bluuebunny/crossref_metadata_2025 huggingface dataset:
46. Teaching of Astronomy
Authors: Müller Edith A. , Kleczek J. , Abell G. , Kharadze E. K. , Kononovich E. , Kourganoff V. , Minnaert M. , Routly P. , Schatzman E. , Swihart T.
Published: July 2016

During the 13th IAU General Assembly in Prague it was decided that each nation adhering to the IAU should be represented in Commission 46 by one member interested in the teaching of Astronomy. Six nations were already represented by the members of the Organizing Committee. For all other nations the Commission President contacted the head of the National Delegations to the IAU with the request to designate one IAU member of the particular country as member of Commission 46. With only a few exceptions every IAU member nation designated a representative in this Commission which now contains representatives of 33 nations. It is hoped that the missing nations in our Commission will also soon be represented by an IAU member active in the promotion of Astronomy education. Each member is responsible to (a) promote the teaching of Astronomy in his own country, (b) to keep in touch with the Astronomy teachers of his country, and (c) to communicate to the Commission President any programs and developments, problems and needs concerned with Astronomy education in his country. It is also hoped that institutions in countries not yet adhering to the IAU but which might wish to start some Astronomy teaching, could contact the Commission and, in some specific cases, could designate a Consulting Member to the Commission.
7. The Cepheid Distance Scale and Galactic Kinematic Parameters
Authors: weaver Harold
Published: July 2016

Cepheid variables have long been a primary source of knowledge of galactic distances. It is therefore important to examine critically the accuracy of the cepheid distance scale to determine whether it is adequate for present needs. Proper motions resulting from the solar motion provide a fundamental determination of the distance scale, according to the well-known formula
6. Rocket and satellite investigation of meteors
Authors: Nazarova I. N.
Published: July 2016

In the U.S.S.R. the study of cosmic rays by rockets was started in 1947. In the beginning, with the help of Geiger counters the number of charged particles was measured, and the formation of the electron-photon component in the interaction of primary particles of cosmic rays with nuclei of light elements was investigated. It was shown that in 1947,1948,1949 and 1951 the intensity of cosmic rays at altitudes up to 75 km was the same and did not change more than by 5 %. In 1949 the data on the photon intensities outside the atmosphere were obtained. In order to measure the number of high-energy photons, one of us (A. E. Chudakov) proposed a method permitting these measurements to be made with a strong background of charged particles.
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

A 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

The 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

The 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

PSR0329+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

Propagation 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

Radio-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

We 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

Space 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).
Investigations of AGNS by the Interplanetary Scintillation Method
Authors: Artyukh Vadim S.
Published: July 2016

This is a brief review of investigations of AGNs by the interplanetary scintillation method made in Pushchino Radio Astronomy Observatory.
The FAST/SKA Site Selection in Guizhou Province
Authors: Zhu B. , Nie Y. , Nan R. , Peng B.
Published: July 2016

Many 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

A 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

In 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

According 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

SS 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

The 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

I 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

The 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

The 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

A 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

Astronomers 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

An 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

We 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.
Multiwavelength observations of eclipsing polars
Authors: Schwope A. , Hambaryan V. , Staude A. , Schwarz R. , Kanbach G. , Steinle H. , Schrey F. , Marsh T. , Dhillon V. , Osborne J. , Wheatley P. , Potter S.
Published: July 2016

Multiwavelength observations of polars are essential for developing the big picture of these systems, particularly to gain understanding of the relevant accretion-induced heating and cooling processes. Eclipsing polars are prime targets for such studies since different radiation processes can be disentangled by observations with high-time resolution. We present a preliminary combined analysis of space-based observations (XMM-Newton, ROSAT, HST) with ground-based high-speed photometry (MCCP, OPTIMA, ULTRACAM) of DP Leo, HU Aqr and UZ For. We determine the location and extent of different emission components and find secular and short-term changes in the accretion geometries. We find displaced optical and X-ray emission regions in DP Leo and HU Aqr as well as mini-bursts and accretion arcs of variable size in HU Aqr. We report marked changes in the X-ray eclipse length of UZ For between high and low states.
The CHANDRA data of the Classical Nova RR Pic (1925): A possible Magnetic Cataclysmic Variable Candidate
Authors: Balman Şölen , Küpcü-Yoldaş Aybuke
Published: July 2016

