bluuebunny/crossref_metadata_2025 huggingface dataset:
Aligning Corporate Social Responsibility with Green Economy Development Pathways in Developing Countries
Authors: Shah Kalim U. , Arjoon Surendra , Rambocas Meena
Published: March 2016

Corporate social responsibility (CSR) can be conceptualized as a mechanism through which private sector investment aligns with and shapes sustainable development. In recent years the new economic paradigm of the green economy has been adopted by many developing countries and forwarded by governments and multilateral institutions. It is in this burgeoning socio‐economic context that firms will practice their CSR. In this study, we explore the determinants of such CSR in a green economy by using structural equation modeling techniques to analyze empirical data collected from five Caribbean countries already on the green economy pathway. We find that firm level environmental policies and to a lesser extent relationships with external stakeholder networks are the main determinants of CSR in the green economy. Firms’ environmental practices and internal practices also influence CSR, but only indirectly when mediated by their environmental policies. The findings suggest that firm level environmental policies are critical to successfully aligning CSR with sustainable development in the green economy context. Copyright © 2016 John Wiley & Sons, Ltd and ERP Environment.
Exploring Links Between Education and Sustainable Development Goals Through the Lens of UN Flagship Reports
Authors: Vladimirova Katia , Le Blanc David
Published: March 2016

Based on an exhaustive content analysis of 37 global reports, this paper examines how well links between education and other Sustainable Development Goals (SDGs) are represented in flagship publications of the United Nations system. Taken together, the reports identify links between education and all the SDGs, with the notable exception of SDG 14 on oceans. However, some goal areas have received much more attention than others. While some causal links are identified and highlighted as important, relevant constraints are sometimes not extensively discussed, and few concrete policy options to act on these links are provided. Going forward, it would be important to assess whether the messages contained in UN flagship reports adequately reflect the state of scientific knowledge and the lessons learnt from development programs that focus on education in relation to specific SDGs. The systematic analysis provided here can offer a basis for an integrated analysis of policy priorities for education as a whole. Copyright © 2016 John Wiley & Sons, Ltd and ERP Environment
Sustainable Desert Traditional Architecture of the Central Region of Saudi Arabia
Authors: Mortada Hisham
Published: March 2016

For thousands of years mud houses have represented the practical wisdom and spirituality of people, particularly those of desert regions, who learned how to use local materials to build homes that fitted the environmental and cultural conditions, in which they lived. As a case study, the central region of Saudi Arabia exhibits a tradition of earth architecture that is unique in style, culture and sustainability. Aiming to contribute towards the local debate of the suitability of the traditional mud architecture for today's lifestyle of Saudis, this paper explores the sustainable nature of the traditional adobe architecture of this hot arid region from environmental, social and technical points of view. Copyright © 2016 John Wiley & Sons, Ltd and ERP Environment
Traceback model for identifying sources of distributed attacks in real time
Authors: Ahmed Abdulghani Ali , Sadiq Ali Safa , Zolkipli Mohamad Fadli
Published: March 2016

Locating sources of distributed attack is time‐consuming; attackers are identified long after the attack is completed. This paper proposes a trackback model for identifying attackers and locating their distributed sources in real time. Attackers are identified by monitoring violations of malicious end users on their bandwidth shares predefined in the service level agreement. Then, active connections of the malicious users are investigated to locate the host machines used as distributed sources of attack traffic. Mathematical model and simulation results demonstrate that the proposed model can reduce the required time for identifying malicious users and locating host machines used as the actual sources of attack packets. Copyright © 2016 John Wiley & Sons, Ltd.
Neutron reflectometry study of CrAlN/TiAlN nanostructured multilayers
Authors: Du Xiaoming , Wang Minpeng , Wang Yan , Li Xinxi , Zhang Zhong , Zhang Gang , Huang Chaoqiang , Wu Erdong
Published: March 2016

Alternate CrAlN/TiAlN multilayers with different repeated bilayer thickness ranging from 10 to 20 nm were prepared by sputtering Ti, Al and Cr targets with N2 and Ar gases. The interface structures of multilayers such as the average individual thicknesses, the scattering length densities and interface roughness were characterized using nonpolarized specular neutron reflectometry. The experimental reflectivity can be well described by a multilayer model for all samples. The individual thickness in the repeated bilayers is close to the nominal thickness. The interface roughness diminishes as the thickness of the bilayer in mutilayers decreases. The asymmetric interface roughness on CrAlN‐TiAlN‐Si interfaces causes the larger interface roughness of CrAlN on TiAlN interface. The scattering length density profiles of multilayers suggest that the chemical composition is approximate to Cr0.86Al0.14N/Ti0.5Al0.5N and which is more accurate for thinner films. Copyright © 2016 John Wiley & Sons, Ltd.
New insights into the evaluation of randomized controlled trials for rare diseases over a long‐term research horizon: a simulation study
Authors: Bayar Mohamed Amine , Le Teuff Gwénaël , Michiels Stefan , Sargent Daniel J. , Le Deley Marie‐Cécile
Published: March 2016

