bluuebunny/crossref_metadata_2025_split huggingface dataset:
9. Instruments and Techniques
Authors: Rösch J. , Nikonov V. B. , Babcock H. W. , Baum W. A. , Giovanelli R. G. , McGee J. D. , Meinel A. B. , Mel’nikov O. A. , Valniček B. 
Published: July 2016

Le présent rapport ressemblera peu à ceux présentés aux précédentes Assemblées Générales de l’Union; d’abord en raison des prescriptions du Comité Exécutif concernant la limitation du texte, la suppression des références bibliographiques et la latitude laissée au Président dans la conception même du Rapport; ensuite parce qu’il est apparu que la Commission 9 avait un rôle et une position assez différents de ceux de la plupart des autres Commissions et que l’un des points auxquels il convenait de s’attacher était précisément le re-modelage de son activité.Toutefois, un certain nombre de membres de l’Union ayant bien voulu résumer l’activité de leurs Institutions ou de leurs pays dans le domaine de l’instrumentation astronomique, leurs contributions trouveront place dans le présent Rapport et fourniront ainsi aux membres de l’Union une information non exhaustive mais cependant des plus utiles, en attendant que soit mise au point une nouvelle forme de documentation.Enfin, l’un des groupes de travail de la Commission - sur les Tubes à images - ayant poursuivi son travail de coordination et d’information comme par le passé, un rapport spécial sur son activité figurera à la suite du Rapport Général de la Commission 9.
Groupe de Travail Sur l’Emploi en Astronomie des Récepteurs Photoélectriques d’Images
Authors: Wlerick G. 
Published: July 2016

Un article de synthèse a été publié par Kent Ford en 1968 (1). De plus, le 4ème Symposium international sur les récepteurs photoélectriques d’images s’est tenu à Londres en Septembre 1968 et les comptes rendus des communications paraissent actuellement (2); il y sera fait référence par la mention (AE, page).Il est espéré que les travaux omis involontairement et les développements nouveaux pourront être présentés lors des séances de la Commission 9 à Brighton.Le rapport considère les trois types principaux de récepteurs: ceux qui emploient l’électronographie, ceux qui utilisent un écran fluorescent (convertisseurs d’images) et enfin les appareils de télévision.
Committee 3: Collision Cross Sections and Line Broadening
Authors: Seaton M. J. 
Published: July 2016

Two review articles have been published (1,2).1.1.Collision broadening by neutral atoms.The continued study of widths and shifts produced by neutral atom impacts at low densities has shown that the Van der Waals interaction ( — C6r−6)as used, for example, in (3), is an inadequate representation of the interatomic potential. The classical theory for a Leonard-Jones potential(C12r−12— C6r−6)has been developed (4) and subjected to experimental test (5). Further improvements result from introducing a term C8r−8in the potential (6) and from allowance for quasi-static effects (7). Applications to broadening by H—atom impact are discussed in (8).
20. Positions and Motions of Minor Planets, Comets and Satellites
Authors: Chebotarev G. A. , Edmondson F. K. , Arend S. , Herget P. , Hirose H. H. , Wood H. W. 
Published: July 2016

The Report in the part dealing with the minor planets and satellites has been compiled at the Institute of Theoretical Astronomy in collaboration of S. G. Makover (minor planets) and V. A. Shor (satellites). Contributions to this report have been received from S. Arend, H. Debehogne, J. Dommanget, P. Herget, S. Herrick, G. M. Jannini, B. G. Marsden, V. V. Michkovitch, B. Milet, Z. M. Pereyra, B. Popovič, E. Rabe, E. Roemer, J. Schubart, W. Strobel, C. Torres, H. Wood. The part on comets has been prepared by E. Roemer.The main feature of minor planet research during this triennium has been the further application of modern electronic computing machines to the practice of computing. The time has gone when the computations of orbits and ephemerides were performed with the aid of logarithmic tables or with desk calculators. Therefore it is no wonder that all computational work in the field of the motion of minor planets is nowadays concentrated in a limited number of institutions provided with powerful up-to-date computing techniques, like the following.(1)Institute of Theoretical Astronomy, Leningrad has used till recently a computer BESM-2 and now has at its disposal a new more powerful computer BESM-4.(2)The Observatory of Cincinnati has used till recently a powerful computer NORC. Unfortunately this machine has been nowadays dismantled, but the observatory can perform some kinds of computations with an IBM-360 computer.(3)Latvian State University, Riga, has made a large amount of computations with the computer BESM-2.(4)University of California, Los Angeles, makes a large amount of computations with its own computer.
25. Stellar Photometry
Authors: Cousins A. W. J. , Crawford D. L. , Argue A. N. , Golay M. , Hardie R. H. , Kron G. E. , Nikonov V. B. , Rybka E. , Stock J. 
Published: July 2016