During 25ksec of CHANDRA ACIS-S3 observations of the old nova RR Pic 1925 a count rate of 0.067±0.0017 c/s was detected. The results show evidence (spatial and spectral) for X-ray emission from the region around the prominent SW blob in the Hα images. Shell emission is detected with count rate ≥ (1.95±1.33)×10−3 c/s. The spectral analysis shows that the source spectrum can not be explained by a single or two temperature bremsstrahlung or VMEKAL models including photoelectric absorption, only models using powerlaw distribution of temperature fit the data well and indicate excess O, Al, Mg, S, and Si in the source spectrum. A soft excess in the CHANDRA data could be explained by a partial covering absorber model with covering fraction in a range 14-86 % consistent with characteristics of the Magnetic Cataclysmic Variable systems. The light curve shows significant orbital and other modulations.
The Near-Synchronous Polar Candidate V4633 Sgr (Nova Sagittarii 1998)
Authors: Lipkin Y. , Leibowitz E. M.
Published: July 2016

The classical nova V4633 Sgr (1998) exhibits two photometric periodicities. The shorter period (P1=3.01 hr) is stable, while the other one, longer by ~2.5%, has decreased monotonically since shortly after the nova eruption, with Ṗ2 ≈ –10−6 (Lipkin et al. 2001).

Here we report on results of photometric monitoring of the star in 2001 and 2002. During our observations, the longer period decreased more, and in 2002 it was only 1.8% longer than P1 The decrease rate (Ṗ2) in 2001-2002 was an order of magnitude smaller than in 1998-2000.

These new results support the Near-Synchronous Polar classification which was suggested for V4633 Sgr (Lipkin et al. 2001). In this model, the longer period of V4633 Sgr is the spin of the white dwarf, and its variation since 1998 reflects changes in the moment of inertia of the white dwarf, and angular momentum transfer in the system following the nova eruption.
X-ray broad band spectral Properties of Intermediate Polars
Authors: Matt Giorgio , de Martino Domitilla , Belloni Tomaso , Chiappetti Lucio , Haberl Prank
Published: July 2016

We summarize the broad band spectral properties of a small sample of bright Intermediate Polars studied with BeppoSAX.
Multi-epoch spectroscopy, photometry and polarimetry of the polar UW Pic
Authors: Romero-Colmenero E. , Potter S. B. , Buckley D. A. H. , Barrett P. E. , Vrielmann S.
Published: July 2016

Our multi-epoch observations show that UW Pic undergoes very pronounced changes in accretion geometry. We explain our observations in terms of changing accretion rates of UW Pic coupled with a particular orientation of the system to the observer.
Ultra-Short Period Double-Degenerate Binaries
Authors: Cropper Mark , Ramsay Gavin , Wu Kinwah , Hakala Pasi
Published: July 2016

We review the current observational status of the ROSAT sources RX J1914.4+2456 and RX J0806.3+1527, and the evidence that these are ultra-short period (< 10 min) binary systems. We argue that an Intermediate Polar interpretation can be ruled out, that they are indeed compact binaries with a degenerate secondary, and that the period seen in the X-ray and optical is the orbital period. A white dwarf primary is preferred, but a neutron star cannot be excluded. We examine the capability of the three current double-degenerate models (Polar, Direct Accretor and Electric Star) to account for the observational characteristics of these systems. All models have difficulties with some aspects of the observations, but none can be excluded with confidence at present. The Electric Star model provides the best description, but the lifetime of this phase requires further investigation. These ultra-short period binaries will be strong gravitational wave emitters in the LISA bandpass, and because of their known source properties will be important early targets for gravitational wave studies.
Unveiling the nature of the 321s Orbital Period X-ray source RX J0806.3+1527
Authors: Israel GianLuca , Stella Luigi , Covino Stefano , Campana Sergio , Marconi Gianni , Mauche Christopher W. , Mereghetti Sandro , Negueruela Ignacio
Published: July 2016