Large sample sizes are required in randomized clinical trials designed to meet typical one‐sided 2.5% α‐level and 80% power. This may not be achievable when the disease is rare. We simulated a series of two‐arm superiority trials over a 15‐year period. The design parameters examined were the α‐level and the number of trials conducted over the 15‐year period (thus, trial sample size). Different disease severities and accrual rates were considered. The future treatment effect was characterized by its associated hazard rate; different hypotheses of how treatments improve over time were considered. We defined the total survival benefit as the relative difference of the hazard rates at year 15 versus year 0. The optimal design was defined by maximizing the expected total survival benefit, provided that the risk of selecting at year 15 a treatment inferior to the initial control treatment remains below 1%. Compared with two larger trials with typical one‐sided 2.5% α‐level, performing a series of small trials with relaxed α‐levels leads on average to larger survival benefits over a 15‐year research horizon, but also to higher risk of selecting a worse treatment at the end of the research period. Under reasonably optimistic assumptions regarding the future treatment effects, optimal designs outperform traditional ones when the disease is severe (baseline median survival ≤ 1 year) and the accrual is ≥100 patients per year, whereas no major improvement is observed in diseases with better prognosis. Trial designs aiming to maximize survival gain over a long research horizon across a series of trials are worth discussing in the context of rare diseases. Copyright © 2016 John Wiley & Sons, Ltd.
The Marian restoration in Ireland
Authors: Jefferies Henry A.
Published: March 2016

Mary’s endeavours to restore Catholicism in England have attracted much scholarly attention and not a little controversy, primarily because of her bloody response to the scale and persistence of the Protestant challenge she faced there. Her endeavours in Ireland, by contrast, have been relatively overlooked. Yet the Marian restoration in Ireland ought to be recognised as an integral part of Mary’s religious programme for her dominions. It offers interesting points of comparison for the implementation of the queen’s programme in England, and it was significant in its own right, not as a decisive watershed but, as a time when religious controversies were crystallised and definite decisions were made that proved significant in the subsequent survival of Catholicism as the religion of the people of Ireland.
The Cross cult, King Oswald, and Elizabethan historiography
Authors: Stapleton Paul J.
Published: March 2016

In Thomas Stapleton’sThe History of the Church of Englande(1565), the first modern English translation of Bede’sHistoria Ecclesiastica Gentis Anglorum, the cross cult is promoted as a definitive element of English religious and national identity, via the legend of the Saxon king Oswald. The version of the legend in Stapleton’s narrative, which includes textual supplements like illustrations, appears to be intended as a corrective in light of attacks upon the cross cult made in works of religious controversy by the reformists William Turner, John Jewel, and James Calfhill, but also in works of historiography such as the 1559 edition of Robert Fabyan’sChronicle.In response to Stapleton’s expanded presentation of the Oswald legend, John Foxe reconfigures the narrative in the 1570Acts and MonumentsorBook of Martyrs, but in a bifurcated manner, perhaps to appease members of Matthew Parker’s circle of Saxon scholars. Surprisingly, in Book Three ofThe Faerie Queene(1590), Edmund Spenser carries on Stapleton’s iconodule understanding of Oswald’s cross in contrast to his reformist Protestant precursors.1
On the Age and Growth Rate of Giant Cacti: Radiocarbon Dating of the Spines of Cardon (Pachycereus Pringlei)
Authors: Delgado-Fernández Mariana , Garcillán Pedro P , Ezcurra Exequiel
Published: March 2016

Age estimation has been a limiting factor in the study of giant columnar cacti. In order to test the feasibility of using radiocarbon methods to estimate the age of the giant cardon cacti (Pachycereus pringlei), we selected six sites spanning the latitudinal and precipitation range of the species in the Baja California peninsula. In each site, we selected four individuals of different heights and sampled a spine from the lowest areole in the stem. The age of the spine was estimated using 14C dating, and the mean annual growth rate of the plant was calculated dividing the height of the lead shoot by the plant’s age. Mean annual growth rate was 0.098 m/yr, with values varying between 0.03 and 0.23 m/yr. Within the range of plants sampled, mean annual growth rates were significantly correlated with the height of the plant (r2=0.82, P<0.0001), and no other site-specific variable such as precipitation or latitude was a significant predictor of mean annual growth rates. A model integrating mean growth rate versus height showed that relatively small differences in growth rates between plants accumulate during the plants’ lifetime, so that plants of similar size may have very different ages. We conclude that 14C dating provides a robust method to explore the growth and demography of columnar cacti.
Antimicrobial activity of the pygidial gland secretion of the troglophilic ground beetleLaemostenus(Pristonychus)punctatus(Dejean, 1828) (Insecta: Coleoptera: Carabidae)
Authors: Nenadić M. , Soković M. , Glamočlija J. , Ćirić A. , Perić-Mataruga V. , Tešević V. , Vujisić L. , Todosijević M. , Vesović N. , Ćurčić S.
Published: March 2016

