bluuebunny/crossref_metadata_2025 huggingface dataset:
27. Commission des Étoiles Variables
Authors: Shapley M. H. , Nijland M. A. A. , Ascarza MM. , Baldwin  , Banachiewicz  , Bemporad  , Blagg Mile , Blažko MM. , Brown A. N. , Campbell L. , Cannon Mile , Cox MM. , Danjon  , Roy De , Dugan  , Gerasimovič  , Graff  , Grouiller  , Guthnick  , Henroteau  , Hertzsprung  , Hoffmeister  , Jordan  , Kordylewski  , Kristensen  , Lacchini  , Ludendorff  , Luplau-Janssen  , McLaughlin  , Mascart  , Merrill  , Pickering D. B. , Prager  , Ryves  , Schilt  , Shinjo  , Silva  , Stebbins  , Stein  , Sternberk  , Strömgren E. , ten Bruggencate
Published: July 2016

Fourteen members of the committee have failed to respond to correspondence; nearly all of the others have expressed the definite opinion that non-responsive members should be dropped from committee membership when a new list is prepared a few correspondents indicating however, that the policy should be adopted for Commission 27 only if generally adopted for all commissions of the Union.
34. Commission de la Parallaxe Solaire
Authors: Jones M. H.Spencer , Camera MM. , Dyson  , Esclangon  , Hammond  , Hinks  , Kopff  , Schlesinger  , Schorr  , Stroobant  , Witt
Published: July 2016

1. Catalogue of Primary Reference Stars. Two lists of primary reference stars containing, in all, 821 stars were prepared by Prof. Kopff and published in Ast. Nach.224, No. 5375 and 226, No. 5403. These stars were widely observed at the following Observatories: Babelsberg, Cincinnati, Cape, Greenwich, Bergedorf, Heidelberg, La Plata, Leiden, Lick, Padova, Uccie and Washington. The stars were selected to give as uniform a distribution as possible to a distance of I° on either side of the path of Eros according to the preliminary ephemeris of Prof. Gustav Witt (Ast. Nach.224, No. 5375; M.N.R.A.S.85, 997, 1925). The early observations of Eros in the autumn of 1930 indicated that the actual path of Eros deviated considerably from the path indicated by this ephemeris and that the deviation near the time of opposition, when the motion of Eros was almost entirely in declination, would amount in R.A. to about 15 minutes of arc. The primary comparison stars as selected would thus extend on one side of the path, near opposition, to a distance of only 45’. This necessitated either (1) centring the photographic plates on the computed path of Eros, or (2) centring the photographic plates on Eros itself and selecting and observing sufficient additional primary comparison stars to cover the blank strip. It was finally decided to adopt the second alternative and a third list of reference stars, containing eighty-seven stars, was prepared by Prof. Kopff and published in Ast. Nach.240, No. 5756, with a recommendation that sufficient stars of the second list should be re-observed along with the stars of the new list to enable the new observations to be reduced to the system which Prof. Kopff had meanwhile derived from the observations of the two main lists.
Commission 6. (Telegrams.)
Authors: Strömgren E. , Roy Felix De
Published: July 2016

Sir Frank Dyson submitted the following resolution, which was seconded by Prof. Van Biesbroeck, and carried:

“The Commission recommends that the yearly subsidy of £66, granted since 1928 by the Union to the Central Bureau of Telegrams, be continued.”

The President described some proposals of modifications to the European code which he thought desirable. By using time instead of arc for Right Ascension, and Declination instead of Polar Distance, anybody receiving a telegram would be able to read it directly, without any computations, whereas its security would remain sufficient. This code is, in the main, similar to one which Prof. Förster had suggested many years ago.
Commission 12. (Solar Physics.)
Authors: St John C. E. , Minnaert M.
Published: July 2016

Dr St John explained why it would be necessary to reorganize Section 12. In the Committee there were too many members and too many sections. It was impossible for the President to write to 70 persons! At the request of the general secretary, propositions would be made for a fresh arrangement.

A first scheme was drawn up by Dr St John, Prof. Abetti, Prof. Brunner, Dr d’Azambuja and Dr Minnaert, in a preliminary meeting where they discussed the reorganization problem.
Commission 16. (Planets, Comets and Satellites.)
Authors: Phillips T. E. R. , Luplau-Janssen C.
Published: July 2016

The President referred to two matters left over from the meeting at Cambridge, Mass, in 1932, viz. (a) the formation of a small sub-committee on Martian Nomenclature, and (b) the appointment of a Secretary to deal with the work on the physical study of comets. He had requested Messrs Antoniadi, Lampland, and Maggini to form the Committee on Martian Nomenclature, but the question was difficult and complicated, and it had not yet been found possible to come to a conclusion apart from the acceptance of the nomenclature of Schiaparelli as an agreed basis.
Commission 30. (Radial Velocities.)
Authors: Plaskett J. S. , Adams W. S.
Published: July 2016

Section 1 of the Report was adopted without discussion save for the correction of a misprint.

The Report of the Sub-Committee on Standard Velocity Stars in Section 2 was discussed in some detail. The President read a letter from Dr Young urging the more systematic and frequent observation of such stars at different observatories. Dr Plaskett also referred to the desirability of the inclusion of more faint stars of early type, particularly of type A, in the recommended list.