A nearly simultaneous X-ray/optical (Chandra and VLT) observational campaign of RX J0806.3+1527 has been carried out during 2001. These observations allowed us to phase the X-ray and optical light curves for the first time. We measured a phase–shift of ~0.5, in good agreement with the presence of two distinct emission regions and with the X-ray irradiation process predictions. The Chandra data allowed us also to study in details the X-ray spectrum of RX J0806.3+1527, which is consistent with a soft (kT<70eV) and small (RBB <20km) black-body component. We discuss the present findings in the light of the models proposed so far to account for the X-ray emission detected from RX J0806.3+1527, and its twin source RX J1914.4+2456.
Seth Carlo Chandler and the Observational Origins of Geodynamics
Authors: Mulholland J. Derral , Carter William E.
Published: July 2016

Geodynamics can be defined as the study of the motions of Earth with respect to its own center of mass and three locally-inertial directions. These motions include rotations of the whole Earth, as well as episodic, cyclic and secular deformations of the crust, and internal fluid circulations. Geodynamics is still largely an observational science, since there is yet no satisfactory theory to account for several of the most interesting of these motions. The observational aspects of geodynamics are basically astronomical, since the most obvious effects of terrestrial rotation and deformation (excepting of course occasional cataclysmic deformations) are seen as variations in the apparent positions of celestial bodies, as observed from the surface of the mobile, non-rigid Earth.
Optical Observations of Time and Latitude and the Determining of the Earth’s Rotation Parameters in 1980
Authors: Shu-Hua Ye
Published: July 2016

This paper is based on optical observations of 85 instruments (Table 1-a) from January to October 1980. The accuracies of all instruments, 62 for time and 54 for latitude, are shown in Table 1-b, in which:

–

the roughness ε1i of daily observations is defined by the standard deviation of the observation values of the i-th instrument with respect to the smoothed values of themselves;

–

the ε2i is the standard deviation of mean observation values during every 0.05 year with respect to the global reference system.

The average accuracy of each type of instrument is given in Table 2, regional averages are given in Table 3.

These tables show that errors in time observations are greater, generally speaking, than those in latitude, and low frequency errors are greater than high frequency ones in time observations.
Rotation of the Earth From Lunar Laser Ranging
Authors: Langley R. B. , King R. W. , Morgan P. J. , Shapiro I. I.
Published: July 2016

We have extended our estimates of variation of latitude and UTO from the McDonald Observatory lunar laser ranging (LLR) observations to span the period October 1970 to November 1980. The typical formal uncertainties of our values are about 6 milliarcseconds (mas) and 0.5 milliseconds (ms) of time, respectively. We have compared our values of variation of latitude with those derived from the smoothed Circular D pole positions published by the Bureau International de l’Heure. The root-mean-square (rms) difference about the mean difference is 14 mas. A comparison of our smoothed UTO estimates with those calculated from the smoothed Circular D values of UT1 and pole position gives a corresponding rms difference of 1.5 ms. For the period covered by the MERIT Short Campaign, we have also compared our smoothed UTO values with (unsmoothed) ones derived from daily UT1 and pole-position values obtained by the Goddard Space Flight Center / Massachusetts Institute of Technology / Haystack Observatory group from very-long-baseline interferometric observations spanning two one-week periods. The rms difference about the mean difference is 0.3 ms.
Intercomparison of Lunar Laser and Traditional Determinations of Earth Rotation
Authors: Fliegel H. F. , Dickey J. O. , Williams J. G.
Published: July 2016

