bluuebunny/crossref_metadata_2025_split huggingface dataset:
33. Commission de la Statistique Stellaire
Authors: Lindblad M. , Bok MM. , Eddington  , Hertzsprung  , Hirayama S. , Lundmark  , Luyten  , Malmquist  , Mineur  , Oort  , Pannekoek  , Russell  , Schatén  , Schilt  , Seares  , Strömberg  , van Maanen  , van Rhijn  , von der Pahlen  
Published: July 2016

In the wide field of research covered by the Commission considerable progress has been made in recent years, and it is only possible here to touch briefly on the results of a few lines of investigation, without any attempt to completeness.Stellar luminosities. On the basis of the new list of Mount Wilson spectroscopic parallaxes and a compilation of the long series of modern trigonometric parallaxes A. van Maanen finds 617 objects within a distance of 20 parsecs from the sun. It is very doubtful, however, if we know all the stars even in the region of 5 parsecs radius. Almost all the known stars within 20 parsecs belong to the main sequence, the faintest star being of absolute magnitude +16.6. The most interesting deviations from the main sequence are the three “white dwarfs”, Сотр. of Sirius, Comp. o2 Eridani, and van Maanen’s F type star. G. P. Kuiper lists 3 additional white dwarfs at larger distances which were estimated to be of types Bo, B7 and A2. For the first two stars, A.C. 70°8247 and Wolf 1346, a revision of the spectral types by Adams and Humason gives A2 and A5, respectively, although the spectra differ considerably from normal ones. The A2 star in Kuiper’s list is the one discovered by Oosterhoff in the region of the cluster h, X Persei; its spectral characteristics have been examined by Öhman and by Humason. The absence of the high-numbered members of the Bahner series and of the continuous absorption at the Balmer limit seems to be an important criterion of such stars. A white dwarf of quite peculiar spectrum (type probably about B8) is the companion of o Ceti discovered spectro-graphically by Joy in 1922. There appear several additional deviations towards faint magnitudes from the main sequence which may be classed more or less safely among the white dwarfs. A few such cases have been discussed at Lund by J. Tuominen.
Commission 13. (Solar Eclipses.)
Authors: Stratton F. J. M. , Minnaert M. 
Published: July 2016

At the request of the President, Prof. Sotome gave some information about the possibilities of observing in Japan and offered to give any additional details to all those who were interested. In the best central part there was about 40% probability of a clear sky.No Russian astronomer being present, Prof. Carroll reported that scientific workers in Russia were anxious to give all possible cooperation; he intended to go himself to Russia this summer, in order to prepare an expedition to Siberia, and he was prepared to get all questions answered which any one should wish to put. Letters about this subject must reach him before the end of August.
Commission 29. (Stellar Spectra.)
Authors: Russell H. N. , Swings P. 
Published: July 2016

1. Le rapport distribué aux personnes présentes commence par un court aperçu des principaux travaux faits dans le domaine des spectres stellaires depuis l’assemblée précédente. Le Président demande si l’une ou l’autre personne désire suggérer des modifications ou compléments à cet exposé. Aucune observation n’est présentée.2. Le rapport du sous-comité chargé de l’examen des critères de classification des spectres stellaires est ensuite mis en discussion. Une lettre de Mme Payne-Gaposchkin a été reçue à ce sujet; Mme Payne-Gaposchkin signale que des détails manquent dans le rapport du sous-comité; elle demande aussi que soient définis clairement les types A7 et K7 actuellement utilisés fréquemment, ainsi que les symboles g et d distinguant les étoiles géantes et naines.
3. Commission des Notations, des Unités et de L’économie Des Publications
Authors: Strömgren M. E. , Bosler MM. , Chant  , Eddington  , Grabowski L. , Horn d’Arturo  , Lou Kao , Ludendorff  , Russell  , Schlesinger  
Published: July 2016

