bluuebunny/crossref_metadata_2025_split huggingface dataset:
Discussion Sur Les Resultats De Theories Planetaires
Authors: Bretagnon P. 
Published: July 2016

AbstractLa construction de théories planétaires précises est un travail long et, pour ce qui nous concerne, n’est pas encore achevée. Aussi, les résultats dont nous parlerons ici ne sont que des résultats provisoires. Nous développerons quelques aspects des difficultés que nous avons rencontrées et les conséquences de ces difficultés sur l’orientation des méthodes utilisées pour résoudre les problèmes suivant qu’il s’agit des planètes intérieures ou des grosses planètes.
Improvement of Orbits of Satellites of Saturn Using Photographic Observations
Authors: Sinclair A.T. 
Published: July 2016

AbstractA programme of photographic observations of the satellites of Saturn, and the method of reduction and analysis are described. The observations have been used to update existing theories of Tethys, Dione, Rhea and Titan. A new theory of the motion of lapetus has been fitted to the observations.
Orbital Stability in the Elliptic Restricted Three Body Problem
Authors: Williams C.A. , Watts J.G. 
Published: July 2016

AbstractBased on the concept of orbital stability introduced by G. W. Hill, a method is presented to facilitate the determination of the orbital stability of solutions to the planar elliptic restricted problem of three bodies. The invariant relation introduced by Szebehely and Giacaglia (1964) contains an integral which is expanded here about a Keplerian solution to the problem. If the expansion converges, it can be used to determine the conditions for Hill stability. With it one can also define stability in a periodic sense.
Relativistic Hierarchy of Reference Systems and Time Scales
Authors: Brumberg V.A. 
Published: July 2016

AbstractRelativistic hierarchy of reference systems (RS) developed in recent years by different authors is examined in detail. Metric expressions and transformation relations for solar system barycentric RS (BRS), heliocentric RS (HRS), Earth-Moon local RS (LRS), geocentric RS (GRS), topocentric RS (TRS)and Earth satellite RS (SRS) may be obtained explicitly in harmonic coordinates of GRT. The time coordinate of any RS involves the corresponding time scale. Particular attention is given to the closed form representation of GRS avoiding expansions in powers of the geocentric coordinates. GRS has been constructed in both versions of dynamically non-rotating GRS (DGRS) or kinematically non-rotating GRS (KGRS). DGRS and KGRS differ in their space axes orientation by the amount of the geodesic precession. Similarly, taking into account the motion of the Sun around the center of the Galaxy one should distinguish between dynamically non-rotating BRS (DBRS) and kinematically non-rotating BRS (KBRS) differing in their space axes orientation by the amount of the galactic precession. Reduction to the galactic time and the galactic space axes may be needed in the nearest future.
Link between Hipparcos and VLBI Celestial Reference Frames
Authors: Arias E.F. , Lestrade J.-F. 
Published: July 2016

AbstractThe celestial frame of HIPPARCOS astrometric satellite will be materialized by the positions and proper motions of about 120000 stars relative to arbitrary origins. As the HIPPARCOS reference frame is not naturally related to fixed directions in space, it has to be linked to an inertial frame of similar quality. The technique of VLBI determines the coordinates of extragalactic radio sources precise at the milliarcsecond level in an equatorial frame. The precision expected for HIPPARCOS normal mission is 0.002ʺ for the positions, yearly proper motions and parallaxes.
A Global VLBI/LLR Analysis for the Determination of Precession and Nutation Constants
Authors: Charlot P. , Sovers O.J. , Williams J.G. , Newhall X X 
Published: July 2016

AbstractTwo decades of LLR data and one decade of VLBI data are combined in a global analysis to yield improved estimates of the Earth’s precession and nutation. In this analysis, LLR provides a strong determination of precession, while VLBI is stronger in fixing nutation terms with short periods. In all, 24 nutation amplitudes are estimated. The largest correlation coefficient, between precession and 18.6 yr out-of-phase nutation in longitude, is 0.88. With the exception of some 9 yr and 18.6 yr terms, formal uncertainties are 0.1 to 0.2 milliarcseconds.
The Establishment of the Radio/Optical Reference Frame
Authors: Russell J.L. , Johnston K.J. , DeVegt C. , Zacharias N. , Ma C. , Shaffer D. , Jauncey D. , Reynolds J. , White G. , Hughes J. , Hindsley R. 
Published: July 2016