Prof. Salet called attention to his investigations indicating the presence in the large Lick Observatory Catalogue of Radial Velocities of slight systematic differences between the values measured for stars near or far from opposition. It is important to learn whether such differences arise from the value of the constant of aberration or from flexure in the instruments employed. Prof. Salet expressed the desire that observers publish not only the mean values of the radial velocities but individual values, giving the dates and hour angles. Dr Beer supported this suggestion.
4. Commission des Éphémérides
Authors: Comrie M. L. J. , Fayet M. G. , Brouwer MM. , Brown E. W. , da Costa Lobo F. M. , Fukumi  , Herrero  , Kopff  , Leuschner  , Michkovitch  , Noumerov  , Peters  , Robertson  , Sadler  , Hansen Mlle Vinter
Published: July 2016

The agenda for the meeting in Stockholm are:

(1)

Report on the progress of the FK3 catalogue, and the volume of apparent places of the stars in this catalogue.

(2)

At the meeting in Paris it was suggested that the value of the Gaussian constant k should be fixed, and the President was asked to consult people known to be interested. As complete agreement appears to have been reached, the following resolution will be moved: “That the value of the Gaussian constant k shall be taken as 0-01720 20989 50000, the unit of time being the mean solar day for 1900·0”
16. Commission Pour les Observations Physiques des Planètes et des Satellites
Authors: Maggini M. M. , Andrea M.M. , Antoniadi  , Armellini  , Campbell L. , Delporte  , Dunham  , Hargreaves  , Harwood Mlle , Jarry-Desloges MM. , Lampland  , Link  , Luplau-Janssen  , Lyot  , Nicholson  , Peek  , Phillips  , Plakidis  , Quénisset  , Ross F. E. , Slipher E. C. , Wildt  , Wright F. E. , Wright W. H.
Published: July 2016

Depuis la dernière Assemblée générale, notre commission a eu le regret de perdre deux de ses membres les plus éminents: M. Paul Stroobant, directeur de l’Observatoire Royal de Belgique et M. W. H. Pickering, ancien directeur des succursales de l’Observatoire de Harvard à Arequipa (Pérou) et Mandeville (Jamaïque). Les recherches de M. Paul Stroobant se rapportent pour une grande partie aux planètes, notamment Mercure, Vénus, les petites planètes et Saturne dont il étudia pendant des années les anneaux. Il faisait partie de notre Union comme président de la 5e commission et membre de beaucoup d’autres.
Committee 5: Molecular Spectra
Authors: Phillips J. G.
Published: July 2016

The laboratory study of molecules of interest to astrophysicists has been progressing at a steady pace. A complete bibliography for the year September 1968 to September 1969, for instance, would show work on 68 molecules of possible interest; the diatomic and simpler polyatomic molecules. During this period 38 papers appeared on H2 alone, notably on its polarizability and the character of its spectrum near the ionization limit. Twenty-one papers on CO included studies in the vacuum UV, its Franck-Condon factors, chemiluminescence and IR absorptances. In the interests of saving space in this report, the detailed discussion of published work on each molecule of interest will be deleted. Instead, attention might be called to the fact that a complete card file bibliography is maintained by Phillips at Berkeley, and inquiries are welcome. In addition, a bi-monthly Newsletter is distributed from Berkeley in collaboration with S. P. Davis of the Physics Department.
17. La Lune (The Moon)
Authors: Dollfus A. , Mikhailov A. A. , Pettengill G. H. , Middlehurst B. , Kuiper G. P. , Menzel D. H. , Minnaert M. G. J.
Published: July 2016

Selon les instructions reçues de la part du Secrétaire Général de l’UAI, l’esprit général du présent “Draft Report” de la Commission 17 “La Lune” ne doit plus représenter, comme par le passé, un résumé des travaux effectués dans la discipline au cours des trois dernières années. Son rôle sera de donner un aperçu général sur les aspects et les tendances des recherches sur la Lune, la contribution présente et future de la Commission 17 du l’UAI dans son développement, ainsi que les coopérations dont elle est l’objet ou devrait l’être dans l’avenir.
Report of the Committee on Meteorites
Authors: Javnel’ A. A.
Published: July 2016

Several monographs and collections of papers were published in Meteoritics during 1967 to 1969 (Chirvinskij, 1967; Vdovykin, 1967; Wood, 1968; Cikulin, 1969; Anders et al, 1967; Stanjukovič, 1968). Extensive work on meteorites is continuing in the Meteorite Committee of the Academy of Sciences of U.S.S.R. Fesenkov and Krinov continued publishing the journal Meteoritika, where most of the papers of scientists of the U.S.S.R. are published. Hoffleit continued publishing Meteoritics of the Meteorite Society. Javnel’ continued editing a bibliography on meteorites. A bibliography on the isotopic and chemical composition of meteorites was published by Kielbasinski and Wanat. The UNESCO working group on meteorites under the chairmanship of Orcel edited the Directory of Meteorite Collections and Meteorite Research in 1968.