At the Paris meeting in 1935 the following resolutions of Commission 3 were adopted by the Union:1.Que la liste préliminaire de notations préparée par le Président de la Commission soit, après certaines modifications, imprimée dans les Transactions de l’Union à titre de liste recommandée provisoirement, et que les astronomes intéressés à la question soient invités a adresser au Président de la Commission les changements qu’ils y suggéreraient.2.Que l’Union donne son approbation à la publication d’un complément mentionnant les changements et additions à la liste des Observatoires et des Astronomes publiée en 1931, sous les auspices de l’Union, par l’Observatoire Royal d’Uccle.3.Que l’Union consacre, si possible, une somme n’excédant pas cinq cents francs or, à aider la publication de ce complément.The provisional list of notations was printed, as an appendix to the report of Commission 3, Trans. I.A.U. 5, 18, 1935. A number of astronomers communicated to the President of the Commission suggestions of changes. On the basis of these suggestions a corrected list of notations was prepared.Reprints of this list were circulated to the various observatories and suggestions of changes invited. In response to this a number of suggestions were received.
II. Commission des Phénomènes Chromosphériques
Authors: D’Azambuja M. L. , Abetti MM. , Bosler  , Brunner  , Butler  , da Costa Lobo F. M. , Deslandres  , Donitch N. , Evershed  , McMath  , Merlin  , Newbegin  , Newton  , Nicholson  , Pettit  , Rodés  , Rowland  , Royds  , Sotome  , Unsöld  , Woltjer  
Published: July 2016

La Commission vient de subir une lourde perte en la personne de George Ellery Hale, Directeur honoraire de l’Observatoire du Mont Wilson, décédé le 21 février 1938, à l’âge de 70 ans.L’enregistrement des phénomènes chromosphériques qui sert de base aux relevés et statistiques publiés régulièrement par divers observatoires, a été poursuivi sans changements notables depuis le dernier congrès. Le tableau reproduit dans Trans. I.A.U. 5, 59, 1935 et dans lequel sont groupés les renseignements relatifs à ces travaux d’observation courante, est donc toujours valable.
18. Commission des Longitudes par Télégraphie Sans fil
Authors: Perrier Général G. , Lambert M. A. , Baîllaud MM. R. , Bianchi  , Bowie W. , Coculesco  , Lobo F. M. da Costa , de Lemos  , Esclangon  , Fayet  , Fichot  , Guyot  , Hasimoto  , Ivanov  , Jackson J. , Jeffers  , Jones Spencer , Jouaust  , Kohlschütter E. , Krassowski J. , Lejay  , Moreau  , Niethammer  , Nörlund  , Nušl  , Pavlov  , Plakidis  , Sampson  , Silva  , Sollenberger  , Stewart R. M. , Stoyko  , Tsiang  , Volta  , Watts  , Witkowski  , Zimmer  
Published: July 2016

La centralisation au Bureau international de l’Heure des résultats d’observations de l’Opération internationale de 1933 a été très lente, puisque les dernières données attendues ont été reçues vers la fin de 1937.Le nombre des stations ayant coopéré à l’Opération internationale et ayant transmis leurs observations à l’organisme centralisateur s’élève à soixante et onze. Ainsi qu’il a été expliqué à notre Commission mixte, lors du Congrès de l’Union géodésique et géophysique internationale tenu à Édimbourg en 1936, ces stations ont été réparties en trois groupes:Le Ier comprenant vingt Observatoires, disposant chacun de plusieurs horloges de première classe (soit à poids sous pression et à température constantes, soit à quartz piézoélectrique);
31. Commission de L’heure
Authors: NöRlund M. N. E. , Perrier G. , Esclangon M. E. , Baillaud MM. R. , Banachiewicz  , Bianch  , Carnera  , Dneprovsky  , Dyson  , Fayet  , Gallo  , Guyot  , Lambert A. , Lejay  , Moreau  , Niethammer  , Picart L. , Postoev  , Preipich-Freyberg  , Sampson  , Silva  , Sollenberger  , Sotome  , Stewart  , Stoyko  , Tinoco  , Verbaandert  , Voûte  
Published: July 2016

Durant la période de 1933 à 1936 le Bulletin Horaire a donné les heures définitives des signaux horaires d’après la moyenne de 15 observatoires. A partir du Ier janvier 1937 on introduit trois observatoires en plus (Kharkov, Manille et Tokyo), qui communiquent régulièrement leurs résultats au B.I.H.Au Bureau International de l’Heure certains perfectionnements sont actuelle ment en voie de réalisation. Il s’agit d’une horloge à diapason d’une part, et, de l’autre, d’un ensemble nouveau pour l’émission des signaux horaires. M. Lambert va donner une communication sur ce sujet.
5. Study of Cosmic Rays by Rockets and Sputniks in the U.S.S.R.
Authors: Vernov S. N. , Chudakov A. E. 
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.
4. Ephemerides
Authors: Wilkins G. A. , Kovalevsky J. , Clemence G. M. , Chebotarev G. A. , Duncombe R. L. , Fricke W. 
Published: July 2016