This 5-yr program which began in 1987 is to establish a link between the radio and optical reference frames, using about 400 extragalactic sources which are compact and flat spectrum in the radio and which are observable in the optical. An overview of the program is presented at this meeting by Johnston et al. Various specific aspects of it are also discussed in Ma et al., McCarthy et al. and Reynolds et al.The observations have been continuing in both hemispheres and in both the radio and the optical. We have observed 348 sources with VLBI. There is at least one astrograph plate available for 369 sources and at least one prime focus plate available for 138 sources. Altogether there are 450 sources with some data.
Periodic Variations in the Coronal Green Line Intensity and their Connection with the White-light Coronal Structures
Authors: Minarovjech Milan , Rybanský Milan , Rušin Vojtech 
Published: July 2016

AbstractWe present an analysis of short time-scale intensity variations in the coronal green line as obtained with high time resolution observations. The observed data can be divided into two groups. The first one shows periodic intensity variations with a period of 5 min. the second one does not show any significant intensity variations. We studied the relation between regions of coronal intensity oscillations and the shape of white-light coronal structures. We found that the coronal green-line oscillations occur mainly in regions where open white-light coronal structures are located.
Call K Imaging to Understand UV Irradiance Variability
Authors: Kariyappa R. 
Published: July 2016

AbstractTo identify and understand the underlying physical mechanisms of total solar and UV irradiance variability and to estimate the contribution of various chromospheric features to UV irradiance, detailed analysis of spatially resolved data is required. The various chromospheric features have been segregated and different parameters have been derived from CaII K Spectroheliograms of NSO/Sac Peak and Kodaikanal Observatory and compared with UV irradiance flux measured in MgII h and k lines by NOAA 9 satellite. The important results of this detailed analysis of CaII K Images of 1992 together with UV irradiance data will be discussed in this paper.
The Space Stellar Photometry Mission COROT: Asteroseismology and Search for Extrasolar Planets
Authors: Baglin Annie , Vauclair Gérard ,   the COROT team
Published: July 2016

AbstractThe main scientific objectives, asteroseismology and search for extrasolar planets for the COROT photometric mission are presented, and its interest in terms of stellar variability. A description of the payload, details of the scientific program, the ground based preparatory observations and bibliography can be found athttp://www.astrsp-mrs.fr/corot/pagecorot.html.
New Intermediaries for the Main Problem in Satellite Theory
Authors: Ferrándiz José M. , Floría Luis 
Published: July 2016

AbstractAfter reviewing the original approach leading to the introduction of intermediaries in Satellite Theory, a general procedure to define intermediaries for the Main Problem in this Theory is proposed. This procedure is susceptible to an intuitive interpretation analogous to solving a simple puzzle. The application of this method to the Main Problem allows us not only to recover the well known classical intermediaries but also to obtain several completely new ones, all admitting simple solutions.
The Infrared Spectra of Synthesized Amorphous Silicates with Compositions of Olivine and Pyroxene
Authors: Koike Chiyoe , Tsuchiyama Akira 
Published: July 2016

AbstractAmorphous olivines synthesized by evaporation method show two very broad bands at 10-11 μm and 17.5-19 μm, which resemble the spectra of symbiotic stars. On the other hand, amorphous pyroxenes produced by the same method show two broad bands at 9.5-10.3 μ and 20-22 μ which are narrower than that of amorphous olivine. The features of amorphous olivine were easily altered by heating or hydration, and the peak wavelength of 18 μm band was easily shifted to longer wavelengths.
Light Scattering by Dust Particles in the Outer Solar System
Authors: Hovenier J.W. , Bosma P.B. 
Published: July 2016