The Meteorite Committee of the Academy of Sciences of the U.S.S.R. organized its 13th meteorite conference in 1968. The Meteorite Society had its 30th to 32nd annual meetings during 1967 to 1969. The International Atomic Agency in cooperation with UNESCO and five other international scientific unions and organizations including the IAU represented by Millman, prepared a Symposium on Meteorite Research in Vienna, Austria, 7-13 August, 1968, initiated by the UNESCO Working Group on Meteorites. More than 70 papers were presented at this Symposium, showing the interests of various sciences in meteorites. The Symposium volume appeared very soon after the sessions were closed in the series Astrophysics and Space Science Library, published by D. Reidel Publishing Company, Dordrecht, Holland, under the title Meteorite Research edited by P. M. Millman (1969, 940 pages).
Report of the Committee on Variable Stars in Cluster
Authors: Sawyer-Hogg H. B. , Feast M. W. , Herbig G. H. , Rosino L.
Published: July 2016

Because of space restrictions, this report on the variable stars in clusters differs in form from those in earlier IAU reports, and is more condensed. Not all of the papers which have appeared since the last IAU General Assembly can be mentioned.

A definite trend is apparent in this field. A few years ago the aim of many programs was to detect new variables or to determine the periods of those known. While this is still being carried on, especially for the clusters in the far south, the emphasis has subtly changed to an avid pursuit of information about individual variables. For many variables, much more is known now than just the periodicity of their magnitude variations in photographic light. The number of observers studying these stars and the number of telescopes used in the program have greatly increased.
35. Stellar Constitution
Authors: Masevič A. G. , Schatzman E.
Published: July 2016

During the period under review, theoretical work in the field of stellar constitution and evolution of stars has been effectively continued by several teams permanently working in Belgium, Denmark, France, German Democratic Republic, German Federal Republic, Italy, Japan, Poland, the United Kingdom, the U.S.A., the U.S.S.R. as well as by individual scientists in Argentina, Bulgaria, Czechoslovakia, India, Sweden and others. Most attention has been given during the past three years to analysis of late stages of stellar evolution, rotation, evolution of binaries, loss of mass on various stages of evolution, stellar stability, neutrino astrophysics, physical processes in the presupernovae stage. The discovery of pulsars has raised extremely the general interest for white dwarfs and neutron stars, and consequently the number of papers with new hypotheses concerning quasi-stellar sources has substantially dropped.

Many new evolutionary sequences of stellar models for various masses and different chemical compositions have been computed using improved numerical techniques and large computing programs. It is regretted that many of these results are difficult to compare mainly because of the differences in the input physics and the way the numerical results are being published. This is a field in which a closer international co-operation is highly desirable, especially on the following points: exchange of ideas on the programs presently under way and the planned programs in order to avoid unnecessary duplications: agreement on the numerical results which should be published; exchange of technical informations: (input physics, computing methods, detailed results of computations, opacity tables, etc.). Several attempts in this direction have been undertaken during the period under review (for example, Commission 35 Circular Letters NN 1–7 containing information on current work, publication by the U.S.S.R. Academy of Sciences of the Cox and Stewart’s Opacity Tables for 23 mixtures, several joint international projects for using the same programs, etc.), but the problem still remains to be solved.
Working Group on Future Large Scale Facilities in Astronomy
Authors: Butcher H. R.
Published: July 2016

The idea for a Working Group (WG) on “Future Large Scale Facilities in Astronomy” grew from a discussion held on 20 August, 1994, during the IAU General Assembly in The Hague. The IAU Executive Committee approved its formation in August, 1995, and its composition in October, 1995. The WG will remain active at least until the XXIIIrd General Assembly in Kyoto in 1997. Members are: H. Butcher (Chairman), R. Ekers, B. Fort, N. Kardashev, M. Longair, F. Pacini, L. Rodriguez, G. Swarup, Y. Tanaka, H. Tananbaun, and L. Woltjer (ex officio). The WG carries out its work mostly by email and FAX.
Limits on Astrometric Accuracy
Authors: Fey Alan L.
Published: July 2016

A general overview of the various factors limiting the accuracy to which astrometric observations can be made is presented. Since this is a very broad topic, it is limited primarily to radio astrometry of extragalactic objects.
Densifying the Optical Reference Frame: The Tycho-2 Catalog of 2.5 Million Stars
Authors: Urban S.E. , Wycoff G.L.
Published: July 2016

Since the establishment of the Hipparcos Catalog as the defining source of the optical reference frame, densification beyond its ≈ 120,000 stars has been made possible by the utilization of the Tycho-1 Catalog. The ACT, combining the old Astrographic Catalog (AC) data with the Tycho-1 positions, is the best known example of this. The Tycho-2 consortium, led by E. Høg, has performed new reductions on the Tycho data. This not only has increased the astrometric and photometric accuracies of the original 1 million Tycho-1 stars, but also has added an additional 1.5 million stars. The U.S. Naval Observatory led the effort to compute the proper motions of these 2.5 million stars. They are based not only on the AC data but also include over 140 other ground-based catalogs, all directly reduced to the Hipparcos system. The result of these efforts is the Tycho-2 Catalog, available since February 2000. Positions, proper motions, and BT and VT magnitudes are given for 2.5 million stars. The catalog is 99% complete to V=11.0, and 90% complete to V=11.5. Positional accuracies at the mean epochs vary from < 10 mas for stars V < 9 to just under 100 mas for V > 12. Proper motion accuracies are estimated to be 1.3 mas/year to 3.0 mas/year for the same magnitude ranges. Photometric accuracies range from 0.02 magnitudes for the brightest stars to 0.25 magnitudes for the faintest.
Problems of Using Hipparcos Astrometry of Double Stars
Authors: Urban S.E. , Corbin T.E. , Wycoff G.L. , Mason B.D.
Published: July 2016

