onto SAW–substrate materials (LiNbO3 and LiTaO3) using AR‐XPS
Authors: Vogel U. , Gemming T. , Eckert J. , Oswald S.
Published: March 2016

Modern surface‐acoustic‐wave devices are characterised by their trend to higher frequencies, power densities, and new applications. For this, a shrinking of the dimensions is necessary but hardly possible to achieve with standard Al‐based metallisation because of increased stress‐induced damaging (acoustomigration). In this context additional barrier interlayers between substrates and electrodes are necessary, especially for high‐temperature applications. For this, we present results of a detailed chemical interface analysis of deposited Ta and Ti thin‐film growth onto surface acoustic wave–substrate materials (LiNbO3 and LiTaO3) with respect to their interface layer structure and its temporal and thermal stability in vacuum. The analysis was mainly performed using non‐destructive and surface sensitive angle‐resolved X‐ray photoelectron spectroscopy. Besides a slight oxidation (oxygen adsorption) at the surface of these highly reactive metal thin films all interface sequences are stable up to 24 h. We also report higher thermal stability of Ta thin films up to 600 °C in contrast to Ti thin films (300 °C) because of presumed diffusion of Ti along grain boundaries. Copyright © 2016 John Wiley & Sons, Ltd.
Addressing biodiversity impacts of land use in life cycle assessment of forest biomass harvesting
Authors: Gaudreault Caroline , Wigley T. Bently , Margni Manuele , Verschuyl Jake , Vice Kirsten , Titus Brian
Published: March 2016

Forests are an increasingly important source of feedstock for bioenergy as global efforts to mitigate atmospheric CO2
concentrations increase. In keeping with the principles of sustainable forest management, it is important that feedstock procurement not have negative impacts on the environment, including biodiversity. Impacts of land use, including forest management, can be evaluated along all stages in the production of these goods and services, using life cycle assessment (LCA), which is a potentially powerful tool for organizing and evaluating the impacts of production. There is growing recognition of the need to integrate land‐use impacts into LCA for forest products such as bioenergy, especially on biodiversity. Integrating quantitative indicators of biodiversity into LCAs of biomass production systems is particularly challenging because biodiversity is a multidimensional concept that can never be fully represented by a single number, and yet many proposed approaches rely on this. Reliance on a single metric oversimplifies ‘biodiversity’ and might lead to inappropriate conclusions on local land management practices. LCA is not suited to providing reliable site‐specific assessment of forest product systems in regard to the complexities of biodiversity. Nevertheless, the global and comprehensive nature of LCA makes it a useful tool for preventing a shift in environmental problems or burdens across the value chain because of local land management decisions. In this context, complementary site‐specific and/or regional studies or analyses may help mitigate against inaccurate conclusions being drawn from LCA. WIREs Energy Environ 2016, 5:670–683. doi: 10.1002/wene.211

This article is categorized under:

Bioenergy > Climate and Environment

Energy and Development > Climate and Environment
“MOORS KNOW THE LAW”: SOVEREIGN LEGAL DISCOURSE IN MOORISH SCIENCE RELIGIOUS COMMUNITIES AND THE HERMENEUTICS OF SUPERSESSION
Authors: Dew Spencer
Published: March 2016

Among the many individuals and groups espousing affiliation with the Moorish Science Temple of America movement, some continue founding prophet Noble Drew Ali's emphasis on engaging in American citizenship as a religious duty, while others interpret the prophet's scriptures to lend authority to claims of being outside the jurisdiction of American legal authority. Such sovereign Moors, whose actions range from declaration of secession to rejection of drivers or marriage licenses, advance legal discourse rooted in historical narratives, tailor their legal thinking toward practical instruction and efficacious results, and appeal to etymology to further authorize their claims. Such sovereign Moorish legal discourse is best understood, following Catherine Wessinger's work on the Montana Freemen, as “magical,” and understanding the magical role played by legal texts and discourse within these communities can help scholars and legal professionals in their approach to and interactions with sovereign Moors.
Dissolved Inorganic Radiocarbon in the Northwest Pacific Continental Margin
Authors: Ge Tiantian , Wang Xuchen , Zhang Jing , Luo Chunle , Xue Yuejun
Published: March 2016

This article presents a modified method for extraction of dissolved inorganic carbon (DIC) from seawater for radiocarbon measurement by accelerator mass spectrometry (AMS). Standard tests indicate that the extraction efficiencies of DIC are >96%, and the respective precisions of Δ14C-DIC and δ13C-DIC analyses are 6‰ and 0.1‰ or better. Using the method, we report Δ14C-DIC profiles collected from the shelf and slope in the East China Sea (ECS) of the northwest Pacific Ocean. Both the DIC concentration and Δ14C-DIC in the shelf and slope regions seem primarily affected by the Kuroshio Current. It is estimated that 54–65% of the bottom water in the shelf region could be from the intrusion of Kuroshio intermediate water, which carries a high concentration and low Δ14C values of DIC, and which influenced the DIC and its 14C signature on the shelf. Compared with the Δ14C-DIC profiles at other sites in the northwest Pacific reported previously, it appears that the Δ14C-DIC distributions are mainly controlled by the major oceanic currents in the region, and large variations in Δ14C-DIC occurred mostly in the upper 800 m of the water column. The similarity of Δ14C-DIC at depth suggests that the deep-water circulation patterns have been relatively stable in the northwest Pacific Ocean in the last 20 yr.
LUCIAN ON THE TEMPLE AT HELIOPOLIS
Authors: Kaizer Ted
Published: March 2016