AbstractPhotometric observations of the zodiacal light performed by Pioneer 10 indicated that there may be very little scattering by dust in the outer solar system. To shed more light on this problem we formulate explicit expressions for interpreting the brightness observed by a spacecraft travelling inside or outside a finite homogeneous cloud of scattering particles. An application is made to the ecliptic zodiacal light brightness as observed by Pioneer 10 and tabulated by Toller and Weinberg (1985). A satisfactory interpretation of these data as well as earthbound observations can be given by means of a model having a particle density distribution or mean scattering cross section which vanishes beyond 2.8 - 3.7 AU. Some implications for the nature and spatial distribution of the interplanetary dust are discussed.
Comets as a Source of Interplanetary and Interstellar Grains
Authors: Hoyle F. , Vickramasinghe N.C. 
Published: July 2016

AbstractProperties of cometary dust with regard to bulk density, optical characteristics and sizes, derived from recent observations, are used to model scattering properties of cometary and interstellar grains. A wide range of astronomical observations are shown to be explained if cometary objects are hypothesised as a major source of dust grains in the galaxy.
Spectropolarimetry of Comet Halley
Authors: Visvanathan N. , Meglick Z. , Wickramasinghe D.T. 
Published: July 2016

AbstractSpectropolarimetric observations from 3800 to 7000 Å were obtained for the nucleus of comet Halley for nine nights during 1985-86. The observations were spaced over phase angle of 2 to 66 °. The continuum polarization without molecular-line contamination as well as the polarization of the molecular lines were evaluated. The plot of polarization versus the phase angle shows small negative polarization for angles less than 20°. The highest polarization measured for phase angle ≤ 66° is 19.6% .The lowest polarization of −2.0% has been measured at the phase angle ~ 10°. The variation of polarization with phase angle is nearly linear in the range 30 to 60° giving a slope of 0.4316% per degree. There is small dependence of polarization with the wavelength in the region 3800 to 6500Å. The polarization of the molecular bands CN, C3, C2(0,0) and C2(1,0) have also been evaluated for the spectra of 15th December 1985, 18th and 19th March 1986 and 8th April 1986.
The Orbital Distribution and Origin of Meteoroids
Authors: Steel Duncan 
Published: July 2016

AbstractApproximately 68,000 orbits of meteoroids, ranging from sizes of 10 cm and more down to microgram masses, are now available through the IAU Meteor Data Center. These orbits were measured in surveys based in the U.S.S.R., the U.S.A., Canada, Somalia, and Australia, using photographic, radar and television techniques; the data represent our best knowledge of the orbital distributions of smaller solid bodies in the solar system. It is found that quite different distributions result in different mass regimes, with implications for the origin and evolution of these particles: for example the larger bodies, observed as fireballs, are associated with meteorites in coming from the region of the asteroid belt with low-inclination orbits, whereas the smaller meteoroids have more comet-like orbits. There is also evidence for several meteoroid streams associated with specific Apollo asteroids. The data may additionally be viewed as a suitable source function in investigations of the production of interplanetary dust from the fragmentation of larger meteoroids in mutual collisions. However, inspection of the data raises many questions: for instance there seem to be many meteoroids on small retrograde paths, but no possible parent objects are known to exist on such orbits.
Vertical and Radial Distributions of Gas and Young Objects in the Galaxy and the Schmidt’s Law of Star Formation
Authors: Guibert J. , Lequeux J. , Viallefond F. 
Published: July 2016

AbstractThe thickness of the disc distribution of young objects is shown to be significantly smaller than that of the interstellar gas over the whole Galaxy, as predicted by the Schmidt’s law of star formation. The radial distribution of the density of young objects at z = 0, compared with that of the gas, is also consistent with the Schmidt’s law. The exponent in this law is found to be between 1.5 and 2. A brief discussion of simple models of galactic evolution using the Schmidt’s law is made.
The Kamiokande Solar Neutrino Experiment
Authors: Hirata K. S. , Kajita T. , Kifune T. , Kihara K. , Nakahata M. , Nakamura K. , Ohara S. , Sato N. , Suzuki Y. , Totsuka Y. , Yaginuma Y. , Mori M. , Oyama Y. , Suzuki A. , Takahashi K. , Takei H. , Tanimori T. , Koshiba M. , Suda T. , Tajima T. , Miyano K. , Miyata H. , Yamada M. , Fukuda Y. , Kaneyuki K. , Nagashima Y. , Takita M. , Beier E. W. , Feldscher L. R. , Frank E. D. , Frati W. , Kim S.B. , Mann A. K. , Newcomer F.M. , Van Berg R , Zhang W. 
Published: July 2016