The current optical realization of the International Celestial Reference System is the Hipparcos main catalog in its entirety. This paper demonstrates that a subset of the main catalog stars — specifically those marked as double (“C” stars), acceleration solution (“G”), variability induced movers (“V”), and stochastic solution stars (“X”) — is of much lower quality than the majority of the catalog. Stars marked as suspected doubles (“S”) were investigated and found to show few problems. The authors have put forth a resolution (Resolution 2, this conference) to remove the C, G, V, and X stars, in addition to the Hipparcos orbit stars (“O stars”), from the optical realization of the reference frame.
Triangulation Measurements in the Solar System
Authors: Abalakin V.K. , Chubey M.S. , Eroshkin G.I. , Kopylov I.M.
Published: July 2016

The operational work of the Interplanetary Solar Stereoscopic Observatory (ISSO) may continue for 11 years. The ISSO Project is designed to insert two spacecraft (SC) into Lagrangian triangular libration points of the “Sun + barycenter (the Earth + the Moon)” system. The Project scientific program consists of two sets of experiments related to solar physics and to dynamical astronomy, respectively.

Various options of the astronomical observation program are possible. We discuss the option where the stereoscopic mode is applied to the direct triangulation observations of the solar system objects with respect to the ICRS coordinate frame.

The stereoscopic mode with the baseline equal to appears to be suitable for receiving the three-dimensional (3-D) measurement series for planets during the ISSO’s lifetime. Extended investigation of the planetary aberration based on the observations of major and minor planets, the direct distance determinations for minor planets and Kuiper’s belt objects, and the new set of star parallaxes may be used for constructing a new fundamental ephemeris and establishing an alternative scale of stellar distances. The accuracy of the angular measurements is expected to attain the milliarcsecond level.
Improvement of Nonrigid-Earth Nutation Theory by Adding a Model Free Core Nutation Term
Authors: Shirai Toshimichi , Fukushima Toshio
Published: July 2016

From the analysis of VLBI observational data compiled by USNO (U.S. Naval Observatory) from MJD 44089.994 to 51618.250 (McCarthy, 2000), we showed that a strong peak around –400 sidereal days in the spectrum of its differences from the IERS96 nutation theory could be explained by adding a model Free Core Nutation (FCN) term in the form of a single damped oscillation. Then we developed a new analytical theory of the nonrigid-Earth nutation including the derived FCN model. We adopted RDAN98 (Roosbeek and Dehant, 1998) as the rigid Earth nutation theory. It was convolved with a transfer function using numerical convolution in the time domain (Shirai and Fukushima, 2000). The form of the transfer function was the same as that of Herring (1995). However, its free parameters such as the complex amplitude and frequency of the FCN were readjusted by fitting to the above VLBI data. Even after truncating the forced nutation series so as to contain only 180 terms, the WRMS (Weighted Root Mean Square) of the complex residuals for the new nutation series is 0.312 mas, which is significantly smaller than 0.325 mas, that of the IERS96 nutation theory. As for the FCN term, we estimated its oscillatory period as –430.8±0.6 sidereal days, and its Q-value as 16200 ± 1600. Also we estimated the correction of the precession constants as −0.29297±0.00047”/cy in longitude and −0.02430±0.00019”/cy in obliquity, respectively.
Nonrigid-Earth Rotation Solution
Authors: Bretagnon P. , Rocher P. , Simon J.-L.
Published: July 2016

The accuracy of the rigid-Earth solution SMART97 is 2 μas over the time interval (1968, 2023). To obtain a nonrigid-Earth solution, we use the transfer function of Mathews (1999). The perturbations of the third component of the angular velocity vector are taken into account.
Advances in the Unified Theory of the Rotation of the Nonrigid Earth
Authors: Getino Juan , Ferrándiz José M.
Published: July 2016

Investigations of nonrigid-Earth rotation usually rely on the convolution of a transfer function with a rigid-Earth solution. A possible alternative is to develop a unified theory to encompass in only one body both rigid and nonrigid effects. It is represented in the Hamiltonian theory by Getino and Ferrándiz (GF). This theory combines the convenience of being a really analytical theory with good practical performance, since the residuals with respect to observations are also at the same ±1 mas level as the present IERS series.

We report on more recent results we obtained in the last year, not collected in the “Considerations” paper of the WGN (joint IAU/IUGG Working Group on Nutations).
Kinematical Relativistic Corrections for Earth’s Rotation Parameters
Authors: Brumberg V.A. , Bretagnon Pierre
Published: July 2016

Dynamical theories of the Earth’s rotation like SMART97 (Bretagnon et al., 1998) are to be considered in a DGRS (dynamically nonrotating geocentric reference system) (Brumberg et al., 1996). Such a theory gives the explicit expressions in terms of TCG (Geocentric Coordinate Time) of three Euler angles relating a DGRS to the ITRS (International Terrestrial Reference System). These angular quantities together with their TCG derivatives enable one to get all Earth’s rotation parameters. At the same time, the analysis of observations result in the values for slightly different angles and their TCG derivatives characterizing the relationship between the ITRS and a KGRS (kinematically nonrotating geocentric reference system). The differences between these two sets of six quantities represent kinematical relativistic corrections (due to geodesic precession, geodesic nutation and luni-planetary terms). The paper presents these differences computed by means of the VSOP87 series (Bretagnon and Francou, 1988). In particular, in analysing observations at the microarcsecond level these expressions will permit an experimental check of geodesic precession in a more direct manner than it is done nowadays (Bertotti et al., 1987).
Observational Model for Precision Astrometry with the Space Interferometry Mission
Authors: Turyshev Slava G. , Milman Mark H.
Published: July 2016