The rotational orientation of the earth (UTO at McDonald Observatory) has been determined from lunar laser ranging (LLR) measurements for the interval 1971 to 1980. The results have been differenced from those obtained by conventional means as published by the Bureau International de l’Heure (BIH), on its 1979 system. The difference displays a quasi-seasonal signature, which we ascribe to systematic errors in the conventional measurements. The lunar data are well represented by a smooth curve, which gives UTO at McDonald with a precision of about 3/4 milliseconds or better, and UT1 to within 1 millisecond using BIH polar coordinates.
Comparison of Polar Motion Results Using Lunar Laser Ranging
Authors: Dickey J. O. , Fliegel H. F. , Williams J. G.
Published: July 2016

A comparison of polar motion results from three sources [Bureau International de l’Heure (BIH), Defense Mapping Agency Hydrographic/Topographic Center (DMAHTC-Doppler), the International Polar Motion Service (IPMS)] was performed using lunar laser ranging (LLR) data. The rms errors, both of the LLR data and of the determinations of polar motion by the three services, decreased in recent times. The BIH and Doppler polar motion are comparable in quality (12 ± 6 cm for BIH values taken from August 1976 through May 1980, 14 ± 7 cm for Doppler results taken from June 1977 through May 1980). The IPMS errors were substantially larger (33 ± 7 cm for data taken from August 1976 through May 1980). All three analyses give 13 ± 3 cm as an estimate for the combined LLR modeling, fitting, and instrumental error (noise) for the last four years.
Analytical Theories of the Motion of the Moon
Authors: Henrard Jacques
Published: July 2016

Almost every aspect of the analytical theory of the motion of the Moon has been reinvestigated lately. This paper is a review of these investigations.

The improvement upon the I.L.E. (the best known earlier theory based upon the work of Brown) is spectacular, but it is still too early to assess the exact value of these theories with respect to numerical integration.
Numerical Studies of the Lunar Orbit at Cerga
Authors: Calame O.
Published: July 2016

Until very recently the only available source of accurate positions for the Moon and planets were the american export ephemerides from JPL in particular DE86/LE40 which expired in May 1979 and then DE96/LE44 and DE102/LE51. Unfortunately, these ephemerides were constructed for various applications, but are not necessarily adapted for a purpose such as the EROLD program. Furthermore, these ephemerides are badly documented, which prevents having good homogeneity with the computations for the representation of the various motions of a lunar laser reflector with respect to a terrestrial station. Thus, in this framework, some other studies were useful.

A few years ago, we decided that it would be desirable to support the Lunar Laser data reduction with the construction of a new ephemeris by numerical integration. This was considered valuable not only from the scientific point of view, but also as an operational tool for the EROLD and MERIT programs. Early in 1980, we adopted this ephemeris, called ECT 18, in the EROLD computations for the Annual Reports of BIH and for the needs of MERIT Operating Center and Analysis Center at CERGA.
Report on the Discussions on Library and Information Services in Astronomy During IAU Colloquium 110 (Washington, D.C., 1988)
Authors: Wilkins G.A.
Published: July 2016

This report provides an overview of the presentations and summarises the discussions at IAU Colloquium 110, which was held in Washington, D.C., on 1988 July 26-30 and at the Goddard Space Flight Center on 1988 August 1. The topics included: the publication and acquisition of books and journals; searching for astronomical information; the handling and use of special-format materials; conservation; archiving of unpublished documents; use of computers in libraries; astronomical databases and various aspects of the administration of astronomy libraries and services. Particular attention was paid to new developments, but the problems of astronomers and institutions in developing countries were also considered.
Journal Costs: Journal Publishing as Part of a Society’s Operations
Authors: Boyce Peter B.
Published: July 2016