During the past three years there has been increased activity in many fields where photometric methods are employed; more telescopes have been commissioned or adapted for photometric measurements and new magnitude systems have been proposed and tried, but much of the observing is now of a routine nature. Most of this continues to be done in the wide-band UBV system, but more measurements are now being made in the red and infra-red.More interest is being shown in narrower band-widths that emphasize particular features of a stellar spectrum, because these offer better prospects of separating the effects of temperature, luminosity, interstellar reddening, composition and duplicity. Attention has been given to finding the most useful bands and practical ways of measuring them, both photoelectrically and photographically.
Working Group for Research on Supernovae
Authors: Zwicky F.W. 
Published: July 2016

By October 1966, the number of supernovae in extragalactic systems which had been definitely identified was 184. During the following three years an additional 70 supernovae were discovered, bringing the total number by July 1969 to 254.The search for and the investigation of supernovae has been engaged in by an ever increasing number of observatories and astronomers, the majority of whom strongly support the continuation of the working group on supernovae and, until further notice, of the writer as its chairman.Circular letter No. 9 was issued to the members of the working group in June 1968, giving data on the supernovae Nos. 171 to 216. A catalogue-monograph on the supernovae found since 1885 is in preparation and should be ready for presentation at the 1970 IAU Assembly. In the meantime K. Rudnicki and A. Karpowiczowa have announced that the manuscript of their catalogue of supernovae, including all major bibliographic data has been sent to the printer.Two new approaches to the search for supernovae are in the first stages of realization, namely (a) automated searches by Professors Hynek and Colgate, the first having already resulted in 40000 bright galaxy reductions, the second being expected to start operation in the fall of 1969 and (b) the endeavours by J. Strong and F. Zwicky to have full-size objective gratings built for large (up to 50˝ apertures) Schmidt telescopes. With gratings of this type, supernovae to about mp = 16·5 may be discovered on single plates, the spectrum being observed at discovery.
8. Some new ionizing agents and properties of
the ionosphere
Authors: Krassovsky V. I. 
Published: July 2016

The instruments with which we have obtained our results are displayed at the Industrial Exhibition (in Moscow), and therefore I shall not describe them here. I shall state briefly the results of those investigations in the upper atmosphere which are related to the interplanetary medium and are therefore of interest to astronomers.We made an attempt to measure corpuscular fluxes by means of the third sputnik. For this purpose we used as indicators two fluorescent screens made of ZnS (Ag) (2 x i o - 3 g cm-2), covered with aluminium foil of different thicknesses (8 x i o - 4 g cm-2 and 4 x io~4 g cm-2). There were three aluminium diaphragms 5 mm thick in front of screens 5 cm in diameter. Each diaphragm had a window for capturing all corpuscles with a solid angle of 1/4 steradian. The emission of the fluorescent screens was detected by photo-multipliers. The electrical signals so produced were transmitted to a storage device and then to the Earth by a radio-telemetering system.
The UCAC as Input Catalog for FAME
Authors: Zacharias N. , Rafferty T.J. , Urban S.E. , Zacharias M.I. , Wycoff G.L. 
Published: July 2016

AbstractA new, highly accurate, astrometric star catalog is available from the U.S. Naval Observatory, covering ≈ 80% of the Southern Hemisphere to R ≈ 16m. The observing program is ongoing and full-sky coverage is expected by 2003. The final catalog will be used as the input catalog for the FAME space mission.
Intermediate Stars in Extragalactic Radiosource Fields: Astrometric Measurements
Authors: Birlan Mirel , Bocsa Gheorghe 
Published: July 2016

AbstractThe statistical analysis of the O – C and the standard errors for the astrometric RRS2 standard stars, and the analysis of the standard errors for the intermediate PIRS stars for 75 extragalactic radiosource fields are presented. This study was performed at Bucharest Observatory.
Report of the IAU Working Group on ‘Nonrigid-Earth Nutation Theory’
Authors: Dehant Véronique 
Published: July 2016