This paper focusses on two lines in what counts as our best available literary source for the study of religious life in the Roman Near East. In paragraph 5 of Περὶ τῆς Συρίης Θεοῦ (On the Syrian Goddess), a treatise professing to describe the temple and cult at Hierapolis, a place in northern Syria also known by its indigenous names of Manbog or Bambyce, the author writes:

ἔχουσι δὲ καὶ ἄλλο Φοίνικες ἱρόν, οὐκ Ἀσσύριον ἀλλ’ Αἰγύπτιον, τὸ ἐξ Ἡλίου πόλιος ἐς τὴν Φοινίκην ἀπίκετο. ἐγὼ μέν μιν οὐκ ὄπωπα, μέγα δὲ καὶ τόδε καὶ ἀρχαῖόν ἐστιν.

The Phoenicians have another temple, not Assyrian, but Egyptian, which came to Phoenicia from Heliopolis. I have not seen it, but it too is large and ancient.
EPICURUS AND THE IUVENIS AT VIRGIL'S ECLOGUE 1.42
Authors: Bing Peter
Published: March 2016

‘But tell us, Tityrus, who is that god?’ (sed tamen, iste deus qui sit, da, Tityre, nobis). This is what the herdsman Meliboeus asks in Virgil's first Eclogue (Ecl. 1.18) in response to Tityrus' assertion that a certain deity granted him the leisure to sing and to pasture his herd (o Meliboee, deus nobis haec otia fecit. | namque erit ille mihi semper deus, Ecl. 1.6–7). In posing this question, the herdsman raises the issue of this god's identity also for us, Virgil's readers. We are invited to ponder ‘Who is that deus?’ The question lingers, hanging over the text for the next twenty-three verses, without answer. For despite Meliboeus' blunt and plainspoken query (qui sit, da … nobis), which demands a concrete response, Tityrus—on finally returning to the question qui sit—pointedly names no names. Rather, he leaves his divinity anonymous. We learn only that the god is a iuuenis, whom Tityrus saw at Rome, and who answered the herdsman's entreaty (hic illum uidi iuuenem … | hic mihi responsum primus dedit ille petenti, Ecl. 1.42, 44). In honour of this deity, Tityrus' altars smoke with sacrifice every month of the year (quotannis | bis senos cui nostra dies altaria fumant, Ecl. 1.42–3). As the poem takes the form of a dramatic dialogue without narrative frame, no authoritative voice intervenes to offer further guidance as to the god's identity. Thus we continue to wonder as to the identity of this divine iuuenis. The question remains open, an incitement to readerly conjecture.
THE STATIUS OF GRONOVIUS (AMSTERDAM, 1653) AND THE MANUSCRIPTS LONDON BL ROYAL 15.C.X AND 15.A.XXI
Authors: Berlincourt Valery
Published: March 2016

The edition of Statius which Johannes Fredericus Gronovius (1611–1671) published in Amsterdam in 1653 is acknowledged as the most significant stage in the evolution of the printed text of the Thebaid before the late nineteenth century. J.B. Hall rightly stresses that, in spite of some blemishes, it is the first edition of Statius' works which ‘shows the application of much thought to the editorial process’ and ‘deserves to be called critical in the fullest sense’. In accordance with contemporary practice, Gronovius aimed not at establishing Statius' text through a reconstruction of the manuscript tradition but, rather, at selectively correcting a printed textus receptus. The prototype used for producing the text of his edition was the text of the edition of Amsterdam 1630 (a reproduction of that of Amsterdam 1624, itself derived from Gevartius' edition of Leiden 1616). Gronovius' text is not beyond reproach, even when judged from the perspective of the textus receptus. The number of passages corrected remains indeed limited. It is, however, higher than in any other printed text between the first Aldine (Venice, 1502) and the edition of Müller (Leipzig, 1870). More importantly, Gronovius' corrections are usually of great value, and many of them promote readings that are still considered correct today. From the disappointingly short commentary (‘gustus’) in which Gronovius discussed a few problematic passages, it can be clearly seen that his corrections relied on solid information and good skills. Although Gronovius' knowledge of the textual transmission of Statius did not compare with Heinsius' knowledge of that of Ovid, his edition stands out, in the tradition of the Thebaid, for the numerous manuscripts it made use of: eleven (at least), as we learn from his commentary.
The “Dulles Doctrine on Love”: Immigration, Gender, and Romance in American Diplomacy, 1956–1957
Authors: M. BLASCHKE ANNE
Published: March 2016

