bluuebunny/crossref_metadata_2025_split huggingface dataset:
XXXII.—On the Harmonic Analysis of certain Vowel Sounds
Authors: Jenkin Fleeming , Ewing J. A. 
Published: July 2016

The permanent record obtained with Mr T. A. Edison's phonograph has afforded a new opportunity of investigating the nature of spoken sounds, and the method which this invention placed at our disposal appears to us to possess several important advantages.This method consists in obtaining a magnified transcript on paper of the indentations impressed by spoken vowels on the tinfoil of the phonograph, and then subjecting the periodic wave-forms thus obtained to harmonic analysis.The curves as drawn in ink on paper represent to a large scale the surface of a longitudinal section of the tinfoil made along the centre of the furrow impressed by the pricker of the phonograph. The forms impressed on the tinfoil depend essentially on the movement which a particle of air performs when the given sound is being uttered, and the harmonic constituents of each period of the continuous wave-form indicate the relative proportions in which the prime tone and its harmonics are present in the sound.We thus obtain what may be called a harmonic analysis of the vowel sounds.
Hands-On Astrophysics: Variable Stars for Astronomy Education and Development
Authors: Mattei Janet A. , Percy John R. 
Published: July 2016

AbstractAmateur astronomers, and students, can contribute to astronomical research by measuring the brightness of variable stars. Hands-On Astrophysics (HOA) is a project which uses the unique methods and the International Database of the American Association of Variable Star Observers (AAVSO) to develop and integrate a wide range of science, mathematical and computer skills, through the measurement and analysis of variable stars. It is very flexible and can be used at many levels, in many contexts — for classroom use from high school to university level, or for individual projects. In this paper we describe HOA, and how it can be used to promote international astronomy education and development, through research-based science education.
Astronomy in Algeria: Past and Present Developments
Authors: Irbah Abdenour , Abdelatif Toufik , Sadsaoud Hamid 
Published: July 2016

AbstractAstronomy studies have been developed in Algeria since 1890 when the Algiers Observatory was built. Several instruments were soon installed on the site and have contributed to many scientific projects such as the international sky-map program. However, the observatory activities were suddenly interrupted by the departure of all French astronomers in 1962. Twenty years were needed before new astronomy programs were developed at Algiers observatory. They are principally based on imaging through atmospheric turbulence, solar physics and studies of pulsating variable stars. Only one observational program, however, has so far been developed. This consists of solar observations in the framework of an international program to survey the Sun’s radius. The astronomers now form a relatively important team since more than twelve researchers have permanent status. This is a good start taking into account the fact that astronomy is not taught in Algerian universities. We will begin first by giving an overview of the history of Algiers Observatory, including its instrumentation. We will then present the existing Algerian team and all their current scientific work and proposed projects.
The Choice of Small Telescopes
Authors: Crawford David L. 
Published: July 2016

AbstractSmall telescopes can be powerful tools for astronomical research. Many are being used by professional and amateur astronomers to do important, even frontier, research. They are also extremely valuable tools for education. This paper discusses the characteristics of such telescopes, and it makes recommendations about items such as field of view, focal length, and so on. It also discusses a few small telescopes representative of what is currently being done. Astronomy needs such facilities as much as it needs the giant telescopes. They complement each other very well.
What Can be Done with Small Telescopes?
Authors: Soonthornthum Boonraksar 
Published: July 2016

AbstractModern astronomy has developed rapidly in the last few decades. Large telescopes, several metres in diameter, have been constructed and installed at many sites around the world, in order to carry out high-quality research work at the frontiers of astronomy. In many parts of the world, only small telescopes are available, because of budgetary limitations and the stage of development of science in the country. However, much effort has been put into using these small telescopes to the best of their capabilities. A small telescope with modern detectors can do good astronomical research. Sirindhorn Observatory, Chiang Mai University, is the only observatory in northern Thailand which plays an active role in astronomical research. The major instrument is the 40-cm Cassegrain reflecting telescope with standard wide-band and intermediate band photoelectric photometers, CCD photometers and a CCD spectrograph. Because of Thailand’s hot and humid climate, the telescopes and detectors at Sirindhorn Observatory need regular maintenance. Major research at the Observatory emphasizes the study of physical propoerties and evolution of close binary systems, especially near-contact and contact binaries, by photometric techniques. Networks in this field of research have been established through national and international collaboration with some astronomical institutes in the region. A larger telescope is being developed for more efficiency in operation; it is expected to be able to serve the future development of astronomical research in Thailand.
Third-World Astronomy Network
Authors: Narlikar Jayant V. 
Published: July 2016