The basic astrometric observable of the Space Interferometry Mission (SIM) instrument is the pathlength delay. This measurement is made by a combination of internal metrology measurements that determine the distance the starlight travels through the two arms of the interferometer and a measurement of the white light stellar fringe to find the point of equal pathlength. Because this operation requires a non-negligible integration time, the interferometer baseline vector is not stationary over this time period, as its absolute length and orientation are time-varying. This paper addresses how the time-varying baseline can be “regularized” so that it may act as a single baseline vector for multiple stars, as required for the solution of the astrometric equations.
SIM Grid Star Observations: Astrometry with a New High Dynamic Range Imaging Device
Authors: Winter L.
Published: July 2016

First astrometric and photometric applications of the logarithmically scaled HDRC4 imager (developed by the Institut für Mikroelektronik Stuttgart, IMS, Germany) are presented. To test the HDRC4 imager at the telescope, a cooled camera had to be constructed by modifying a camera designed by IMS. First observations were performed with various telescopes at Hamburg Observatory, Germany. These showed the dynamic range to exceed 14 mag and the sensitivity to be comparable to that of the Kodak KAF 4200 CCD at a chip temperature of –35°C.
The Galactic Distribution of Electron Density Microstructure Inferred from Radio Scattering Observations
Authors: Cordes James
Published: July 2016

I first review the observables and optics of interstellar seeing associated with radio wave scattering in the interstellar medium. I then describe the Galactic distribution of electron density and its fluctuations, as inferred from a number of observables, including angular and pulse broadening, diffractive scintillations, and dispersion measures. Propects for improving the Galactic model are outlined.
On Post-SKA Radio Astronomy
Authors: Parijskij Yuri , Chernenkov Vladimir
Published: July 2016

It is suggested that the development of the SKA will drastically change the face of radio astronomy in the 21 st Century. A FAST-style SKA would admit observations of low contrast features, and would be the best design for studying the ‘dark ages’ of the Universe (x » 1) where sub-arcmin total power instruments can usefully be employed. To date there have been no proposals for post-SKA, billion square-metra instruments; we speculate that mobile communication systems can be used. In the very distant future, SKA multi-beam systems could be used to collect signals reflected by Solar system bodies such as the asteroid belt.
Modelling, Simulation and Testing of an Optomechatronics Design of a Large Radio Telescope
Authors: Duan B.Y. , Qiu Y.Y. , Su Y.X. , Wang W.L. , Nan R.D. , Peng B.
Published: July 2016

An innovative design for a feed support structure for the next generation large radio telescope, based on the idea of integrating mechanical, electronic and optical technologies (Optomechatronics), is considered. Theoretical analyses and simulations are carried out. A 5 m experimental model is built to demonstrate the idea.
Introductory Remarks
Authors: Eggleton Peter P.
Published: July 2016

Welcome to IAU Colloquium 187.
The Gamma-ray Large Area Space Telescope (GLAST)
Authors: Kotani Taro
Published: July 2016

GLAST, the next U.S. general gamma-ray astrophysics mission scheduled to be launched into low Earth orbit in April, 2006, for 5–10 years of operation, is described. A product of a NASA/DOE and international collaboration, the Large Area Telescope (LAT) is the primary instrument that covers the < 20 MeV to > 300 GeV band with an effective area > 8000 cm2. The angular resolution ranges from < 3.5° at 100 MeV to < 0.15° at 10 GeV. The GLAST Burst Monitor (GBM) consists of a group of NaI and BGO detectors to extend GLAST’s sensitivity to gamma-ray bursts to the < 10 keV to > 25 MeV band. GLAST’s localizations enables us to identify the X-ray, optical and radio counterparts of thousands of gamma-ray sources and to determine their nature.
Multiple Probes of the AS Cam Dynamical Problem
Authors: Van Hamme W. , Wilson R.E. , Branly R.M.
Published: July 2016

AS Camelopardalis is notorious for its apparent disregard for the theory of apsidal motion. The orbit of this 3.43-day double-lined eclipsing binary (B8V + B9.5V) rotates approximately 15° per century, which is only 0.3 to 0.4 as fast as predicted (classical + relativistic). Our dynamical program explores, as have others, the suggestion that a third star perturbs the orbit of the eclipsing pair and slows its apsidal motion, dω/dt. On the observational side, we unify the process of extracting apsidal motion and light-time effect parameters from eclipse minima by directly including a third body light-time effect along with the usual ephemeris parameters. By numerical experiment we identify third body parameters consistent with the eclipse timings and with the dynamics of third body perturbations. Results include the minimum third body mass required to produce the given retrograde apsidal rate. Finally, we use a general binary star light curve program that includes a light-time effect to solve for dω/dt and ephemeris parameters together with other quantities, combining 21 years of radial velocities and light curves within one coherent analysis. The program has an improved stellar atmosphere routine based on Legendre polynomials that have been fitted to Kurucz atmosphere models. By analyzing whole light curves, the program has access to more information than only times of minima. Results agree well with those from eclipse timings over 100 years and attain smaller standard errors despite utilizing only one-fifth of the traditional method’s baseline in time.
Strange Among the Strange: The B-emission Star γ Cassiopeiæ
Authors: Harmanec P.
Published: July 2016

γ Cas (HD 5394) is an important representative of Be stars, hot B stars exhibiting Balmer and other emission lines in their spectra at certain epochs. Its emission spectrum was observed as early as in 1863 and has undergone spectacular changes since then. γ Cas is also extremely interesting because it qualifies for several phenomenologically defined groups: it is a light and colour variable, long-term radial-velocity variable, X-ray source, IRAS source, rapid line-profile variable, a single-line spectroscopic binary and a central star of a reflection nebula.