This article explores the gendered potential and limitations of eastern bloc immigration to the United States under Eisenhower and his Secretary of State, John Foster Dulles. When Dulles endorsed the romantic marriage of Czechoslovakian Olympic gold medalist Olga Fikotova to fellow Olympic winner – and American – Harold Connolly in 1957, he engineered a cultural-diplomacy coup that complimented the president's New Look brinkmanship abroad. Feminine, heteronormative, Protestant, and a world champion, Fikotova initially seemed an ideal Cold War immigrant. When she and her new husband arrived on American shores amid media fanfare, though, she exercised her newfound freedom of speech to criticize American social problems and advocate women's equality.
Immigration Forum Comment: Cultural Responses to Immigration
Authors: LEWTHWAITE STEPHANIE
Published: March 2016

In an age when politicians and the mainstream media continue to divide immigrants into deserving and undeserving subjects, making them both hypervisible and yet invisible, the essays by Lauret, Krause and Schreiber are timely and compelling. Together, they map the historical and contemporary processes of state violence, legal erasure and cultural coercion that have shaped immigrant lives and subjectivities. Models of cultural conformity and whiteness, hyphenation, and either/or binaries that enforce the strict separation of old and new, legal and illegal, have affected the immigrant psyche and induced forms of individual and collective trauma, including ethnic shame, madness, family fragmentation and the physical exploitation of human bodies. In their essays on Americanization and Dominican American fiction, Lauret and Krause reveal the less than celebratory narratives that get lost in stories of emancipatory assimilation, ethnic persistence and hyphenated and multiple subjectivities. Likewise, in her essay on contemporary Latino/a music video and undocumented immigration, Schreiber asks us to see what is obscured from view, but also to find room in these new narratives for patterns of immigrant visibility, agency and activism. These essays suggest that immigrant testimony, literature and visual and aural media can be powerfully combined with historical analyses of immigration policy to unravel the complex realities behind the walls of national nostalgia and racial stereotyping. They also suggest alternative ways of seeing that demand we recognize every immigrant's right to humanity and a sense of belonging.
Community at the border or the boundaries of community? The case of EU field diplomats
Authors: Hofius Maren
Published: March 2016

This article contributes to the communities of practice (CoP) literature by focusing on the neglected role of the boundary in constructing community. It takes issue with advocates of International Relations’ (IR) most recent ‘practice turn’ who have overrated inclusive practices of linking to the detriment of taking account of exclusive practices of demarcation. A conceptual turn to the boundary, understood as a ‘site of difference’, highlights how the two sets of practices operate simultaneously in creating shared senses of belonging to a community. The article empirically probes this turn to the boundary by studying how the postmodern community of the European Union (EU) is (re)constructed by EU diplomats in its neighbouring state Ukraine. As a borderland, it symbolises an interstitial zone of high connectivity where the EU’s otherwise latent order is unearthed. A reconstructive analysis of interviews with members of this ‘community of practice’ reveals that they function as ‘boundary workers’ who engage in both boundary-spanning and boundary-drawing practices on an everyday basis. Zooming in on the ‘boundary work’ by EU diplomats exposes the complex process of community-building and thereby helps grasp community as an emergent structure of possibilities whose meaning is contextually mediated by its members’ social experience of the boundary.
Democratic peace and the norms of the public: a multilevel analysis of the relationship between regime type and citizens’ bellicosity, 1981–2008
Authors: Jakobsen Jo , Jakobsen Tor G. , Ekevold Eirin Rande
Published: March 2016

The democratic peace literature has convincingly shown that democracies do not fight other democracies. Theoretical explanations of this empirical phenomenon often claim that the citizenry in democracies prefers peaceful resolution of interstate conflicts. Still, there is a dearth of studies exploring the public’s preferences and values directly. We seek to rectify this by investigating, in a novel way, the relationship between regime type and citizens’ bellicosity. A comprehensive multilevel research design is employed, with data spanning 72 countries over the period of 1981–2008. This enables us to test one of the theoretical mainstays of the democratic peace thesis, viz., that regime type helps shape individuals’ attitudes toward war-fighting. Our results lend special support to normative democratic peace theory: Citizens of democracies are significantly more pacifistic than citizens of non-democracies. This result upholds when we rigorously control for other relevant factors, including specific characteristics of individuals and rival theoretical explanations.
Data mining for building knowledge bases: techniques, architectures and applications
Authors: Krzywicki Alfred , Wobcke Wayne , Bain Michael , Calvo Martinez John , Compton Paul
Published: March 2016