AbstractSeveral developing countries of the Third World have been actively interested in astronomy, as is evidenced by the membership of the IAU. The enthusiasm of individual astronomers from these countries is, however, not matched by the resources available to them to pursue their interest in astronomy, in teaching as well as research, at an above-threshold level. Major problems requiring solutions are (i) isolation from the mainstream work, which leads to research work which is not quite relevant or realistic, and to teaching based on outdated knowledge; (ii) lack of financial resources, leading to shortage of books and journals in the library, insufficient computing power, out-of-date instruments, as well as inability to participate in essential activities like schools, workshops, and major international conferences and symposia; and (iii) lack of hands-on experience with state-of-the-art instrumentation that often leads to good scientists being turned away from astronomical observations towards abstract theories.Experience of the International Centre for Theoretical Physics at Trieste, Italy and of the inter-university centres in India, like the IUCAA at Pune, has shown that limited resources can be made to go a long way by sharing, networking and intelligent use of communications technology. Based on the above experience, this proposal envisages setting up a Third World Astronomy Network (TWAN) under the auspices of the IAU, within the wider ICSU-umbrella with support from the UNESCO as well as participating nations. The TWAN will operate with a few key institutions as local nodal points of a wide network. The objectives of the proposed TWAN and the role of the Nodal Institutions (NIs) are spelled out in this proposal, along with the budgetary support required.
Commission 31: Time: (L’heure)
Authors: Petit G. , Matsakis D.N. , Backer D.C. , Beutler G. , Fukushima T. , Leschiutta S.M. , Proverbio E. , Qi G.R. , Veillet C. , Winkler G.M.R. , Zhai Z.C. 
Published: July 2016

The relative frequency stability and the accuracy of atomic time scales, like International Atomic Time TAI, is now of order 1 × 10-15 thanks to progresses in clock technology and in clock comparison techniques. Cold atom primary Cs standards have a stated accuracy of 1 × 10-15 and a stability in the 10-16 region. Other cold atom clocks provide even better prospects, as well as clocks based on trapped ions. Frequencies based on optical and microwave transitions can now be compared with a similar or even better uncertainty thanks to femtosecond comb technology. Clock comparison techniques based on GPS (see http://maia.usno.navy.mil/gpst.html), or on dedicated Two Way technology provide adequate performance when averaging data over one or a few days, and should be improved to accompany the progresses of clocks.Since 1999, a number of organizations initiated a review on the future of the UTC system (insertion of leap seconds between TAI and UTC to keep |UT1 – UTC| < 0.9s). Several working groups have been initiated, notably by the International Telecommunications Union (Special Rapporteur Group (SRG) in the Working Party 7A), by the International Union of Radio Science, and by the IAU following Resolution B2(2000). No immediate conclusion may be foreseen but a consensus should be reached over the next triennium.
Division VII: Galactic System: (Systeme Galactique)
Authors: Freeman K. , Da Costa G. , Binney J. , Blitz L. , Matteucci F. , Spergel D. 
Published: July 2016

The scientific interests of Division VII are concerned with the Galactic system. Its two constituent commissions are Commission 33 (Structure and Dynamics of the Galactic System) and Commission 37 (Star Clusters and Associations). Please refer to the reports of these two commissions for the scientific highlights and lists of major conferences in this area.Study of the Galactic system involves a wide range of astrophysics and astronomical techniques, and the fields covered by many other commissions are therefore of very significant interest to Division VII. In particular, astronomers with interests in the Galactic system could consider reading also the reports of Commissions 5, 7, 24-30, 34-36, 40, 44 and 45, among others.
24. Photographic Astrometry (Astrometrie Photographique)
Authors: Upgren Arthur R. , van Altena William F. , Argue A. N. , Corbin T. E. , de Vegt Ch. , Gliese W. , Kanaev I. I. , Lutz T. E. , Stock J. 
Published: July 2016

One of the continuing problems facing Commission 24 is its name. It has been known and reported for some years that the present title is not suitable for reasons that are all too obvious. This problem has continued during the last three years, despite the growing development and use of non-photographic methods and techniques.Most of the recent meeting activity in which the Commission and its membership has been involved, has centered on its shared interests with Commission 8 and with the Working Group on reference frames formed at the last General Assembly. Since its inception at that time, C. A. Murray has been appointed to represent the Commission on that group.
16. Commission Pour Les Observations Physiques Des Planetes Et Des Satellites
Authors: Lyot M. B. 
Published: July 2016

Depuis sa dernière réunion, la commission a été cruellement éprouvée par la perte de son ancien président, de son président et de deux de ses membres les plus actifs.Le Révérend Père Théodore Phillips, président de 1925 à 1935, est décédé le 13 Mars 1942, à l’age de 76 ans. Il avait dirigé, pendant 35 ans, la section de Jupiter de la B.A.A. et effectué un nombre considérable d’observations. Il nous laisse une œuvre très étendue sur Jupiter et ses courants atmosphériques, ainsi que des dessins de Mars remarquables par leur beauté et leur précision.
18. Commission Des Longitudes Par Telegraphie Sans Fil
Authors: Tardi M. P. 
Published: July 2016

Les modalités de la publication ont été décidées lors de l’Assemblée Générale de Stockholm en 1938.Il est rappelé que le nombre des stations ayant participé à l’opération n’est pas moindre que soixante-et-onze. Le rassemblement des renseignements a été très long et a duré jusqu’à la fin de 1937, soit quatre ans après la fin des mesures.Il avait été décidé de publier à frais répartis par moitié entre l’U.A.I. et l’U.G.G.I. un volume par station donnant des renseignements et des tableaux très complets relatifs aux observations astronomiques, aux réceptions radiotélégraphiques et à la marche des garde-temps utilisés. On devait en outre publier un fascicule introductif et un volume de conclusions.
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 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”
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.
Densifying the Optical Reference Frame: The Tycho-2 Catalog of 2.5 Million Stars
Authors: Urban S.E. , Wycoff G.L. 
Published: July 2016

AbstractSince 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

AbstractThe 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

AbstractThe 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.