The antimicrobial activity of the pygidial gland secretion released by adult individuals of the troglophilic ground beetleLaemostenus(Pristonychus)punctatus(Dejean, 1828), applying microdilution method with the aim to detect minimal inhibitory concentration, minimal bactericidal concentration and minimal fungicidal concentration, has been investigated. In addition, morphology of the pygidial glands is observed. We have tested 16 laboratory and clinical strains of human pathogens – eight bacterial both gram-positive and gram-negative species and eight fungal species. The pygidial secretion samples have showed antimicrobial properties against all strains of treated bacteria and fungi.Micrococcus flavusproved to be more resistant compared with other bacterial strains. More significant antimicrobial properties of the secretion are observed againstEscherichia coli, which proved to be the most sensitive bacteria.Aspergillus fumigatusproved to be the most resistant, whilePenicillium ochrochloronandPenicillium verrucosumvar.cyclopiumthe most sensitive micromycetes. Commercial antibiotics Streptomycin and Ampicillin and antimycotics Ketoconazole and Bifonazole, applied as positive controls, showed higher antibacterial properties for all bacterial and fungal strains, except forP. ochrochloron, which proved to be more resistant on Ketoconazole compared with the pygidial gland secretion ofL.(P.)punctatus. Apart from the role in ecological aspects, the antimicrobial properties of the tested secretion possibly might have medical significance in the future.
Climate effects on crop yields in the Northeast Farming Region of China during 1961–2010
Authors: YIN X. G. , OLESEN J. E. , WANG M. , ÖZTÜRK I. , CHEN F.
Published: March 2016

Crop production in the Northeast Farming Region of China (NFR) is affected considerably by variation in climatic conditions. Data on crop yield and weather conditions from a number of agro-meteorological stations in NFR were used in a mixed linear model to evaluate the impacts of climatic variables on the yield of maize (Zea mays L.), rice (Oryza sativa L.), soybean (Glycine max L. Merr.) and spring wheat (Triticum aestivum L.) in different crop growth phases. The crop growing season was divided into three growth phases based on the average crop phenological dates from records covering 1981 and 2010 at each station, comprising pre-flowering (from sowing to just prior to flowering), flowering (20 days around flowering) and post-flowering (10 days after flowering to maturity). The climatic variables were mean minimum temperature, thermal time (which is used to indicate changes in the length of growth cycles), average daily solar radiation, accumulated precipitation, aridity index (which is used to assess drought stress) and heat degree-days index (HDD) (which is used to indicate heat stress) were calculated for each growth phase and year. Over the 1961–2010 period, the minimum temperature increased significantly in each crop growth phase, the thermal time increased significantly in the pre-flowering phase of each crop and in the post-flowering phases of maize, rice and soybean, and HDD increased significantly in the pre-flowering phase of soybean and wheat. Average solar radiation decreased significantly in the pre-flowering phase of all four crops and in the flowering phase of soybean and wheat. Precipitation increased during the pre-flowering phase leading to less aridity, whereas reduced precipitation in the flowering and post-flowering phases enhanced aridity. Statistical analyses indicated that higher minimum temperature was beneficial for maize, rice and soybean yields, whereas increased temperature reduced wheat yield. Higher solar radiation in the pre-flowering phase was beneficial for maize yield, in the post-flowering phase for wheat yield, whereas higher solar radiation in the flowering phase reduced rice yield. Increased aridity in the pre-flowering and flowering phases severely reduced maize yield, higher aridity in the flowering and post-flowering phases reduced rice yield, and aridity in all growth phases reduced soybean and wheat yields. Higher HDD in all growth phases reduced maize and soybean yield and HDD in the pre-flowering phase reduced rice yield. Such effects suggest that projected future climate change may have marked effects on crop yield through effects of several climatic variables, calling for adaptation measures such as breeding and changes in crop, soil and agricultural water management.
Common wheat and cereal bug interactions: kernel quality depletion and immunodetection of damage
Authors: VACCINO P. , INGEGNO B. L. , PANSA M. G. , COPPA T. , TAVELLA L.
Published: March 2016

Several species of Heteroptera are responsible for kernel damage in wheat, Triticum aestivum L. (Poaceae), which affects bread-making quality. In Europe, the most noxious bugs belong to the genera Eurygaster (Scutelleridae) and Aelia (Pentatomidae). In the present work, five bug species frequently found in wheat fields in north-western Italy, Eurygaster maura, E. austriaca, Aelia acuminata, Nezara viridula and Carpocoris purpureipennis, were tested in field trials for their capacity to induce wheat damage. The sodium dodecyl sulphate sedimentation volume test was used as the qualitative control. Among the bug species tested, E. maura was the most noxious pest, with C. purpureipennis being almost as noxious as E. maura. In contrast, E. austriaca and A. acuminata, which have been considered the wheat pests of major importance, as well as N. viridula, caused no or only moderate damage to wheat quality. The adoption of an antiserum specifically produced with E. maura salivary glands proved to be effective and specific in detecting bug damage. Therefore, this polyclonal antibody is promising for the development of a reliable test for the quick evaluation of commercial wheat flour batches.
The use of large and small subunits of ribosomal DNA in evaluating phylogenetic relationships between species ofCornudiscoidesKulkarni, 1969 (Monogenoidea: Dactylogyridae) from India
Authors: Verma J. , Agrawal N. , Verma A.K.
Published: March 2016