Data mining techniques for extracting knowledge from text have been applied extensively to applications including question answering, document summarisation, event extraction and trend monitoring. However, current methods have mainly been tested on small-scale customised data sets for specific purposes. The availability of large volumes of data and high-velocity data streams (such as social media feeds) motivates the need to automatically extract knowledge from such data sources and to generalise existing approaches to more practical applications. Recently, several architectures have been proposed for what we callknowledge mining: integrating data mining for knowledge extraction from unstructured text (possibly making use of a knowledge base), and at the same time, consistently incorporating this new information into the knowledge base. After describing a number of existing knowledge mining systems, we review the state-of-the-art literature on both current text mining methods (emphasising stream mining) and techniques for the construction and maintenance of knowledge bases. In particular, we focus on mining entities and relations from unstructured text data sources, entity disambiguation, entity linking and question answering. We conclude by highlighting general trends in knowledge mining research and identifying problems that require further research to enable more extensive use of knowledge bases.
Induced and Permanent Magnetism on the Moon: Structural and Evolutionary Implications
Authors: Sonett C. P. , Dyal P. , Colburn D. S. , Smith B. F. , Schubert G. , Schwartz K. , Mihalov J. D. , Parkin C. W.
Published: March 2016

It is shown that the Moon possesses an extraordinary response to induction from the solar wind due to a combination of a high interior electrical conductivity together with a relatively resistive crustal layer into which the solar wind dynamic pressure forces back the induced field. The dark side
response, devoid of solar wind pressure, is approximately that expected for the vacuum case. These data permit an assessment of the interior conductivity and an estimate of the thermal gradient in the crustal region. The discovery of a large permanent magnetic field at the Apollo 12 site corresponds approximately to the paleomagnetic residues discovered in both Apollo 11 and 12 rock samples The implications regarding an early lunar magnetic field are discussed and it is shown that among the various conjectures regarding the early field the most prominent are either an interior dynamo or an early approach to the Earth though no extant model is free of difficulties.
Session I: Origin of the Solar Nebula
Authors: Hoyle F.
Published: March 2016

Prof. Fred L. Whipple kindly agreed to be the chairman for all three panels, and introduced the next speaker, Prof. F. Hoyle, who spoke on ‘The Solar Nebula’. Hoyle: I would like to begin this contribution by considering the deductions we can make by comparing the gross chemical compositions of the planets with the composition of the Sun. For this purpose I have divided the planets into the three groups shown in

The second line gives the mass fractions in the Sun of the major constituents of the planetary groups, while the fourth line gives the factors by which the present masses must be multiplied to give the amounts of solar material needed to yield the appropriate amounts of main planetary constituents. The interesting points emerge that Jupiter and Saturn require the least amount of solar material, and that Uranus and Neptune on the one hand and the terrestrial planets on the other require approximately equal amounts. The total requirement is for ≈10-2Mʘ This is less by a factor ≈10 than the amount postulated in many theories of the origin of the planetary system. However the amount we have now calculated can readily be seen to be consistent with angular momentum requirements.
Microwave Evidence For Interstellar Molecules
Authors: Townes C. H.
Published: March 2016

Some time ago, optical astronomy was successful in detecting the first molecular species in interstellar space. However, these have been limited to the three diatomic molecules CH, CH+, and CN. Consideration of this list made it rather natural, after the development of microwave astronomy, for some attention to be given to a search for OH, which has a rather strong microwave transition. This molecule was first detected, after a considerable search, by Weinreb et al.. The analogous Λ-doublet transitions in SH and CH have since been searched for assiduously; failure to detect them does not necessarily mean these radicals are excessively rare in interstellar space, since various unfavorable factors make the search difficult.

Any consideration of polyatomic molecules in interstellar space immediately raises the question as to whether and where such molecules are likely to exist. Of course, they can occur in stellar atmospheres, where they have already been found to a limited extent. But in free interstellar space they are less likely to exist because of slow rates of formation and a rather short lifetime, the latter being typically limited to a few hundred years because of dissociation by ultraviolet radiation from stars. In dust clouds, molecules are more protected from ultraviolet radiation and their formation may be aided by catalysis on the dust grain surfaces.
Molecules in Dense Clouds And Protostars
Authors: Mezger P. G.
Published: March 2016

This paper deals with the interpretation of molecular line emission from class I OH/H2O emission centers associated with compact HII regions and with the OH 18 cm emission from dark clouds in T-Tauri star associations. Observational evidence is presented, that class IOH/H2O emission centers represent a particular stage in the evolution of a massive star (or a group of massive stars) whereas protostars of lower mass apparently do not go through such a stage.

It appears that in associations the low-mass stars are formed first and the massive O-stars are formed last. T-Tauri star associations may represent an early evolutionary stage of a star association where low-mass stars are formed. Evidence is presented that the physical conditions in some parts of the Taurus complex of dust clouds and T-Tauri stars are appropriate for the formation of single stars of about a solar mass.
Photochemistry of Atoms and Molecules in the Adsorbed State
Authors: Breuer H. D. , Moesta H.
Published: March 2016

Assuming interstellar dust particles being composed at least partly of materials with catalytic activity or of refractory metals and being exposed to the radiation field of the Sun or other stars they can favour the formation of molecules as combinations of the most abundant gases H, C, N and O mainly for three reasons:

(1) By the adsorption at the surface of dust particles the collision probability for two or more atoms is greatly enhanced with respect to the gas phase.

(2) Because of the adsorption bond the excitation and dissociation energies are shifted to lower values.