A critical compilation of the wealth of observational data on the star, with emphasis on its time variability on several time scales, as well as an estimate of the most probable values of all basic physical properties of the object is presented. It is pointed out that in spite of a large quantity of data, systematic and well-calibrated observations are still rather rare. The present understanding of the object is put into perspective of the more general – and as yet unsolved – problem of the formation of Be envelopes.
Maser Emission from Icy Planets Orbiting Young Stars
Authors: Slysh Viacheslav
Published: July 2016

A model of maser emission spots as icy planets orbiting young massive stars is proposed. It is argued that the interstellar gas phase abundance of methanol, H2O and OH is much too low to produce maser emission from small gas clumps. The interstellar grains, on the other hand, consisting mainly of water ice and several per cent of methanol, can produce a favorable environment for the maser emission when evaporated. Big comets or planets covered by the water/methanol ice orbiting young massive stars can be the sites of the maser emission. The ice evaporates under stellar radiation, and water and methanol molecules emit corresponding maser lines, while OH molecules are produced from dissociation of water by the stellar radiation. VLBI observations of masers in W 3(OH), W 75N and V645 Cyg show that proposed planets are found in disks, and are moving on Keplerian orbits around O, B-stars. In the case of the O-star in W 3(OH) the planets are located beyond the compact HII region of the star. Extended envelopes of the icy planets provide molecular abundance, gas temperature and density adequate for the maser emission.
Be Binaries with Warm Dust and Exotic High-Luminosity A–F Emission-Line Stars
Authors: Miroshnichenko Anatoly S. , Bjorkman Karen S. , Klochkova Valentina G. , Chentsov Eugene L.
Published: July 2016

We present the results of photometric and high-resolution spectroscopic studies of a group of B[e] stars (Be stars with warm dust or B[e]Ds) and of two cooler objects with extremely high luminosities (HDE 331319 and IRC+10420). The B[e]Ds is a growing group of objects with very strong emission-line spectra, some of which show direct evidence of the presence of a hot and a cool star in the system. Their basic properties and connection to other groups of binaries are discussed, and a new list of members is presented. Fundamental parameters and chemical composition of an unusual F-supergiant HDE 331319 and recent results on a fast evolving object IRC+10420 are also reported.
The β Pictoris Disk: Peculiar or Just Young?
Authors: Lissauer Jack J. , Backman Dana E.
Published: July 2016

The star β Pictoris is not in itself very remarkable; however, it is surrounded by a dust disk that is much more prominent than any other main sequence star’s disk. The proximity of β Pic and the nearly edge-on viewing geometry of the disk enhance its appearance, but do not fully account for the disk’s prominence. While it is possible that β Pic’s disk is intrinsically unusual, a more likely explanation is that β Pic is simply a very young (~ 20 Myr old) main sequence star with a consequently denser second-generation debris disk remnant of its protostellar disk than possessed by older main sequence A stars.
Light Curve Changes in AH Cancri
Authors: Branly R.M. , Van Hamme W.
Published: July 2016

Light curves of the W Ursae Majoris binary AH Cancri obtained in 1973 and 1988 show a remarkable change in shape. Earlier curves have rounded minima and eclipses appear to be partial; later curves have flat-bottomed minima indicating total eclipses. The 1973 curves are consistent with a system in overcontact with an orbital inclination of approximately 65°. Such a low inclination, however, is incompatible with the -duration flat-bottomed eclipse seen in the more recent light curves. Intrigued by this puzzle we decided to make new photometric observations. We present CCD photometry in V and R obtained with the Southeastern Association for Research in Astronomy (SARA) 0.9-m and Buehler Observatory 0.4-m telescopes. We solve the new light curves and find a high-inclination (i ≈ 84°), low-mass-ratio (q ≈ 0.145) model fits the observations reasonably well. In the post-1988 light curves, limb darkening causes eclipses of the cooler star to be deeper than those of the hotter star. Times of minima suggest a possible third body interaction.
Looking for Twins of Przybylski’s Star
Authors: Hubrig S. , Cowley C.R. , Bagnulo S. , Mathys G. , Ritter A. , Wahlgren G.M.
Published: July 2016

The examination of high resolution spectra of two Ap stars, HD 965 and HD 217522, discloses a spectral appearance similar to Przybylski’s star. Here we present the preliminary results of a comparative study of all three stars. Further, we discuss the possibility of having a good spectroscopic indicator of magnetic fields in Ap stars. In all three studied stars the strong Lu II line at λ 5984 Å is present and very likely not affected by significant blends. Its hyperfine structure has been recently measured and we show the results of a model that accounts for the Paschen-Back effect on hyperfine structure.
Exoticism Among the Familiar and Bright
Authors: Griffin Elizabeth
Published: July 2016