AbstractThe last precession-nutation model adopted by the IAU (International Astronomical Union) in 1980 is the nutation series built on Wahr’s Earth transfer function for the nutations of an oceanless elastic Earth (Wahr, 1979, 1981), and on Kinoshita’s rigid-Earth precession-nutation series (Kinoshita, 1977; Kinoshitaet al., 1979). The resulting precession and nonrigid-Earth nutation series have been used since that time and have been compared with observations. This comparison, which has been done by different teams all-over the world, shows that the theoretical series must be improved to meet observational precision. A Working Group (WG) was set up to examine the possibility of adopting a new nonrigid-Earth nutation series and to study the existing possibilities. On the one hand, the rigid-Earth nutation series have been improved (three new series) and the mutual differences have been shown to be less than a few hundreds of microarcseconds. On the other hand, new Earth transfer functions have been derived based on additional physical considerations within the Earth. The problem with these transfer functions however is that there is no reliable, independent information about the geophysical parameters needed to improve a theoretical model. Instead, the discrepancies with the nutation observations themselves are used to infer those parameters. Recent fits of geophysical parameters to the observed nutations have provided a series that is suitable for practical use, and is also a source of important information on the physics of the Earth’s interior. This paper reviews the recent work of the WG and establishes the reasons and criteria for the choice of the new model ‘IAU 2000’ which is proposed for adoption at the next IAU General Assembly.
The Study of Scattering Effects by VLBI Observations of PSR 0329+54 with HALCA at 1650 MHZ
Authors: Yangalov A.K. , Popov M.V. , Soglasnov V.A. , Semenkov K.V. , Hirabayashi H. , Liu X. , Wang N. 
Published: July 2016

AbstractPSR0329+54 was observed at 1.6 GHz with a space-ground radio interferometer with HALCA as a space radio telescope. The initial results of data processing are discussed.
Optimizing Pulsar Searches Against Propagation Effects
Authors: Cordes James 
Published: July 2016

AbstractPropagation effects are well known to limit the sensitivity of pulsar searches based on periodicity detections. I define several regimes for pulsar searches that are based on whether the search sensitivity is luminosity limited, dispersion limited or scattering limited. Consideration of these regimes allows general statements to be made about pulsar searches in and out of the Galactic plane. Telescope size matters, but only to a point. Once scattering becomes important it is better to search more sky (in a blind survey) than to integrate longer on a given sky position. Example surveys are described.
Studying Pulsar Emission Regions Using Interstellar Scattering
Authors: Gwinn Carl R. 
Published: July 2016

AbstractRadio-wave scattering in the interstellar plasma provides the means to circumvent the diffraction limit for earth-based instruments, and to image the emission regions of pulsars. For the past 25 years, observers have sought to exploit this fact to learn how pulsars shine. I review the techniques developed, and summarize measurements of size of emission regions of pulsars to date.
Examples of Extreme Intraday Variability
Authors: Kedziora-Chudczer Lucyna , Jauncey David L. , Wieringa Mark A. , Tzioumis Anastasios K. , Bignall Hayley E. 
Published: July 2016

AbstractWe present results of the ATCA IDV Survey of southern extragalactic radio sources. We discuss briefly the properties of the 22 new intraday variable sources discovered in the Survey. The follow-up observations of a few extreme examples of strong intraday variability are presented. We find that the characteristics of the total flux density fluctuations at different wavelengths are consistent with intersteller scintillations (ISS) of the microarcsecondsize soorten components. However, the scintillating components of a few extreme IDVs are characterized by the brightness temperatures far exceeding the TB = 1012 K limit. The relativistic beaming invoked in such sources would require Doppler factors up to as high as δ ~ 103.
An ESE Event for PSR 0329+54
Authors: Minter Anthony 
Published: July 2016

AbstractSpace Very Long Baseline Interferometry observations of PSR 0329+54 which, by luck, occurred during an interstellar fringing event, are presented. Separate images of the pulsar were not detected. However, the pulsar was observed to be extended. The size of PSR 0329+54 during this event is 1.88 × 1.67 mas with a position angle of 30° East of North. This could be due to two separate images of the pulsar separated by ∆θ ≲ 0.5 mas or angular broadening. The observed image size is larger than the expected angular broadening size of < 0.1 mas from the observations of Britton, Gwinn and Ojeda (1998).
The FAST/SKA Site Selection in Guizhou Province
Authors: Zhu B. , Nie Y. , Nan R. , Peng B. 
Published: July 2016