Two partial regions of ribosomal DNA (28S and 18S) were used to evaluate genetic variations among the species ofCornudiscoides,viz.C. proximus, C. geminusandC. agarwali, all parasites ofMystus vittatus(Bagridae) from River Gomati, Ganges River basin, India. Our findings demonstrated that both the large and small ribosomal subunits are useful for species identification and genetic characterization of parasites, leading to resolution of inter/intra-relationships at generic and specific levels. The secondary structures of all three species for 28S and 18S rRNA genes contained exact pattern matches (EMPs) displaying the high degree of similarity among them. The phylogenetic analyses within the members of Dactylogyridae demonstrated that species ofCornudiscoidescluster together for 28S rRNA and 18S rRNA genes.
Covariant magnetic connection hypersurfaces
Authors: Pegoraro F.
Published: March 2016

In the single fluid, non-relativistic, ideal magnetohydrodynamic (MHD) plasma description, magnetic field lines play a fundamental role by defining dynamically preserved ‘magnetic connections’ between plasma elements. Here we show how the concept of magnetic connection needs to be generalized in the case of a relativistic MHD description where we require covariance under arbitrary Lorentz transformations. This is performed by defining 2-D magnetic connection hypersurfaces in the 4-D Minkowski space. This generalization accounts for the loss of simultaneity between spatially separated events in different frames and is expected to provide a powerful insight into the 4-D geometry of electromagnetic fields when $\boldsymbol{E}\boldsymbol{\cdot }\boldsymbol{B}=0$.
Meta-analysis of DSM alcohol use disorder criteria severities: structural consistency is only ‘skin deep’
Authors: Lane S. P. , Steinley D. , Sher K. J.
Published: March 2016

Background

Item response theory (IRT) analyses of alcohol use disorder (AUD) and other psychological disorders are a predominant method for assessing overall and individual criterion severity for psychiatric diagnosis. However, no investigation has established the consistency of the relative criteria severities across different samples.

Method

PubMed/Medline, PsycINFO, Web of Science and ProQuest databases were queried for entries relating to alcohol use and IRT. Study data were extracted using a standardized data entry sheet. Consistency of reported criteria severities across studies was analysed using generalizability theory to estimate generalized intraclass correlations (ICCs).

Results

A total of 451 citations were screened and 34 papers (30 unique samples) included in the research synthesis. The AUD criteria set exhibited low consistency in the ordering of criteria using both traditional [ICC = 0.16, 95% confidence interval (CI) 0.06–0.56] and generalized (ICC = 0.18, 95% CI 0.15–0.21) approaches. These results were partially accounted for by previously studied factors such as age and type of sample (e.g. clinical v. community), but the largest source of unreliability was the diagnostic instrument employed.

Conclusions

Despite the robust finding of unidimensional structure of AUDs, inconsistency in the relative severities across studies suggests low replicability, challenging the generalizability of findings from any given study. Explicit modeling of well-studied factors like age and sample type is essential and increases the generalizability of findings. Moreover, while the development of structured diagnostic interviews is considered a landmark contribution toward improving psychiatric research, variability across instruments has not been fully appreciated and is substantial.
Impact of Decorrelation on Success Rate Bounds of Ambiguity Estimation
Authors: Wang Lei , Feng Yanming , Guo Jiming , Wang Charles
Published: March 2016

Reliability is an important performance measure of navigation systems and this is particularly true in Global Navigation Satellite Systems (GNSS). GNSS positioning techniques can achieve centimetre-level accuracy which is promising in navigation applications, but can suffer from the risk of failure in ambiguity resolution. Success rate is used to measure the reliability of ambiguity resolution and is also critical in integrity monitoring, but it is not always easy to calculate. Alternatively, success rate bounds serve as more practical ways to assess the ambiguity resolution reliability. Meanwhile, a transformation procedure called decorrelation has been widely used to accelerate ambiguity estimations. In this study, the methodologies of bounding integer estimation success rates and the effect of decorrelation on these success rate bounds are examined based on simulation. Numerical results indicate decorrelation can make most success rate bounds tighter, but some bounds are invariant or have their performance degraded after decorrelation. This study gives a better understanding of success rate bounds and helps to incorporate decorrelation procedures in success rate bounding calculations.
The Apollo Missions
Authors: Scherer L. R.
Published: March 2016

In successfully carrying out a manned lunar landing and return, with both operational and technological objectives, the Apollo program made possible a variety of significant scientific experiments. This important milestone in the continuing quest for knowledge took the eyes, hands, and mind of man, as well as his instruments, to a new world. The activities of highest priority carried out by the astronauts, once the landing had been successfully completed, were to collect lunar material and data, emplace sophisticated experiments, and record man’s impressions and observations.

In the missions ahead, scientific exploration of the Moon will be the principal goal. Unique features and sites on the Moon will be visited. New experiments, both on the lunar surface and in lunar orbit, will be carried out, as we probe the Moon’s past and attempt to unravel the early history of the Earth. In so doing, we will also be establishing and defining the possibilities and limitations of man as a space explorer as we extend his domain further in space.
Introductory Talk
Authors: Tayler R. J.
Published: March 2016

In this talk I shall try to outline the subject which will be discussed in detail by the succeeding speakers. I shall concentrate on ideas and I shall not attempt to present any definite results. The two sides to this problem are:

(a) How much helium is there in the Universe?

and

(b) Where and how has it been produced?