AbstractThe observation of 8B solar Neutrinos in the Kamiokande-II detector is presented. Based on 450 days of data in the time period of January 1987 through May 1988, the measured flux obtained with Ee ≥ 9.3 MeV was 0.46 ± 0.13 (stat) ± 0.08 (sys) of the value predicted by the standard solar model. The detector and analysis methods were improved since June 1988 and the background level has been decreased by a factor of about three since then.
The GALLEX Project
Authors: Kirsten T. , Breitenbach M. , Hampel W. , Heusser G. , Kiko J. , Kirsten T. , Lalla H. , Lenzing A. , Pernicka E. , Plaga R. , Povh B. , Schlosser C. , Völk H. , Wink R. , Zuber K. , Ammon R.v. , Ebert K. , Henrich E. , Stieglitz L. , Bellotti E. , Cremonesi O. , Fiorini E. , Liguori C. , Ragazzi S. , Zanotti L. , Mössbauer R. , Urban A. , Berthomieu G. , Schatzman E. , d’Angelo S. , Bacci C. , Belli P. , Bernabei R. , Paoluzi L. , Santonico R. , Cribier M. , Dupont G. , Pichard B. , Rich J. , Spiro M. , Stolarczyk T. , Tao C. , Vignaud D. , Dostrovsky I. , Friedlander G. , Hahn R.L. , Rowley J.K. , Stoenner R.W. , Weneser J. 
Published: July 2016

AbstractThe GALLEX collaboration aims at the detection of solar neutrinos in a radiochemical experiment employing 30 tons of Gallium in form of concentrated aqueous Gallium-chloride solution. The detector is primarily sensitive to the otherwise inaccessible pp-neutrinos. Details of the experiment have been repeatedly described before [1-7]. Here we report the present status of implementation in the Laboratori Nazionali del Gran Sasso (Italy). So far, 12.2 tons of Gallium are at hand. The present status of development allows to start the first full scale run at the time when 30 tons of Gallium become available. This date is expected to be January, 1990.
The Baksan Gallium Solar Neutrino Experiment
Authors: Gavrin V. N. , Abazov A. I. , Abdurashitov D. N. , Anosov O. L. , Bychuk O. V. , Danshin S. N. , Eroshkina L. A. , Faizov E. L. , Gavrin V. N. , Gayevsky V. I. , Girin S. V. , Kalikhov A. V. , Kireyev S. M. , Knodel T. V. , Knyshenko I. I. , Kornoukhov V. N. , Mezentseva S. A. , Mirmov I. N. , Ostrinsky A. V. , Petukhov V. V. , Pshukov A. M. , Revzin N. E. , Shikhin A. A. , Slyusareva E. D. , Tikhonov A. A. , Timofeyev P. V. , Veretenkin E. P. , Vermul V. M. , Yantz V. E. , Zakharov Yu. I. , Zatsepin G. T. , Zhandarov V. L. , Bowles T. J. , Cleveland B. T. , Elliott S. R. , O’Brien H. A. , Wark D. L. , Wilkerson J. F. , Davis R. , Lande K. , Cherry M. L. , Kouzes R. T. 
Published: July 2016

AbstractA radiochemical 71Ga−71 Ge experiment to determine the integral flux of neutrinos from the sun has been constructed at the Baksan Neutrino Observatory in the USSR. Measurements have begun with 30 tonnes of gallium. The experiment is being expanded with the addition of another 30 tonnes. The motivation, experimental procedures, and present status of this experiment are presented.
Neutrino Masses, Neutrino Oscillations and Dark Matter
Authors: Harari Haim 
Published: July 2016

AbstractWe discuss bounds on neutrino masses using an analysis based on direct measurements, cosmological bounds, oscillation experiments, the solar neutrino puzzle and theoretical considerations on neutrino decays. We present four possible solutions for the mass range of the three neutrino flavors. We outline experiments which can distinguish among these solutions and discuss their implications for the cosmological dark matter problem.
Variations of the Low l Solar Acoustic Spectrum Correlated with the Activity Cycle
Authors: Pallé P.L. , Régulo C. , Roca Cortés T. 
Published: July 2016