(3) For highly exothermic reactions dust particles can absorb the excess energy and thus lead to the formation of molecules which in the gas phase can be formed only by three body collisions.
Remarks on the Restoration of Occultation Observations
Authors: Deeming Terence J.
Published: March 2016

If the limb of the Moon can be regarded as a straight edge, then the diffraction pattern of a point source which it produces at the distance of the Earth is the well known Fresnel diffraction pattern. Observations of stellar occultations reveal the variation of intensity with time as the diffraction pattern passes across the detector due to the orbital motion of the Moon and the rotation of the Earth. The linear scale of the diffraction pattern in monochromatic light depends on both the wavelength of observation, λ, and on the distance of the Moon, D, so that the scale is proportional to (λD)1/2.
Composition and Galactic Confinement of Cosmic Rays
Authors: Shapiro Maurice M.
Published: March 2016

The ‘Galactic’ cosmic rays impinging on the Earth come from afar over tortuous paths, traveling for millions of years. These particles are the only known samples of matter that reach us from regions of space beyond the solar system. Their chemical and isotopic composition and their energy spectra provide clues to the nature of cosmic-ray sources, the properties of interstellar space, and the dynamics of the Galaxy. Various processes in high-energy astrophysics could be illuminated by a more complete understanding of the arriving cosmic rays, including the electrons and gamma rays.

En route, some of theprimordialcosmic-ray nuclei have been transformed by collision with interstellar matter, and the composition is substantially modified by these collisions. A dramatic consequence of the transformations is the presence in the arriving ‘beam’ of considerable fluxes of purely secondary elements (Li, Be, B), i.e., species that are, in all probability, essentially absent at the sources. We shall here discuss mainly the composition of the arriving ‘heavy’ nuclei -those heavier than helium - and what they teach us about thesourcecomposition, the galactic confinement of the particles, their path lengths, and their transit times.
The Lick Observatory Program on Proper Motions of RR Lyrae Stars
Authors: Klemola A. R.
Published: March 2016

It is the purpose of this note to reveal the nature and progress of a long term astrometric program at the Lick Observatory (see references by S. Vasilevskis in Trans. Int. Astron. Union, XI B, 404, 1962). One of its many goals is the measurement of absolute proper motions of RR Lyrae stars with respect to faint galaxies. The first-epoch photographs, obtained in 1947-54 by Shane and Wirtanen for the sky north of declination – 23°, were supplemented later by plates of poorer quality down to –33° with the 20-in. astrograph. This means that first-epoch plates are now on hand which cover three-fourths of the sky and on which stars of 9-17 mag. may be measured for proper motions. Since these photographs represent the largest and most homogeneous set that will be available in the foreseeable future, we shall try to estimate the number of RR Lyrae stars which may be measured on them.

As a guide we take the 1968 edition of the Russian Variable Star Catalogue, which contains a little over 4400 RR Lyrae stars. For the sky north of —33° nearly 2000 of these stars are brighter than average magnitude 17.0, 1000 brighter than 15.0, and about 350 brighter than 12.0. Experience with the Lick program shows that 80% of these stars should be measurable, after account is made for losses due to plate defects, blended images, and other factors.

An important limitation to the usefulness of the measured motions is imposed by the size of the mean errors, which amount to 0.”7/century for an epoch difference of 20 yr. This mean error is the same size as the proper motion of a typical RR Lyrae star of 13.0 mag. But for an epoch difference of 50 yr the mean error drops to 0.”3/century, which is comparable to the motion of an RR Lyrae star of 15.0 mag. Useful results for the fainter RR Lyrae stars will not be possible until after a third epoch about the year 2000.
Recent Techniques in Solar Optical Astronomy from Space
Authors: Reeves E.M.
Published: March 2016

Abstact

The article summarizes some of the recent advances in the techniques of solar space research, particularly over the last 4 years, in an attempt to review the current state of instrument technology. The present state of development in rocket and satellite vehicles for solar observations, far ultraviolet detectors, optical materials, ultraviolet reflection coatings, filters, and photographic film fogging, are among the topics described.
The Mixing of Lithium
Authors: Spiegel E. A.
Published: March 2016

The observational status of the problem of lithium abundances has been thoroughly detailed in the preceding papers in this symposium, and it is clear why we must consider how matter is mixed from outer convection zones to inner, hotter regions. The need for appropriate mixing mechanisms has also been nicely brought out by Herbig and Wolff, and Böhm has summarized the role of convective mixing. Conventional mixing-length models for the outer convection zones seem to give qualitatively reasonable results for the depletion during pre-main-sequence contraction but do not completely account for the observations, and it seems inescapable that main-sequence depletion of lithium must be considered. I shall therefore simplify the discussion of mixing by concentrating on main-sequence models in the following outline of some possible mixing processes, though most of the remarks to be made should apply generally to other phases. I shall also pretend that there is one principle mechanism (or combination of them) that must be found, though stars in different evolutionary phases, or with different masses, may deplete lithium quite differently. Further, I shall use the Sun as an illustration in general since we know some important details about it that are not always known for other stars.
The Overlap Approach Toward the Derivation of Photographic Stellar Coordinates
Authors: Googe W. D. , Lukac C. F. , Eichhorn H.
Published: March 2016