Scientific Societies have a broad range of goals, all aimed at advancing their area of science. Journal publishing is but one important task of a society. Subscription prices are normally set within the broad context of all the society’s programs. By using a normalization procedure it is possible to evaluate the relative costs and effectiveness of journals. Normalized costs to libraries of scientific journals vary by nearly 100-fold. In general, society published journals are very cost effective.
Foreign Astronomical Literature Acquisitions in China
Authors: Jinming Liu
Published: July 2016

Foreign astronomical literature acquisition in China is accomplished in two ways: (1) by exchange of publications between China and foreign countries, and (2) by purchase of foreign publications.
The Astronomical Publications in China
Authors: Jinming Liu
Published: July 2016

At present there are three different kinds of astronomical publications in China: journals, observatory publications and special publications.

Four journals are issued regularly: Acta Astronomia Sinica, Acta Astrophysica Sinica, Progress in Astronomy and Astronomy Amateur. There are five observatory publications available: Publications of Beijing Astronomical Observatory, Publications of Purple Mountain Observatory, Publications of Shannxi Astronomical Observatory, Publications of Yunnan Astronomical Observatory and Annals of Shanghai Observatory, Academia Sinica. Also several special publications have been published regularly, i. e. Chinese Solar-Geophysical Data (CSGD), Monthly Solar Activity, Time and Frequency Services Bulletin, Time Service Annual Report, etc.
The Revision of the Universal Decimal Classification for Astronomy
Authors: Wilkins G. A.
Published: July 2016

The Universal Decimal Classification system is widely used throughout the world for the arrangement of books in libraries and for the indexing of papers and reports as an aid to the retrieval of information. It is a comprehensive and language-independent system. The classification for astronomy and related topics (UDC 52) is used by many persons whose main interests are outside astronomy as well as by astronomical specialists. It is important that the classification be kept up to date, but the revision of UDC 52 is now overdue, as the last major revision was made in 1975 and published in 1977. It is clearly the responsibility of IAU Commission 5 to provide expert advice to the International Federation for Information and Documentation (FID) on the revision. Persons who are willing to participate in the work of revision are invited to write to the author, who is the current chairman of the relevant revision committee.
T-Rex: A Cooperative Thesaurus Building Project for the International Astronomical Union
Authors: Shobbrook Robyn M.
Published: July 2016

Astronomers and librarians have been experiencing difficulties in keeping up with the amount of published literature. The astronomer tries to keep abreast in his particular field and the librarian in the management, control and retrieval of scientific information. The 1980’s have seen a revolution in the methods for information storage and retrieval and in particular the advent of the online database. The speed of processing information for storage has been embraced by all, however little thought has been given to how we shall achieve effective high precision recall of documents.

Many librarians firmly believe the best road to success in information retrieval from automated systems is provided by vocabulary control. Contrary to belief, free text or natural language searching alone does not lead to high precision recall. Consistency and integrity of the online catalogue can only be achieved with the addition of a controlled vocabulary. With today’s technology it is possible to maintain the best of both worlds. The controlled vocabulary is used to index the major concepts of a given document over and above the natural language used within the document.
The Union list of Serials in Astronomy Libraries of the UK
Authors: Macdonald A.R.
Published: July 2016

The compilation of a common listing of the serials holdings of the main astronomy libraries in the UK was proposed at the first Meeting of Astronomy Librarians of the UK held at the Institute of Astronomy in Cambridge in March 1980. The Library of the Royal Observatory in Edinburgh was at that time already engaged in a project to catalogue its serials holdings and at the same time to compile a separate, briefer, computerised listing for use in the library. Although the original idea had been that the proposed union list should record only the astronomy serials held by the participating libraries, the Royal Observatory Library offered to assume responsibility for the project as a natural development of its own list and to construct a union list that would record the complete serials holdings of all the participating libraries as it was felt that this would be of even greater benefit to these libraries.
Preprint Information Service at the Raman Research Institute Library
Authors: Ratnakar A.
Published: July 2016

An important channel of communication in many scientific fields is “Preprints.” The Astronomical Community uses this method very effectively for speedy communication. One of the main reasons for the prevalence of this practice in Astronomy is to reduce the time gap between the submission of an article and its actual publication in a scientific journal. Preprints are circulated by Astronomers among their colleagues. Libraries receive preprints either from authors or from institutions at which the authors are working.
Handling of Preprints
Authors: Gómez M. E.
Published: July 2016

At La Silla, we receive on average between 90 and 130 preprints a month from institutions all over the world. The preprints are extensively used by our staff as well as visiting astronomers who come to perform observations at La Silla. Most of the preprints are received as donations, others are requested directly from the publishing institute.