I shall sub-divide (a) and (b) into

(a) (i)

Direct observations

(ii)

Inferences from theories of stellar structure and evolution

(b) (i)

Helium production in stars

(ii)

Primeval helium production

(iii)

Production in other objects
Production of Helium by Stellar Evolution
Authors: Kippenhahn R.
Published: March 2016

In order to maintain the luminosity of the Galaxy ⅓ of a solar mass of hydrogen has to be transformed into helium every year. This rate of production is too small by a factor 10 or 20 in order to give a helium content of Y = 0.3-04. within the age of the galaxy if the mass fraction Y of helium was zero at the beginning. The situation is even worse if the destruction of helium by helium burning is taken into account. In his review paper Tayler (1967) came already to this conclusion. I shall discuss the problem here using more recent model calculations, but we shall come up with the same result.
Infrared Observations and Interstellar Molecules
Authors: Woolf N. J.
Published: March 2016

It has been common practice to separate the study of interstellar matter from that of stellar evolution. However, infrared astronomy deals mainly with observations of stars forming and stars dying. Interstellar matter represents a phase intermediate between these two stages, part of a cyclic process (Figure 1).

We find molecules in interstellar space and want to know how they came to be there. Molecules form most easily at high densities and moderately high temperatures. These conditions prevail both in envelopes around forming stars and also around evolved red giants. However, the matter going into star formation is mainly leaving interstellar space, while that from the red giants is going into space. Therefore the evolved red giants are potentially the source of interstellar molecules.

This paper will propose first that the chief interstellar solid molecules were formed in the atmospheres of red giant stars. Volatile solids that might condense in space do not seem to be a major constituent of the grains. Secondly it will be demonstrated that a major part of interstellar matter has probably come from the outer layers of red giant stars. Since the solids formed in these envelopes, it appears possible that less complicated gaseous molecules have also been ejected into space. Whether they are in fact the same molecules that are now observed is a question that cannot yet be answered.
Laboratory Studies of the Spectra of Interstellar Molecules
Authors: Herzberg G.
Published: March 2016

During the last twenty years many studies have been carried out in our laboratory which were aimed at establishing the exact positions of possible sharp interstellar lines of various diatomic and polyatomic molecules. In addition we have been trying to see whether the diffuse interstellar lines cannot be explained as produced by some molecule or molecular ion in the interstellar gas.

The present report is a summary of our recent work in this field.
Interstellar Molecule Formation; Radiative Association and Exchange Reactions
Authors: Klemperer William
Published: March 2016

The present report is a summary of a study, made in collaboration with P. Solomon, on the formation of interstellar molecules by radiative association and chemical reactions. The model to be discussed is limited practically to gas phase reactions in an HI region, where the principal constituents are atomic. It therefore is limited in scope and applicability. The role of the interstellar dust in this model is passive. It shields the region from radiation. Since a number of molecular species are dissociated by radiation and the extent of carbon ionization is determined by radiation, the radiation density is important in determining compositional equilibria.
Opacity Sources in the UV Spectrum of the Sun
Authors: Bonnet R. M. , Sacotte D.
Published: March 2016

In the past three or four years a great deal of attention has been given to the interpretation of the solar UV continuum. Several sets of intensity and limb-darkening measurements made from satellite, rocket and balloon borne instruments are now available, which allow comparisons to be made with theoretical computations. The main purpose of this paper is to discuss these comparisons, we restrict this discussion to the wavelength region between 3000 Å and 1680 Å, in which a significant difference between the observations and the computations still exists. The lines in this wavelength region which are of relevance to the continuum opacity are listed as follows:

the Ly-α line of neutral hydrogen at 1216 Å which appears as a strong emission line;

the resonance doublet of Mgװ at 2795 Å and 2803 Å which causes a broad depression in the solar continuum and shows an emission core similar in shape to the Ly-α line;

the auto-ionization doublet of AlI at 1932 Å and 1936 Å, which appears as two broad absorption features;

several absorption lines such as Mgi 2852 Å Sii 2881 Å;

many FeI and FeII absorption lines.

There are also several discontinuities in the continuum emitted between the lines in the spectrum between 1216 Å and 3000 Å. The most important ones are located at 2500 Å, 2085 Å and 1680 Å, which correspond to the photoionization edges of MgI, AlI and SiI respectively.
The Relative Intensities of Lines From Bel-Like Ions in the Solar Spectrum
Authors: Jordan Carole
Published: March 2016

The permitted transitions 2s21S-2s2p1P and 2s2p3P-2p23P in the Bel-like ions CIII, NIV and OV have been observed for some years in the solar spectrum (Hall et al., 1963). Recently, intensity data have also been obtained for the intercombination line 2s21S-2s2p3P1 in these ions (Burton et al., 1970). A large number of excitation rate coefficients are needed before the intensity ratios of these transitions can be computed and compared with those observed. These excitation cross-sections are now becoming available (Osterbrock, 1970; Eissner, private communication), and the present paper gives the results of an analysis of the intensity data. Figure 1 shows a partial term scheme for the Bei-like ions and the observed transitions.
Relativistic Contributions to Energies of Highly Ionized Atoms
Authors: Snyder Ralph
Published: March 2016