The use of the conditions imposed by the appearance of one star on more than one photographic plate to strengthen the determination of the relationship between the measurement coordinate systems and the system of celestial right ascension and declination, was first advocated by Eichhorn (1960), and since then various reduction procedures have been proposed to incorporate these conditions in the plate-reduction process (Eichhorn, 1963; Henriksen, 1964; Lacroute, 1964; Googe, 1967; Clube, 1967). During the last several years at the Army Map Service the overlap method has been developed and used in several astrometric projects, and the purpose of this paper is to summarize the main features of the algorithm and some of the projects to which it has been applied.
Report on Overlap Methods in Photographic Astrometry
Authors: de Vegt Chr.
Published: March 2016

The usual procedure for deriving standard coordinates ξ,η from the measured rectangular coordinates x, y of a star is to adopt a suitable model for the relationship between the measured x, y, magnitude m, color index c and the ξ, η. This relationship may, in general, be written as

From the known standard coordinates ξr, ηr of some reference stars equally distributed over the plate area, the unknown plate constants aijkl, bijkl are found from a least-squares adjustment. After the adjustment the standard coordinates of each field star can be computed. In most cases a statistical criterion for the choice of the proper form of the above relationship between measured and standard coordinates may be useful because the systematic accuracy, obtained from the adjustment, may be seriously affected by the number of unknown parameters included. (Eichhorn et al., 1967). If the same star occurs on two or more plates, i.e. the plates being partly overlapped, one gets the final position by taking the mean of the individual positions on each plate. In this procedure, no direct account is taken of the ‘overlap’ in the equations of condition for the desired plate constants.
Optical Spectra of Extragalactic Radio Sources
Authors: Burbidge E. Margaret
Published: March 2016

Extragalactic radio sources can be grouped spectroscopically into those that show absorption lines produced by a stellar population (e.g. the nearer radio galaxies, and some more distant ones, usually of D or E type) and those that show only lines (usually in emission) produced by low-density gas (e.g. QSO’s and many N-type galaxies). If absorption lines from stars are present, one can estimate a minimum age from the stellar population, and perhaps a mass for the system from the stellar velocity dispersion. If no spectroscopic evidence on the stellar population is available (and this includes evidence from narrow-band filter photometry), then we have much less hold on the problems of age and evolutionary state. Absence of stellar absorption lines does not necessarily mean that stars are absent, but simply that their light, if present, does not contribute appreciably to the overall optical spectrum.
The Evolution of Quasi-Stellar Sources and Radio Galaxies
Authors: Ryle M.
Published: March 2016

There seem to be two promising ways of investigating the evolution of radio sources: (a) the collection of data on a large number of sources so that attempts may be made to arrange them in an evolutionary sequence, (b) the study of a few sources, for which really detailed information is obtainable, to gain insight into the physical mechanisms occurring.

It is important to distinguish between the most powerful radio sources, the majority of which appear to have a simple double structure at the resolutions now attainable, and the more complex sources. The structure of the latter suggests that energetic particles have been accelerated in multiple ‘events’, each being of smaller magnitude than the events which give rise to the double sources; the total energy released may, however, be comparable.
Photographic Results of the Lunar Orbiter Program
Authors: Brunk William E.
Published: March 2016

The principal goal of the Lunar Orbiter program was to obtain photographic coverage of selected areas of the lunar surface at resolutions of 1 and 8 m. As the success of the program was greater than originally anticipated, the photographic coverage was extended to include the entire front side of the Moon at a resolution one order of magnitude greater than possible from the Earth and almost all of the far side. In this paper, a selection of photographs obtained from all five missions will be presented.
Introduction
Authors: Goldberg L. , Švestka Z.
Published: March 2016

The newly established Inter-Union Commission on Solar-Terrestrial Physics (IUCSTP) has inquired of selected experts about actions useful in the period of the next solar maximum, which need an organization and coordination on international basis. These inquiries have shown that one of the problems, in which a broad international cooperation might lead to substantial improvement of scientific results, is the coordination of ground-base and space-vehicle observations of the Sun and its active phenomena.

Therefore, in order to help the IUCSTP in its preparatory work, the chairmen of IAU Commissions 10 (Solar Activity) and 44 (Observations from outside the Atmosphere) agreed to hold a joint meeting of these two Commissions during the IAU Assembly in Prague, on ‘Coordination of solar observations made at ground-base Observatories and with space vehicles’. It was anticipated that other IAU members interested in this problem, particularly members of Commissions 12 and 40, would also take part in the discussion.
Space Observations Needed for Improving Our Knowledge of Solar Flares
Authors: Severny A.B.
Published: March 2016