The appended reports of the directors of the national ephemeris offices provide a record of the current activity in the publication and preparation of astronomical ephemerides, including those published for use by navigators and surveyors and those prepared for astronomers whose special needs are not met in the printed almanacs. A brief review of the relevant work of other institutions and individuals is also given in the appendix. The reports also cover to some extent activities in positional astronomy and celestial mechanics (i.e. in the fields of interest of Commissions 7, 8, 17, 19, 20 and 31). This report is therefore restricted to reviewing, firstly, the action that has been taken on matters raised at and since the 1967 meetings of the Commission and, secondly, the matters that will require attention at and after the 1970 meetings.Before that review, it is appropriate to pay tribute to the memory of that almost legendary astronomer, Gaston Fayet, who died on 27 December 1967 at the advanced age of 93. As member of the Bureau des Longitudes responsible for the production of the Connaissance des Temps from 1930 to 1961, and President of Commission 4 from 1938 to 1952, he contributed greatly to our subject, in addition to his researches in other fields particularly in respect of the minor planets.
Appendix: Reports of the Directors of the National Ephemerides
Authors: Abalakin V. K. , Kovalevsky J. , Sadler D. H. , Fricke W. , Sinzi A. M. , Lahiri A. M. , Rodriguez M. , Duncombe R. L. , Wilkins G. A. 
Published: July 2016

During the period under review two issues of the Astronomical Yearbook of the U.S.S.R. for the years 1971, 1972 have been published, and that for 1973 is in preparation. The positions and proper motions of the stars are in the FK4 system as recommended by Commission 4 in 1961. Further, as recommended at the meeting in Hamburg in 1964 (Trans. IAU, 12 B (1964), 105,1966) the IAU System of Astronomical Constants has been introduced into the tabulations of the day numbers, solar and lunar eclipses, ephemerides for physical observations of planets, and the factors S &C. The corresponding differential corrections to the Moon’s ephemeris as well as re-calculated eclipse data for 1971 have been tabulated separately in the Appendix to the Yearbook for 1971. As from the edition of the Yearbook for 1972, the lunar ephemeris j = 2 will be published in accordance with the recommendations adopted in Prague in 1967.The regular publication of the ephemeris of the lunar crater Mösting A has been continued in the editions of the Yearbook mentioned above.Fundamental ephemerides of the Sun, Moon, and planets have been printed in full conformity with the first part of the Astronomical Ephemeris circulated in advance by H. M. Nautical Almanac Office, Royal Greenwich Observatory.
Report of the Committee on the Spectra of Variable Stars
Authors: Feast M. W. 
Published: July 2016

The field covered by this report overlaps particularly with the work of Commissions 29 and 45 whose reports should be consulted. I have been greatly helped by reports on Soviet work by Professor Kukarkin and Dr Boyarchuk and a bibliography of European literature by Bloch.The Sonneberg programme for determining spectral types of variables has been described by Götz and Wenzel (AN, 290, 99) and several lists have been published in MVS. Bakos is studying high dispersion spectra of a number of variables that are members of visual binary systems.Stephenson and Terrill (ApJ, 147, 148) and Houk (IB, 228) have given spectral types for a considerable number of long period variables. Terrill (AJ, 74, 413) has made an extensive study of the variation of spectrum with phase for 51 red variables. Deutsch, Keenan and Garrison have continued their extensive programme of spectral classification of Mira variables. Keenan and Dessy (ApJ, 146, 583) suggest that the relatively early spectral type of the very long period Miras (R Cen, R Nor etc.) showing double maxima indicates that the fundamental parameter is the half-period (between successive maxima). A similar conclusion (ApJ, 93, 380; MN, 125, 367) was reached earlier by others on the basis of the correlation with period of the difference between absorption and emission velocities. Feast has used K subgiant companion of U Men to derive an absolute magnitude of — 0m.5 for the Mira star. The radial velocity of the companion agrees with the absorption velocity of the variable near maximum (Obs.).
Report of the Working Group on Flare Stars
Authors: Andrews A. D. , Čugainov P. F. , Geršberg R. E. , Oskanian V. 
Published: July 2016