Historically, the first observation of a relativistic effect in atomic spectra was probably the discovery by Fraunhofer of the splitting of the Nai doublet in the solar spectrum. Thus theoretical understanding of these effects has long been important for interpreting astrophysical spectra, and it is especially important for the ultraviolet and X-ray spectra which form our subject today, for these often arise in highly ionized atoms. Because the relative importance of relativistic to non-relativistic terms is proportional to Z2, where Z is the nuclear charge, relativistic effects often play a major role in such atoms.
Relativistic Corrections to Atomic Energy Levels
Authors: Jones Michael
Published: March 2016

The relativistic effects on bound levels of atomic systems with particular application to systems of astrophysical importance are investigated by including the most important contributions to the low Z Pauli Approximation for the Hamiltonian. This work is an extension of a general purpose automatic computer program for calculating non-relativistic energy levels of complex atoms, described by Eissner and Nussbaumer (1969). The program should give fairly good intermediate coupling wave functions and it may thus be used as a basis for the calculation of intermediate coupling collision strenghts and oscillator strenghts. Numerical results are displayed for the Sodiumi sequence.
The Value of Photoelectric Occultation Timings in Lunar Motion Studies
Authors: Van Flandern Thomas C.
Published: March 2016

The two most important advantages of photoelectric timings of occultations over visual timings are accuracy and freedom from systematic error. The observational error is so small compared with uncertainties in the lunar ephemeris, star positions, limb corrections, and such, that the value of the observations will continue to increase as time goes on and the other error sources are eliminated.

A recent result made possible largely by the availability of photoelectric timings over the last 20 yr is a new value for the secular acceleration of the Moon, with corresponding consequences for the Ephemeris Time scale.

An important current application for simultaneous photoelectric and visual observations is the determination of ‘personal equation’ for the visual observers. Experiments so far indicate the visual observers require a minimum of 0.1 sec to detect that an event has occurred, plus additional time to react to it; hence, typical personal equations are around 0.4 sec.
The Investigation of Lunar Limb Structure by Means of Stellar Occultations
Authors: Evans David S.
Published: March 2016

It has long been recognized that the analysis of occultation traces from point source stars might provide a means of investigating the structure of the lunar limb on a remarkably small scale, certainly of tens of meters, possibly on a scale of meters.

The routine process of analysis of such an occultation trace produces a curve fitted to the standard model for a point source, in which the observed rate of fringe passage is matched to that computed from the rate and position angle of the relative motion of the moon with respect to the star background and the position angle of the point at which the occultation occurs. If θυ is the position angle towards which the relative motion of the lunar center takes place, θ that at which the occultation occurs, and ψ = θν — θ, then the predicted rate of the lunar limb perpendicular to itself at this point is

Rp = V cos ψ

where V is the velocity of the lunar center.
The Effects of Filters and Colour on Stellar Occultations and Appropriate Deconvolution Procedures
Authors: Krishnan T.
Published: March 2016

The theory of the effect of bandwidth of lunar occultations is reviewed. It is recalled that effective beamshapes can be calculated for symmetrical bandpasses and that their widths are related to the absolute width in wavelength of the bandpasses. Restoration with the second differential of the theoretical Fresnel diffraction curves at the central wavelength, at the correct rates, yield source distributions as viewed by these beamshapes. It is shown that for asymmetric bandpasses, the real and odd parts taken about the centroids lead to equivalent even and odd beams. Assuming an approximate color temperature for the stars, the total system response can be evaluated and hence the even and odd parts. Restoration of the data should then be performed using the second differential of the Fresnel curve at the centroid wavelength to minimize the odd part, adjusting zeroes, rates, and centroids by inspection. The even part should then represent the even theoretical response convolved with the one-dimensional stellar distribution, provided the latter is circularly symmetrical.

The technique is applied to the occultation observation of λ-Aquarii by Nather et al. (1970) leading to closely similar results.
Analysis of Lunar Occultation Data
Authors: McCants M. M. , Nather R. Edward
Published: March 2016

The technique of model fitting has been applied to the analysis of data obtained from photoelectric measurements of lunar occultations. A model occultation curve is generated and fitted, by least squares, to the observed light curve, and by this method the values of the model parameters are determined, together with their formal errors. This technique is contrasted with Scheuer’s deconvolution procedure by applying both methods to the same observed data.
Angular Diameters of the Red Giants 46 Leo and φ Aqr and Parameters of some Binary Systems from Occultation Observations
Authors: Poss Howard L.
Published: March 2016

Angular diameters of 0″.0056 ± 0.0011 and 0″.0049 ± 0.0008 have been calculated for the red giants 46 Leo and φ Aqr respectively from occultation observations. The occultation curves of α Lib and ε Cap show that they are binary systems. The separation of the components of the visual binary ε Ari, as calculated from its occultation curve, is 1.3 times its reported value. The occultation curve of α Leo shows distortion effects which are attributed to irregularities in the lunar limb.
Pulsars and the Origin of Cosmic Rays
Authors: Gold T.
Published: March 2016