Up to the present time the technical possibilities of space research were not quite adequate for obtaining the ultraviolet spectrum of flares that occupy only a small portion (less than 10″ of arc) of the solar disk. Up to now all observations have been made in integrated sunlight. The importance of the knowledge of UV spectrum of flares is hardly necessary to emphasize. For example we just could mention that if ultraviolet spectra were available for a flare say from 850 Å up to 2000 Å, we would be able to estimate such extremely important parameters as the number of hydrogen atoms N1 in the first quantum state (by using L-α, L-β, etc.), electronic temperature and density (from Lyman continuum) and other physical parameters of a flare which at the present time we try to derive by different indirect and inadequate methods. Several resonance (ultimate) lines are concentrated in this spectral interval and their careful examination in flares can bring additional important information about conditions prevailing in flares and in the underlying chromosphere. The same applies of course to the whole UV spectrum below 800 Å, and in particular to the resonance lines of HeI (λ 512 Å) and HeII (λ 304 Å), as well as to a number of lines of highly ionized atoms.
The Needs and Requirements from the Standpoint of the Ultraviolet Solar Observations
Authors: Reeves E.M.
Published: March 2016

Extending from the present to the early part of 1969 there are three Orbiting Solar Observatories to be launched, and these will all be capable of constructing spectroheliograms of the Sun in solar emission lines of the EUV and X-ray region. The recently launched and highly successful OSO-III has obtained EUV and X-ray spectra with high-time resolution, but without spatial resolution on the solar disk. The later OSO satellites will provide spatial resolution of 1′ of arc to 30″ of arc, and will provide the basis for the extension to even higher spatial resolution in the future.

The comparatively short periods covered by these satellites, coupled with a real probability of only partial success, make it particularly important to obtain the fullest possible use of the data by implementing a complementary and simultaneous series of ground-based observations.
Galaxies and Their Nuclei
Authors: Ambartsumian V. A.
Published: March 2016

Our Extraordinary General Assembly is devoted to the memory of one of the greatest men of science to the genial Polish astronomer - Nicolaus Copernicus. The main service of Copernicus which has made his name immortal was in finding the correct interpretation of the planetary motions we observe. Instead of geocentric notions, which proved unable to explain the accumulated bulk of empirical data on the apparent motions of planets he has put forward and advocated the notion of a solar system thus presenting the true picture of the part of the Universe we live in. The scientific revolution started by him was continued by Galileo and Kepler and was crowned with the great theoretical generalizations of Newton. As a result a foundation has been created for the most exact theories of motions in the solar system which were developed during the next centuries. These theories in their modern form give also the possibility to solve all the problems concerning the orbital motions of spaceships.

At this stage we can not yet boast that in the study of nuclei of galaxies and their activity we have reached the level which existed in planetary astronomy even before the works of Newton. Only 15 years elapsed from the moment when the idea of activity of nuclei of galaxies was clearly formulated (Ambartsumian, 1958). During these years discoveries of the greatest importance have been made. New unexpected discoveries occur almost each year. These discoveries influence decisively our notions on the diversity of objects and phenomena in the distant space, but they are still insufficient for the construction of adequate theories. In order to penetrate into the very nature of nuclear phenomena we require new observations, new measurements and new data. And if some optimists imagine that the time has already ripen to build a general theory of these phenomena, the more cautious astronomers would like to consider a more or less satisfactory systematization of observational data concerning the activity of nuclei and the understanding of external physical processes accompanying it as a tremendous success.
Pro and Contra Changes in the Conventional Values of Precession
Authors: Fricke W.
Published: March 2016

From an evalution of the arguments pro and contra changes in the precessional constants it is concluded that corrections should be made simultaneously with changes in the values of planetary masses at the time when the new fundamental reference system, the FK5, is introduced into the ephemerides. In this case the location and motion of the equinox would be corrected at the same time. An IAU decision on changes in the constants should be made in 1976. Since the completion of the FK5 may be expected around 1980, the introduction into the ephemerides appears practicable in 1984.
High Resolution Spectra of M and C Stars by Fourier Transform Spectroscopy
Authors: Maillard J. P.
Published: March 2016

A Michelson interferometer was put into operation during the year 1972 at the Coudé focus of the Haute-Provence Observatory’s 76-in. telescope. We built this instrument at Aimé Cotton Laboratory (Orsay-France) where the method of Fourier Transform Spectroscopy has been largely developed in the direction of very high resolution work. A complete description of this device has been given elsewhere (Guelachvili and Maillard, 1970) and further details on the present study are reported by Maillard (1973).
Gould’s Belt
Authors: Lindblad P. O.
Published: March 2016

The zone of bright stars inclined 20° to the galactic plane, pointed out by John Herschel (1847) and by Gould (1874,1879), is generally referred to as Gould’s Belt. This General Assembly is well timed. With the splendour of the centre of the Milky Way in the zenith in the early hours of the night anyone who comes out of the city-lights of Sydney can try to convince himself of the reality of this phenomenon.