The Working Group was organized in order to promote and develop the cooperative studies of flare stars. Up to the present time our observation programmes were restricted to the UV Ceti-type stars only. Organizational activities followed the aims:(1) To extend the existing network of photoelectric observers in order to provide 24-hour coverage of a star during selected sessions lasting usually 14 days.(2) To collect data using standardized techniques in order to study frequency of stellar flares and secondary variations.(3) To provide optical coverage for simultaneous radio, spectroscopic and polarimetric observations.
Working Group on Galaxy Photometry
Authors: de Vaucouleurs G. 
Published: July 2016

1. A tabular presentation has been adopted and the report does not cover work in the U.S.S.R. During the report period Circular No. 6 (Report on Prague Meeting) and a Technical Supplement, No. 6a, were distributed. Work on standard luminosity profiles for a few well-observed galaxies (NGC3115, 3379, 4486) progressed more slowly than expected, but provisional results will be available for presentation at the 1970 meeting.2. On the observational side the major event to report is the publication of an Atlas de Galaxias Australes by J. L. Sěrsic; it gives photographs, descriptions and detailed surface photometry of 50 southern galaxies observed with the 150-cm reflector of Cordoba Observatory. Another important contribution is the dissertation of H. D. Abies on “Optical Study of Nearby Galaxies” of interest to radio astronomy. The isophotometric atlas of 70-80 galaxies and UBV catalogue of 500 galaxies observed by G. and A. de Vaucouleurs at Mt. Stromlo and McDonald Observatories and by H. D. Abies at Flagstaff, F. Bertola at Asiago and other collaborators is being prepared for publication in 1970-71.On the technical side the rapid development of automatic digital methods for data recording and processing should lead to a great acceleration in the production of precise isophote maps, but most commercial instruments are still deficient with respect to mechanical precision, optical design (stray light, beam definition) and electrical stability.
36. Theory of Stellar Atmospheres
Authors: Underhill A. B. , Cayrel R. , Böhm K. H. , Ivanov V. V. , Jefferies J. T. , Thomas R. N. , Ueno S. 
Published: July 2016

This report has been prepared by the President with the assistance of the Vice-President, the Members of the Organizing Committee, V. V. Ivanov, P. Conti and of D. G. Hummer. The work of Commission 36 comes in contact with that of many commissions. Some subjects may be dealt with more fully in those reports; some subjects may have been “unlawfully” included here. Considerable choice has been exercised by the President about what to mention and in which section of the report to place it. The final product is only indicative of the large amount of work going on. An extensive bibliography has been compiled and will be distributed to commission members.Commissions 12, 27, 29, 44 and 45 deal with observational material which our theories attempt to interpret, thus it is essential to study the reports of these commissions to appreciate the diversity of material for which theories are needed and against which theories may be checked. The theoretical treatment of the problems of planetary atmospheres, Commission 16, is not entirely divorced from that of stellar atmospheres. To set realistic inner boundary conditions on our atmosphere models and on our thinking, we must consider the material of Commission 35 while to set the outer boundary conditions we may consider the physical state of planetary nebulae which is one subject of Commission 34. When we wish to apply ideas about the interactions between radiation, atoms, ions and molecules we use material which lies in the province of Commission 14.
Models for Source Structure Corrections
Authors: Charlot P. 
Published: July 2016

AbstractAt the milliarcsecond scale, most of the extragalactic radio sources exhibit spatially-extended intrinsic structures which are variable in both time and frequency. Such radio structures set limits on the accuracy of source positions determined with the Very Long Baseline Interferometry (VLBI) technique unless their effects in the astrometric data can be accounted for. We review the modeling scheme for calculating source structure corrections and discuss the magnitude and impact of these effects for the sources that are part of the International Celestial Reference Frame (ICRF). Results obtained by applying source structure corrections to actual VLBI observations on the time-varying source 4C39.25 (0923 + 392) are also presented.
Rigid-Earth Nutation Models
Authors: Souchay J. 
Published: July 2016