The European Southern Observatory has among other publications, its ESO Scientific Preprints. At La Silla, the library does not deal with the distribution of these preprints, since this is made directly from ESO in Garching, FRG.
Non-Printed Materials
Authors: Jaschek C.
Published: July 2016

Many modern catalogues and/or observing lists are too large for easy printing in a magazine, or have too short a life to be economically worth printing as a catalogue or a book. We have therefore two ways of presenting them:

(a)

on microfiche

(b)

on tape (or diskette).

One could add computer print-outs, but by experience there are mostly made for private use.

Microfiches have never become very popular, although they are quite handy for long catalogues. The Henry Draper catalogue, weighting 10 kgs occupies 14 microfiches weighting 42 grams and can be accommodated in a common envelope. Durability of good microfiches is guaranteed for several decades and its price is cheap. Except thus for the reading device, which is bulky, the microfiche is a handy way to store information, especially when only small amounts of information are to be retrieved.
Observatory Publications and their Significant Role in Astronomical Libraries
Authors: Kaminska Kinga
Published: July 2016

The Library of Warsaw University Observatory is a small one, but it is one of the oldest astronomical libraries in Poland. The library collection has been gathered almost since the beginning of the Warsaw Observatory, that is since 1825. Although a large part of our collection was burned during the Second World War, the remaining part contains many unique items. Scholars doing research in the area of the history of astronomy often find our collection very helpful in their work.

Observatory publications play a significant role in my library. In general, we have limited possibilities for buying publications with hard currency. Therefore, any free publications obtained by my library constitute an extremely valuable source of information about new research and discoveries all over the world.
Observatory Publications in the Small Institute Library
Authors: Fishburn Anne M.
Published: July 2016

I can imagine that many of us here represent a small institute library, and we can only look with wonder and envy at the vast collections of the US Naval Observatory and other such large and long-established libraries. We have a library of approx. 10 000 monographs, 13 000 bound serial volumes, 200 current serial titles and a report/observatory publications collection which grows at the rate of about 650 items per annum. In addition we receive about 800 - 1000 preprints a year. We have a staff of 2 and 2 halves. One of our part-time people deals almost exclusively with the ordering and distribution of our Extraterrestrial preprints, reports and reprints.
Correspondence, Unpublished Papers and Data: Comments on Modern Use of Old Archives
Authors: Debarbat Suzanne
Published: July 2016

For a scientific or historical purpose, nowadays astronomers may need to use documents of the past. On can assume they are then, in a situation similar to the one that next centuries searchers will have to face, when using present time documents we will have left them. So, actual experience may help to know what to do or what not to do, dealing with the contents of future archives.

In astronomy, the most important variable is time. Since in this field, no experiment can be made, the astronomers must watch the universe and an essential task is to observe. Starting from observations, they will set up theories through analysis, treatment, interpretation, or else, starting from theoritical work, they will check their conclusions by comparison with observational data.
Computer System of Library Management and Information Retrieval at the Shaanxi Astronomical Observatory
Authors: De-he Li , Ya-hong Wang , Fa-kuan Dang , Jun Chen , Feng-xiang Chen , Yu-lian Wang , Qiu-ju Xu
Published: July 2016

For modern management and full resource sharing among libraries and scientific departments both in Chinese and worldwide observatories, we established the computer system of library management and information retrieval during the period 1984-1987.