Shapley and Cannon (1922, 1924) showed that the concentration towards Gould’s Belt is very pronounced for the brighter B. stars, while the fainter ones are highly concentrated towards the galactic plane. Their results indicated the radius of this local system to be of the order of 500 pc. The motions of the B. stars brighter than a magnitude of about 5m.5 are characterized by the K-effect, which thus seems to be a property of this local Gould Belt system.
The Kinematics and Ages of Stars in Gliese’s Catalogue
Authors: Wielen R.
Published: March 2016

This contribution gives some results on the kinematics and ages of stars near the Sun. These results are mainly based on the catalogue of nearby stars compiled by Gliese (1957, 1969 and minor recent modifications). Table I shows the number of objects under consideration. While the old catalogue (1957) contained only stars with distances r up to 20 pc, the new edition (1969) includes many stars with slightly larger distances. In Table I, a ‘system’ is either a single star or a binary or a multiple system. The number of systems with known space velocities nearer than 20 pc has increased by about 30% from 1957 to 1969. The first edition of Gliese’s catalogue (1957) has been analyzed in detail by Gliese (1956) and von Hoerner (1960).
Space Distribution and Motion of the Local HI Gas
Authors: Weaver H.
Published: March 2016

In a Joint Discussion devoted to the ages and kinematics of the local stars, inclusion of a paper on the local gas may seem anomalous. There is, however, strong justification for considering such a topic. Newly formed stars retain many properties of the gas from which they originated. To understand the spatial and kinematic properties of local young stars, we must understand the spatial distribution and the kinematics of the local gas from which they were formed.

A cloud within the interstellar gas can collapse gravitationally if its mass, density, and temperature satisfy the Jeans Criterion. Collapse is favored by low temperature and high density.

Various investigators have pointed out that in the Lin Spiral Density Wave Theory a shock must occur on the inner edge of a spiral arm. Such a shock compresses the gas and hence promotes cloud formation with subsequent gravitational collapse to form stars. Shu and several collaborators have shown that such a shock is very effective in triggering cloud formation in a two-phase interstellar medium of the type discussed by Field et al. (1969), and it is widely believed that this is the principal step in the process of forming stars.
OSO-8 X-Ray Polarimeter and Bragg Crystal Spectrometer Observations
Authors: Novick R. , Kestenbaum H.L. , Long K.S. , Silver E.H. , Weisskopf M.C. , Wolff R.S.
Published: March 2016

The OSO-8 satellite contains a focusing mosaic graphite crystal X-ray polarimeter that is oriented along the spin axis of the wheel section of the satellite. The polarimeter operates at 2.6 and 5.2 keV. Polarization in a source appears as a modulation of the counting rate at twice the satellite spin frequency. The amplitude and phase of the modulation are simply related to the polarization and position angle, respectively. Two independent polarimeters are employed, and their axes are offset by 128°. Focusing is achieved by mounting the crystals on a parabolic sector, which reduces the background without reducing the sensitivity. The low background that results from the focusing not only improves the statistical quality of the data but also substantially reduces the danger that an asymmetry in the charged particle background may produce a spurious polarization result. This is particularly important in the case of weak sources. The instrument has been described in detail elsewhere (Novick 1975); here we will briefly discuss the results obtained on the Crab Nebula, Cyg X-l, and Cyg X-2.
A Model for Bursting X-Ray Sources
Authors: Henriksen R.N.
Published: March 2016

A model given by Henriksen and Chia (1972) for short duty cycle X-ray flare sources has been extended by Henriksen (1976), and applied to the recently discovered X-ray bursters. We use their notation here unless otherwise indicated. The model envisages a rapidly rotating magnetic white dwarf or neutron star located in a dense stream or cloud of gas such as might be found in close binary systems or in dense interstellar clouds. The basic charging mechanism for the flare is the accretion of matter into the hydromagnetic wave zone of the rotator at the ‘Bondi’ or ‘tail-shock’ rate (corresponding to a thermal cloud or a stream,-respectively), AB.
Masses of Compact X-Ray Sources
Authors: Avni Yoram
Published: March 2016

The presence of compact x-ray sources in binary systems provides an opportunity to determine observationally the masses of neutron stars and possibly of black holes. These masses are important for equations of state at nuclear densities, for theories of gravitation, and for late stages of stellar evolution. A mass range for each source is determined by finding the sets of orbital elements that are consistent with the available x-ray and optical data. As such analyses are subject to various uncertainties, the resulting mass ranges are rather wide. Nevertheless, significant mass estimates are obtained, accompanied by interesting results on other system parameters.
Density Profiles of Clusters of Galaxies
Authors: Bahcall Neta A.
Published: March 2016

Data on the surface distribution of galaxies in a number of clusters has been given by several authors (see, for example, Shane & Wirtanen 1954; Zwicky 1956, 1957; Omer, Page & Wilson 1965; Clark 1968; Noonan 1971, 1974; Bahcall 1971, 1972a, b, 1973a, b, 1974, 1975; Rudnicki 1963; Rudnicki & Baranauska 1966a, b; Rood et al. 1972; Rood & Sastry 1972; Oemler 1974; Austin & Peach 1974a, b; Chincarini & Rood 1975, 1976; and references quoted therein). The distributions show a relatively smooth fall-off from a high density at the center of the cluster to a low density tail at the outskirts of the cluster. Secondary maxima or subclustering are sometimes superimposed on an otherwise smooth and monotonic profile.