The greater the spectroscopic detail observed, the more one appreciates that stars are individuals. Phenomena exhibited by bright stars illustrate some of the wealth yet to be unearthed – and explained.
Simultaneous Stokes Imaging and Doppler tomography of MCVs
Authors: Potter Stephen , Romero-Colmenero Encarni , Buckley David , Wood Derren
Published: July 2016

Stokes imaging uses polarimetric observations in order to image indirectly the accretion region on the surface of the white dwarf in magnetic cataclysmic variables (MCVs). Doppler tomography uses spectroscopic observations in order to gain insights into the velocity dynamics of the secondary star, and the ballistic and magnetically confined parts of the accretion stream. Until now, both of these techniques have been applied separately. We present and compare the results of applying both techniques to simultaneous spectroscopic and polarimetric observations of MCVs.
Dwarf Nova Oscillations and Quasi-Periodic Oscillations: Extension of the Two-QPO Diagram of X-Ray Binaries, and a new kind of DNO
Authors: Warner Brian , Woudt Patrick A.
Published: July 2016

Seventeen examples are given of Cataclysmic Variable (CV) stars possessing both Dwarf Nova Oscillations (DNOs) and Quasi-Periodic Oscillations (QPOs). These form an extension of the X-Ray Two-QPO correlation to frequencies three orders of magnitude lower. We draw attention to the existence of a second type of DNO in CVs, which is probably caused by magnetically channelled accretion onto the white dwarf.
RX J0524+42: A New Asynchronous Magnetic CV
Authors: Schwarz Robert , Schwope A. D. , Staude A. , Urrutia T. , Rau A. , Hasinger G.
Published: July 2016

Extensive optical photometry of the canditate magnetic CV RX J0524+42 has uncovered three persistent periods at 157, 146 and 136 minutes, which are the manifestation of the orbital motion of the system, the white dwarf spin and a possible side-band period of the latter. Depending on the interpretation of the 146 or the 136 minute period as the spin period, the system is an asynchronous by 7% or 14% (1 – PSpin/Porb), and therefore intermediate between the near-synchronous polars (< 2%) and the two DQ Her stars with long spin periods (EX Hya and V1025 Cen). Sampling the data over the beat period of 1.4 or 0.7 days reveals a prominent double-humped modulation on the spin period for certain fractions of the beat cycle. The phasing of this modulation strongly suggests that either pole switching onto two diametrically opposed accretion sites, or pole migration is operating in this system. With a period right within the period gap, RX J0524+42 is a key object for MCV evolution: it might be the first transition object between the DQ and AM Her subclasses where the white dwarf is currently in the process of synchronisation.
Fireballs, Flares and Flickering
Authors: Pearson K. J. , Horne Keith , Skidmore Warren
Published: July 2016

We review our understanding of the prototype “Propeller” system AE Aqr and we examine its flaring behaviour in detail. The flares are thought to arise from collisions between high density regions in the material expelled from the system after interaction with the rapidly rotating magnetosphere of the white dwarf. We show calculations of the time-dependent emergent optical spectra from the resulting hot, expanding ball of gas and derive values for the mass, lengthscale and temperature of the material involved. We see that the fits suggest that the secondary star in this system has reduced metal abundances and that, counter-intuitively, the evolution of the fireballs is best modelled as isothermal.
Earth rotation from a simultaneous reduction of LLR and LAGEOS laser ranging data
Authors: Shelus Peter J. , Zarate Nelson R. , Eanes Richard J.
Published: July 2016

As the techniques of lunar and artificial satellite laser ranging mature, emphasis is being placed upon the use of these observations to monitor the Earth’s rotation. It is important to note, however, that at the present time neither technique alone can furnish all three components of this rotation to an accuracy which surpasses those results obtained from classical techniques. In the case of LAGEOS laser ranging, unmodeled secular orbital effects couple with axial Earth rotation in such a way that these effects are not separable in the analysis of those observations. In the case of lunar laser ranging, observations have been regularly available only from a single station for the past ten years or so with the result that a change in latitude along the McDonald Observatory meridian is not separable into the ordinary (x,y) components of polar motion. The main purpose of this paper is to present the first stages of an investigation to combine LAGEOS and lunar laser ranging observations. It is hoped that the proper implementation of such a process might eliminate the shortcomings inherent in each technique, while accentuating the advantages of each. This has the potential of producing all three components of the Earth’s rotation to an accuracy and precision which is compatible with the present observational uncertainties.
Earth Rotation in the Erold Framework
Authors: Calame O.
Published: July 2016

The project EROLD (Earth Rotation from Lunar Distances) was conceived in 1974, in the COSPAR framework, with the goal of demonstrating that the lunar distances technique might be an efficient candidate in a new-generation service for the determination of Earth orientation.

Two years later, it was decided that the computations of the observational residuals and partial derivatives, as well as the analyses themselves, would be done at C.E.R.G.A. on a regular basis, for all the participating stations. Indeed, it was recognized to be important that all the observations be reduced in an homogeneous process. The target chosen for this program was that of Apollo XV which is the easiest to observe. Unfortunately, the operations could not start quickly due to a lack of observations and each station was encouraged to press the completion of the equipment, but many problems slowed the integration of these stations. Still now, only McDonald Observatory transmits observations regularly, and Orroral is operating, but with scattered results; presently this latter station is in course of modifications for improvement of accuracy.
On the Absolute Orientation of the Selenodetic Reference Frame
Authors: Kislyuk V. S.
Published: July 2016

The selection of selenodetic reference coordinate system is an important problem in astronomy and selenodesy. For the purposes of reduction of observations, planning and executing space missions to the Moon, it is necessary, in any case, to know the orientation of the adopted selenodetic reference system in respect to the inertial coordinate system.