The system is composed of ten component sub-systems:

1.

Book ordering system. This system can produce orders for books and periodicals, balance accounts, produce statistics as well as claims for outstanding book orders.

2.

Book cataloguing system. This system can catalogue books under certain rules while appending new records of books to the databases. It can also produce catalogue cards and produce written reports about the new books.

3.

Book retrieval system has the ability to search for a specific book in several ways.

4.

Book lending or circulation system. This system is a complete circulation system; including book lending, renewals, waiting lists, and recall of borrowed books.

5.

Periodical management system. This system is in charge of processing of periodicals and magazines in the library, including cataloguing, management, and lending.

6.

Scientific information retrieval system. One can retrieve scientific information by keywords or in many other ways.

7.

Internal material booking system. It can make orders of internal materials, claims for materials outstanding and make exchanges with other observatories and institutions both in or outside the country.

8.

Internal material management system. It can do the work that is analogous to that done with books and periodicals.

9.

Information relationship system. It handles exchanges of information between institutions. Computer system of library management ... at Shaanxl 183

10.

Scientific information network management system. It manages affairs within a certain information network.
Resource Sharing and Cooperative Activities in Astronomical Libraries
Authors: Lastovica Ethleen
Published: July 2016

The Shorter Oxford English Dictionary defines “resource” as ‘A means of supplying some want or deficiency; a stock or reserve upon which one can draw when necessary’. The Collins English Dictionary further defines “resources” as ‘a source of economic wealth especially of a country or business enterprise (capital,equipment,personnel,etc.)’.

The essential theme of this Workshop is resource sharing because it has been organized to provide an opportunity for librarians of astronomical observatories and institutions to meet to discuss common problems and ways of stimulating greater cooperation between libraries in different countries. The White House Conference on Library and Information Services held in 1979 outlined the justifications for resource sharing by stating:... ‘resource sharing is now mandated by the information explosion, the advance of modern technology, the rapidly escalating costs of needed resources, and the wide disparity between resources available to individuals by reason of geographic location or socio-economic position’.
An Astronomical Software Documentation Collection at the Smithsonian Astrophysical Observatory
Authors: Rhodes Carol , Kurtz Michael , Rey-Watson Joyce
Published: July 2016

We have established a library collection of documentation for software used in the reduction of astronomical data. We make some recommendations to the authors of documentation in addition to discussing the future directions of this collection. Instructions on how to contribute to and access this collection are provided.
Physics and Mathematics Acquisitions in French Libraries Specialized in Astronomy: Some Comments
Authors: Vin M.J. , Motais de Narbonne A.M.
Published: July 2016

The importance of physics and mathematics in astronomical research has been growing for the last twenty years; yet, the volume of book acquisitions in the relating fields has been decreasing in most french libraries specialized in astronomy (graph 1).

Great are the consequences of the physics book high prices (graph 2) on the acquisition volume and more drastic is the selection when the total amount of acquisitions is low, i.e. in small libraries (graphs 3 and 4). Yet, the restriction of acquisitions has not generated increasing inter-library loans in the relating fields and national service (CADIST) acquisitions in physics and mathematics have also been dropping. This point, connected with the concomitant general growth of astronomical book accessions, leads us to explain the contradictory observations as mentioned above here from the astronomical publication contents.
Light Pollution – A Problem for All of Us
Authors: Crawford David L.
Published: July 2016

Light Pollution is a severe problem for amateur and professional astronomers, and, indeed, for the general public. All these suffer from a lack of awareness of the issues, however. Poor quality outdoor nighttime lighting has several major problems: light trespass, glare, clutter and confusion, urban sky glow, and energy waste. There are solutions to the light pollution problem, most involving the use of better quality lighting. We all must educate our colleagues and the public about the issues, and push for solutions. Quality lighting is compatible with dark skies, and with energy savings. Our view of the universe, as professionals and as the public, and our children’s, depends on our being successful.