AbstractMany karst depressions with diameters of 300 m to 500 m, suitable for constructing Arecibo-style radio telescopes, were identified in the south of Guizhou Province by Remote Sensing (RS) and Geographic Information System (GIS) technologies together with field investigations. Fundamental topography and landform databases were established for 391 candidate depressions, and using GIS the 3-dimensional images of depressions, at a scale of 1:10000, were then simulated to fit a spherical antenna.
Five-Hundred-Meter Aperture Spherical Telescope Project
Authors: Peng B. , Nan R. , Su Y. , Qiu Y. , Zhu L. , Zhu W. 
Published: July 2016

AbstractA Five hundred meter Aperture Spherical Telescope (FAST) is proposed to be built in the unique karst area of southwest China, and will act, in a sense, as a prototype for the Square Kilometer Array (SKA). It will be over twice as large as the Arecibo telescope coupled with much wider sky coverage. Some results from site surveys for such a SKA concept are briefly reported. Technically, FAST is not simply a copy of the existing Arecibo telescope but has rather a number of innovations. Firstly, the proposed main spherical reflector, by conforming to a paraboloid of revolution in real time through actuated active control, enables the realization of both wide bandwidth and full polarization capability while using standard feed design. Secondly, a feed support system which integrates optical, mechanical and electronic technologies will effectively reduce the cost of the support structure and control system. Pre-research on FAST has become a key project in the CAS.
Analysis for Reflector Aluminum Mesh Panels of Five-Hundred Meter Aperture Spherical Telescope
Authors: Guoqiang Li , Liyuan Shen , Yongfeng Luo , Changgen Deng , Yamei He 
Published: July 2016

AbstractIn this paper, an analysis of the aluminum reflector mesh panels for the Five-hundred meter Aperture Spherical Telescope (FAST) is described. The study concentrates on one element of the reflector surface with the shape of a triangle. For the analysis, the panel is modelled as a mesh of cables so that it can be treated as continuous. It is demonstrated that the results so obtained are reasonable.
Structural Analysis of FAST Reflector Supporting System
Authors: Luo Y.F. , Deng C.G. , Li G.Q. , He Y.M. 
Published: July 2016

AbstractAccording to the deformation and movement requirements of the FAST reflector, a multipurpose analysis, including the load-bearing behavior, deformation, construction costs of the reflector supporting structure and its model, is presented in this paper. The advantages and disadvantages of steel and aluminum alloy structures are also discussed and compared through detailed design calculations under load-bearing capacity and normal working conditions.
Twenty-Five Years with SS 433
Authors: Chakrabarti Sandip K. 
Published: July 2016

AbstractSS 433 was catalogued twenty five years ago, and yet, very little is known about the true identity of the compact component. We present a brief review of the behaviour of this enigmatic object with a special emphasis on the more recent results and their interpretation. We also speculate on some of the properties of the observed jet components.
X-Ray Observations of SS 433: Review and Recent Results
Authors: Kotani Taro , Band David , Denissyuk Eduard K. , Kawai Nobuyuki , Kinugasa Kenzo , Namiki Masaaki , Safi-Harb Samar , Trushkin Sergei 
Published: July 2016

AbstractThe X-ray characteristics of SS 433 are reviewed together with results of recent multi-wavelength observing campaigns.
Three Incomprehensible Binaries
Authors: Eggleton Peter P. 
Published: July 2016

AbstractI describe three eclipsing double-lined binaries whose fundamental data (spectra, masses etc.) are totally out of line with theoretical concepts. Accepting the data at face value, they seem to imply that (i) a massive star (about 10 – 30 M⊙) in a moderately wide binary (P ≈ 50 – 250 d) can eject almost its entire envelope to infinity, without shrinking its period substantially, (b) some formerly triple systems can become binaries through the merger of two of the three components, and (c) a red giant can be stimulated to lose half its mass in a stellar wind before reaching its Roche lobe.
A Reprise of the Properties of the Exotic Eclipsing Binary RT Lacertae
Authors: Milone E.F. 
Published: July 2016