Let us introduce the following coordinate systems:

C(ξc, ηc, ζc), the Cassini system which is defined by the Cassini laws of the Moon rotation;

D(ξd, ηd, ζd), the dynamical coordinate system, whose axes coincide with the principal axes of inertia of the Moon;

Q(ξq, ηq, ζq), the quasi-dynamical coordinate system connected with the mean direction to the Earth, which is shifted by 254" West and 75" North from the longest axis of the dynamical system (Williams et al., 1973);

S(ξs, ηs, ζs), the selenodetic coordinate system, which is practically realized by the positions of the points on the Moon surface given in Catalogues;

I(X,Y,Z), the space-fixed (inertial) coordinate system. All the systems are selenocentric with the exception of S(ξs, ηs, ζs On the whole, the origin of this system does not coincide with the center of mass of the Moon.
Preprint Databases at NRAO and STScI
Authors: Bouton Ellen , Stevens-Rayburn Sarah
Published: July 2016

A couple of different facts coalesced in the mid-70s that forced us to try to come up with a manageable scheme for handling preprints. First, as librarians at the National Radio Astronomy Observatory, we were charged with tracking papers by NRAO staff and by visitors using Nrao telescopes to provide an annual listing of staff and visitor publications and to aid in compiling statistics on telescope use.

Second, staff and visitors kept asking for preprints — by series and/or by author, subject, or cover color — and the number of preprint series being received had increased to the point where we could no longer always pull that information off the tops of our heads. So, after consulting with colleagues who had similar concerns, we put together a database in 1978, modestly based on the highly successful Preprint/Antipreprint lists produced by the Stanford Linear Accelerator Center. We decided to produce a biweekly list of new papers received and an as-needed list of recently published papers. The scientific staff were very enthusiastic from the beginning, seeing that our efforts would make their efforts to keep up with the literature that much easier.
An Observatory Publications Reclassification Project
Authors: Cummins Marlene
Published: July 2016

In our library we define observatory publications as all materials disseminated in serial form and on its own behalf, by an observatory, astronomical institute or university department. Included are annual reports, research reports, reprints, newsletters, and monograph series. Preprints, though fitting the description, are handled separately. Excluded and catalogued separately are individual monographs and users manuals. Sometimes items such as catalogues and atlases are catalogued and shelved elsewhere with a dummy left in the appropriate place.

Traditionally, libraries have shelved observatory publications alphabetically according to the city or town in which the observatory is located. Reference tools such as Astronomy and Astrophysics Abstracts and the Bibliography of Non-commercial Publications have used that arrangement too. One of the problems of this system is that without a number, it does not provide a single, unique, identifier for observatories with many locations. The same holds true in cases where there are many observatories in one location. In addition, the location may not be known or the library’s arrangement may have idiosyncracies.
Session 3 Overview: Management of Astronomical Pecularities
Authors: Hutchins Carol
Published: July 2016

Session 3 on “Handling and Use of Special Format Materials” dealt with diverse items which are of unique importance in astronomical libraries.

Preprints and reprints are important in several ways. Libraries’ collection and dissemination of information about pre-publication journal and conference papers boosts the astronomer’s awareness of current research in a timely fashion. Individual libraries’ practices range from very basic—the receipt and physical display of preprints—to the more elaborate activities including production of lists, gathering of subsequent publication information about the papers themselves, construction of local databases listing preprints, and electronic network exchange of listings.

There was a consensus that the sending of reprint series is far less important than it was in years past.

We heard a call for formal recognition or designation of a central clearinghouse for information about astronomy preprints.
SIMBAD: An Astronomical Database
Authors: Dubois P.
Published: July 2016

Simbad is the astronomical database produced and updated by the Strasbourg astronomical Data Center (CDS). Some guidelines are given how to retreive the astronomical information.
The Care of Obsolete Instruments
Authors: Vargha Magda
Published: July 2016

Hungary is a little country with old traditions. Hungarian celebrate the 950th anniversary of the death of the first king Stephan I this year. As regards astronomy, during the Renaissance in the court of the Hungarian king Matthias I there was a modest flowering in astronomy and this continued until 1526, when because of the Turkish occupation, the region was cut off and remained so for centuries. I do not want to list all the tragic historical events. Rather I would like to emphasize what we know by own experiences: what it means to reconstruct destroyed buildings and to try to collect valuable old items that are thrown away by guilty negligence.
Identifying Academic Physical Science Research in Progress
Authors: Primack Alice Lefler
Published: July 2016

For the scientist working on a research problem, books and journals serve mostly as archival records documenting what has been done and who did it. But the researcher usually has difficulty when he wants to determine what areas are currently being researched. Personal communication is a widely-used method of obtaining information, but one which is often inefficient and incomplete, especially as the number of colleagues working in a particular area of interest expands. Beyond this, current awareness of research in progress is available only by consulting an array of sources: preprints and lists or indexes of preprints, newsletters and annual reports, letters journals, reviews of research, directories of research grants, directories of graduate faculties or research facilities and their interests, indexes of theses and dissertations, indexes of progress reports, papers presented at conferences and lists and indexes of these papers, and lists of articles submitted or accepted for publication.