AbstractDespite the fact that the main causes of the differences between the observed Earth nutation and that derived from analytical calculations come from geophysical effects associated with nonrigidity (core flattening, core-mantle interactions, oceans, etc…), efforts have been made recently to compute the nutation of the Earth when it is considered to be a rigid body, giving birth to several “rigid Earth nutation models.” The reason for these efforts is that any coefficient of nutation for a realistic Earth (including effects due to nonrigidity) is calculated starting from a coefficient for a rigid-Earth model, using a frequency-dependent transfer function. Therefore it is important to achieve high quality in the determination of rigid-Earth nutation coefficients, in order to isolate the nonrigid effects still not well-modeled.After reviewing various rigid-Earth nutation models which have been established recently and their relative improvement with respect to older ones, we discuss their specifics and their degree of agreement.
SOFA Software Progress Report
Authors: Wallace P. 
Published: July 2016

AbstractThe IAU set up the SOFA initiative at the 1994 General Assembly, to promulgate an authoritative set of fundamental-astronomy constants and algorithms. At the subsequent General Assembly, in 1997, the appointment of a Reviewing Board and the selection of a site for the SOFA Center (the outlet for SOFA products) were announced. The time since then has been spent developing the specifications for a basic collection of fundamental-astronomy algorithms. Progress has been slow, for a number of reasons: the task is difficult and requires great circumspection; a substantial toolkit of support routines must be adopted or developed before work on the astronomy routines themselves can begin; and it takes time for a geographically dispersed committee to reach a consensus on matters that involve value judgements, such as programming style. However, despite these formidable difficulties, significant progress has been made. A library of 52 vector/matrix routines has been developed, supporting a set of 25 astronomy algorithms. The Reviewing Board is about to start validating these algorithms, at which point they can be released through the SOFA Center.
The Definition of UTC
Authors: McCarthy Dennis D. 
Published: July 2016

AbstractThe current definition of Coordinated Universal Time (UTC) is related to the unpredictable, variable rotation rate of the Earth. This is accomplished by irregular insertions of leap seconds, creating unpredictable discontinuities in UTC. With the increasing importance of a continuous, uniform time scale for users, it is appropriate to re-examine the current definition of this time scale. There are several possibilities to address this problem, and it is appropriate that the International Astronomical Union establish a working group to investigate the continuing need for leap seconds and possible changes in the definition of UTC.
The Effect of Companions on the SIM Reference Frame
Authors: Jacobs Christopher S. , Turyshev Slava G. 
Published: July 2016

AbstractThe Space Interferometry Mission (SIM) is a 10-m Michelson space-based optical interferometer designed for precision astrometry (4μas, 3μas/yr) with better accuracy hoped for over a narrow field of view. It is intended to search for planets and investigate a number of problems in Galactic and extra-galactic astronomy.The accuracy and stability of SIM’s celestial reference frame is subject to degradation over the 5-year mission from the reflex motion induced by massive companions of the objects used to construct the celestial reference frame. We present the results of simulations which show the sensitivity of reference frame accuracy to companions as a function of mass and period. We assume that pre-launch ground surveys will eliminate all objects with RMS radial velocity > 10 m/s. We further assume that the standard astrometric parameters of position, parallax, and proper motion plus acceleration terms in right ascension and declination will be allowed to absorb reflex motion.
The Parkes Multibeam Pulsar Survey and Interstellar Scattering
Authors: Manchester R.N. 
Published: July 2016

AbstractThe Parkes multibeam pulsar survey is a major survey for pulsars lying within a 10°-wide strip along the southern Galactic plane, using the multibeam receiver on the Parkes 64-m radiotelescope. It is an international collaboration between groups at Jodrell Bank Observatory, Massachusetts Institute of Technology, Bologna Astronomical Observatory and the ATNF. The survey commenced in 1997 August, and has so far succeeded in finding more than 550 previously unknown pulsars. Many of these are distant, with some beyond the centre of the Galaxy according to current models of the interstellar electron density distribution. Interstellar scattering affects the pulse profile of many of the more distant pulsars even at 1374 MHz, the centre frequency of the survey. Preliminary results from the survey are presented.
Scattering of the Low Frequency Pulsar Radiation
Authors: Kuzmin Arkady 
Published: July 2016

AbstractWe report the results of the measurements and analysis of the pulse broadening due to interstellar scattering on 43 pulsars at 102 MHz. This is the largest uniform sample of direct measurements of pulsar scattering τsc, which make it feasible to analyze the dependence of this value on other pulsar parameters. The measured dependence of τsc on dispersion measure τsc(DM) = 40(DM /100)2.1 is close to theoretically expected relation τsc(DM) α DM2. A frequency dependence of the scattering pulse broadening is weaker than commonly accepted τsc α v−4.4.