AbstractThe 5.07-d eclipsing system RT Lacertae is at the interface of Algol systems and RS CVn-type systems. Three strong lines of evidence support its Algolid nature: gas streaming; the close proximity of the larger star to its Roche lobe; and evidence of circumstellar material. Supporting the stellar activity model are moderately successful, if non-unique, modeling of light curve anomalies and ‘migration waves’ with star spot models, and a general expectation based on similarities to RS CVn-like systems. Recent work by Lanza et al. (2002) provides support for the latter class of models, but other light curve analyses and non-optical passband studies are examined below and directions for the resolutions of the problems and paradoxes presented by the RT Lac system are provided. An observational campaign to acquire simultaneous spectroscopic, photometric, and polarimetric data is suggested.
η Carinae – A Massive Star In Its Death Throes?
Authors: Humphreys Roberta M. , Davidson Kris , Smith Nathan 
Published: July 2016

AbstractThe very name of η Carinae conjures up the spectre of unsolved problems and challenging physics in the minds of many stellar astrophysicists. High spatial resolution spectroscopy and imaging of η Car during the past few years have answered some questions, but new and even more puzzling ones have appeared. In this review we highlight some of the recent discoveries and the still outstanding questions - what causes its 5.5 year spectroscopic cycle, what is the origin of its famous “great eruption,” and what is the underlying source of its instability?
Fluorescence Model for AG Draconis
Authors: Van Hamme W. , Wilson R.E. 
Published: July 2016

AbstractA fluorescent light curve model (ionization-bounded wind and chromosphere with scale height) that previously found most fluorescent variation in symbiotic nova V1329 Cygni to be chromospheric, is applied to AG Draconis, where the strong wind of a well-detached red giant is illuminated by ultraviolet radiation from an accreting white dwarf. Bandpass dependence of light curve amplitude is even more striking than in V1329 Cyg and eliminates thermal re-radiation from the red star photosphere as a principal variation mechanism, since thermal re-radiation cannot change by large factors from U to B to V. Spectra show strong continuum and line emission, so both light curves and spectra show the importance of fluorescence. A small secular decay was included by fitting in time rather than phase, with dTwd/dt as a parameter. There is a 3σ indication of a large negative dP/dt. Chromospheric fluorescence accounts for the entire U variation, while B and V variations are too small for wind and chromosphere to be distinguished. We confirm a previously identified 355-day radial velocity period that is consistent with red star pulsation.
Historic Spectra of Exotic Objects at your Fingertips: Raking up their Past
Authors: Griffin Elizabeth 
Published: July 2016

AbstractAstronomers possess a heritage of enormous wealth and potential: historic observations detailing the foundations of astrophysics, witnessing the observable universe decades ago, and recording any number of periodic or sporadic phenomena. If those observations were available on-line, what an enormous resource they would constitute for research. But they are not; they are on non-digital photographic plates, and we risk losing all that information for ever unless some measures are taken fairly soon to transfer it digitally to a more accessible medium.
Magnetic CVs in the UCT CCD CV Survey
Authors: Woudt Patrick A. , Warner Brian 
Published: July 2016

AbstractAn overview is given of all the magnetic CVs found in the UCT CCD CV Survey (Woudt & Warner 2001, 2002, 2003a). We have identified eight new candidate Intermediate Polars (IP), of which six are classical novae (RR Cha, DD Cir, AP Cru, V697 Sco, V373 Sct, and RXJ1039.7-0507). The two other candidate IPs are Aqr1 (2236+0052) and RX J0944.5+0357. In addition, there are two probable Polars, namely V351 Pup (= Nova Puppis 1991) and FIRST J102347.6+003841.
Magnetic Field Topology of Accreting White Dwarfs
Authors: Reinsch Klaus , Euchner Fabian , Beuermann Klaus , Jordan Stefan 
Published: July 2016

AbstractWe report first results of our systematic investigation of the magnetic field structure of rotating single magnetic white dwarfs and of white dwarfs in magnetic cataclysmic variables. The global magnetic field distributions on the isolated white dwarf HE 1045-0908 and the accreting white dwarfs in EF Eri and CP Tuc have been derived from phase-resolved flux and polarization spectra obtained with FORS1 at the ESO VLT using the systematic method of Zeeman tomography.