The basic idea that pulsars may be the origin of cosmic rays arises when one realizes that they meet some of the criteria, perhaps not all as yet, for an origin theory of cosmic rays. Those criteria are: (1) there must be some possible mechanism that one can recognize for the acceleration of particles; and the pulsars have given us a very clear hint that particles are accelerated to at least the medium range of energies of cosmic rays - 1013 eV. (2) The objects that are thought responsible for cosmic rays must have enough total energy available to them to produce the entire cosmic ray beam in the Galaxy. I will come back to that, but it is clear that the total number of pulsars that one might expect in the Galaxy can indeed produce an adequate supply and even a good margin above that, if one makes the estimate on the basis of one plausible set of assumptions. (3) One would like of course that the mechanism proposed should generate the right spectrum; but there we as yet know too little. We do not understand what the energy spectrum of particles accelerated in pulsars should be, and we cannot as yet make any conclusive statement as to whether this spectrum can or cannot match the observed cosmic ray spectrum in the Galaxy. There is no reason for thinking otherwise, but there is no positive evidence in favor at the moment.

Then we have (4) the problem that the process selected must generate the correct composition. There we have the problem that we have just discussed, which is certainly a difficult one; I don’t know that it is completely clear what type of particles you must expect to come from pulsars; how much of the material accelerated in the vicinity of the pulsar is material that is being cycled into it at the time and going out again; and how much is material which is preferentially sucked out of the surface, perhaps by reason of a high charge-to-mass ratio.
Infrared Astronomy
Authors: Low Frank J.
Published: March 2016

The Earth’s atmosphere transmits infrared radiation through a number of windows. Table 1 lists the seven photometric systems in use at the University of Arizona which are chosen to fit the windows between 1·0 and 25 microns. An absolute calibration (Johnson, 1965; Low, 1966) has been worked out for each wavelength band and, for reference, we include an estimate of our current limiting magnitudes using a 60-inch telescope. At about 1000 microns, observations from the ground are again possible and both our group and workers in Russia (Fedoseev 1963) and England (Baldock et al., 1965) have succeeded in making observations of celestial sources. Between 25 and 1000 microns a few data have now been obtained from stratospheric altitudes by observers using jet aircraft (Low and Gillespie, 1968) and helium-filled balloons (Hoffman et al., 1967). We can anticipate that activity of this sort will increase greatly in the near future. At present, however, most of what we know concerning the nature of celestial objects at infrared wavelengths was obtained with ground-based instruments.
Some Problems and Instrumental Features of Submillimeter Astronomy
Authors: Salomonovič A. E.
Published: March 2016

Modern astronomy includes optical, ultraviolet, infrared and, in recent years, radio, γ-ray, and X-ray astronomy. Such a classification is justified to a certain degree. In fact, the difference in wavelength ranges causes a distinction in the methods and techniques of receiving radiation. Also, the solution of specific problems requires observation in different wavelength regions. In this respect it is possible to describe a new astronomical branch, the submillimeter one.

The submillimeter range is intermediate between the infrared and microwave regions, as shown in Table 1. The boundaries of this region are not very definite. Some authors include in the submillimeter range the wavelengths longer than 50 microns, others, those longer than 100 microns. The long wavelength edge of the range is also diffuse. Formally it is a wavelength of 1 mm, but in some cases the 2-mm or 4-mm wavelengths are also included in the submillimeter range. The measurements of submillimeter receiver performances are sometimes carried out at wavelengths up to 8 mm. The uncertainty of the boundaries is very understandable: their shifting depends on the methods of generation, transmission, and detection of radiation. In this review paper, following Martin’s (1962, 1963) terminology, wavelengths between 50 microns and 2 mm will be attributed to the submillimeter range.
A Cosmic X-Ray Survey in the Southern Hemisphere
Authors: Cooke B. A. , Pounds K. A. , Stewardson E. A.
Published: March 2016

An unstabilised Skylark rocket (SL 118) was launched from Woomera, South Australia at 20:20 local time on April 10, 1967. The rocket carried a large-area proportional counter to perform a high-sensitivity survey for cosmic X-ray sources in the Southern sky. The flight was successful and during the period of observation with the rocket above the absorbing atmosphere, from 80 to 350 sec after launch, a total of 50 scans across the sky were obtained. In addition to the predominant roll motion of the rocket, a slow precession about a flat (70° half angle) cone provided at least two separate looks at every part of the celestial hemisphere. At the time of the flight, the Milky Way was almost perpendicular to the horizon and a region around the Galactic equator from Scorpius to Taurus via Centaurus, Carina, Puppis and Orion was visible.
The X-Ray Spectra of Cygnus XR-1 and the Crab Nebula
Authors: Peterson Laurence E.
Published: March 2016

In this paper we wish to present briefly the latest results which have been obtained on the hard X-ray spectra of two strong sources in the Northern skies. These observations, which have been discussed in detail previously (Peterson et al., 1967), were made from balloons launched at Palestine, Texas, to 3 gm/cm2 atmospheric depth during September 1966. The Crab Nebula and the Cygnus XR-1 were observed to have a differential number power law spectra with an index of about –2 over the 20–200 keV range. Both sources have the same intensity within about 10%. The Crab Nebula has been observed on two occasions, one year apart, and showed no change in intensity over this range at about a 5% significance level.
Observations of Beryllium in Stars
Authors: Boesgaard Ann Merchant
Published: March 2016

Since a considerably higher temperature is necessary to consume Be atoms by (p, α) reactions than Li atoms, it has been thought that many clues to the understanding of the synthesis and destruction of the light elements could be found by studying Be abundances and the Li/Be-abundance ratios. Calculations have been made by Bodenheimer (1966) to determine the amount of convective depletion of Be during pre-main-sequence evolution. He found that a star reaching the main sequence at K5 would have destroyed 15% of its original Be; a K2 dwarf would have depleted its Be by 2%. For early K stars main-sequence depletion subsequent to this would be very slight. If there are no complicating effects such as magnetic fields and unusual patterns of circulation of stellar material, the observed Be abundances in stars of type G and earlier should be the initial pre-stellar or proto-star abundances. The BeII resonance lines lie far in the ultraviolet at λ 3131. But despite the very difficult nature of the observations, there are now Be abundances determined in about 60 dwarfs and sub-giants of types A, F, and G and in 2 K giants.
Preliminary Results of the Determination of Absolute Proper Motions of Stars Referred to Galaxies
Authors: Fatčihin N.V.
Published: March 2016

Absolute proper motions have been determined for 14000 stars in the 82 areas indicated in Figure 1. These proper motions result from measures made on 105 plate pairs taken with the Pulkovo normal astrograph which has a focal length of 3·5 m. The plates, which had an average epoch difference of 22·4 years, were measured film-to-film in a Repsold measuring machine. The number of galaxies used for defining zero proper motion was 271, and among the stars measured were 1283 from the AGK3. The probable error of a determination of proper motion from one plate pair was

The images of the galaxies were estimated as having an average quality of 6 on a scale of 10. (Deutsch et al., 1955).
Desiderata for Fk5
Authors: Fricke W. , Gliese W.
Published: March 2016

A fundamental catalogue compiled from independent and differential observations of stellar positions at various epochs provides the fundamental system of positions and proper motions of the stars. The system ought to be compiled in such a way that it represents the inertial frame of reference as accurately as practicable. Its direct purpose is to serve as the reference system of positional astronomy. It should fulfil the requirements of astronomical research, in particular in celestial mechanics and galactic research, as well as the demands of the astronomical determinations of time and of latitudes. It has also to fulfil the requirements of geodesy and navigation. For all these purposes the system must be uniform over the whole sky (free from regional systematic errors), and it has to be uniform over a large range of stellar magnitudes (free from errors depending on the magnitude of the stars).
Radio-Source Spectra and their Time Variations
Authors: Kellermann K.I. , Pauliny-Toth I.I.K.
Published: March 2016

During the past few years there has been a large increase in the available data on the spectra of radio sources, particularly at short wavelengths, where a number of sources have shown unexpectedly large time variations, with time-scales of 1 year or less.

The simple power-law spectrum, which is a straight line on a log-log plot of flux density against frequency, is shown by about 30% of sources. Most sources have a spectrum with negative curvature, which steepens at high frequencies. Many have a sharp cut-off, which is almost certainly due to synchrotron self-absorption, at low frequencies. In several of these sources, such as 3C 48, 3C 147 and 3C 295, the spectrum begins to flatten at a considerably higher frequency than the cut-off frequency. This flattening is too sharp to be caused by a change in the energy distribution of the electrons and is probably due to parts of the source becoming optically thick at higher frequencies. Some sources have components which are optically thick even at centimetre wavelengths. These must have angular sizes of 10−3″ or less. The energy density in relativistic electrons in these compact sources is much larger than the magnetic-energy density, so that the source cannot be stable and variations in the flux density are to be expected.
Hard Solar X-Ray Bursts
Authors: de Jager C.
Published: March 2016

A tentative spectrum of the Sun in the X-ray region is shown in Figure 1 (De Jager, 1967). The quiet Sun emits a measurable spectrum at photon energies below about 3 keV. During the occurrence of solar flares an enhancement of the emitted energy, and a hardening of the spectrum is clearly visible. The soft X-ray bursts apparently show a maximum radiation flux at wavelengths of about 10 Å.

In the spectral region above about 10 keV hardly any quiet solar radiation is observable. During the occurrence of solar flares hard X-ray bursts are occasionally observed. From the point of view of observational techniques these bursts may be divided in the so-called deka-keV bursts, covering the range 10-200 keV, and the deci-MeV bursts in the range between 0·2 and 1 MeV. Many deka-keV bursts have been observed during the years 1966-67 by Winckler et al., by means of the OGO-I and OGO-III satellites (see Arnoldy et al., 1967). The existence of deci-MeV bursts has been doubted various times (see e.g. Chubb et al., 1966). Its reality seems now to be proved (see also De Jager, 1967). However, they may be much rarer than the deka-keV bursts, although it is not yet completely sure that the selection is not observational.