AbstractSolar cycle variation of the frequencies and of the power of solar acoustic oscillations are investigated. Integrated sunlight data from 1977 to 1988 obtained at the Observatorio del Teide (Izaña, Tenerife), using a resonant scattering spectrophotometer, is analyzed in 60 day time strings and their power spectra are calculated from 2 to 3.8 mHz. To study the frequency variation, each power spectrum is cross-correlated with the one corresponding to the 1981 series and the shifts of the centroids of the cross-correlation peaks are calculated. The results show a clear variation in frequency of the cross-correlation peaks of −0.37 ± 0.04 μHz peak to peak as solar activity cycle goes from maximum to minimum. Moreover, this effect is found to depend on the l value of the modes, being absent for l = 0 and of 0.42 ± 0.06 μHz for l = 1. These results can be interpreted as an amplitude modulation between modes of the same multiplet, probably as a consequence of the action of strong magnetic fields. As low l modes penetrate deeply into the Sun’s interior, these observations suggest changes in its structure correlated with the solar activity cycle. When the power of the modes is calculated, using the same series as before, and its change along the solar cycle is studied, a variation of ~ 40% is found, the power being higher when solar activity is at its minimum. If this effect is independent of the l value of the p-modes, the results can be interpreted in terms of a change in the efficiency of the excitation mechanism of such modes. Indeed, if turbulent convection is such a mechanism, a change in the characteristic size of the granulation would account for the observed effect. Alternatively, another explanation could be a selective change in the efficiency of the excitation and/or damping mechanisms of the l ≤ 3 modes in front of other l value modes.
The Early Outburst Spectra of Nova V1500 Cygni
Authors: Mikołajewski M. , Mikołajewska J. 
Published: July 2016

Nova Cygni 1975 (V1500 Cyg) was outstanding in several respects. It was the most luminous galactic nova ever observed, had the largest outburst amplitude, and had the fastest evolution with time.The spectra, with dispersion 28 A/mm and in spectral range λλ3560-5055 A, were obtained with the CCS spectrograph on 90 cm reflector at Toruń Observatory by the research group supervised by prof. A. WoszczyK. The CCS spectrograph was equipped with the 3.5 arcsec aperture Richardson’s image slicer and stars with known spectral energy distributions were observed on each night, so we were able to derive absolute energy distributions for the V1500 Cyg spectra. The calibration of the energy scale was performed by comparing synthetic B magnitudes calculated from our spectra with numerous published B photometry of the nova. The first spectra were obtained about 3h later than spectra reported by Boyarchuk (1977) and about 6h earlier than spectra discussed by Duerbeck and Wolf (1977); thus they are among the earliest spectra of the nova available. Simultaneously, the spectra correspond to the earliest state of spectral evolution of a nova ouburst yet observed. The pre-maximum spectral evolution of Nova V1500 Cyg is extremely fast. The spectra (Figures 1 and 2) secured on JD 2442654 are characterized by a very strong continuum and broad blueshifted absorption lines of OII, NII and CII of unusual strengths, as well as the Balmer series and Hel.
Model Atmospheres for Novae During the Early Stages
Authors: Wehrsě R. , Hauschildt P. H. , Shaviv G. , Starrfield S. 
Published: July 2016

AbstractContinuum and line blanketing models for the photospheres of novae in the early stages of their outbursts are presented. The expanding envelopes are characterized by a very slow increase of density with decreasing radius which leads to very large geometrical extensions and large temperature differences between the inner and outer parts. The spectra show a large IR excess and a small Balmer jump which may be either in absorption or in emission. For the parameters considered (Teff = 104, 1.5 × 104, 2 × 104K, R = 1011 cm, solar composition), most lines are in absorption. The effects of both modifications in the temperature structure (e.g. by heating from shock fronts) and changes in the abundances of the heavy elements on the emergent spectra are briefly discussed.
Modelling the Common Envelope Phase in Classical Novae
Authors: Shankar Anurag , Truran James W. , Burkert Andreas , Livio Mario 
Published: July 2016

AbstractPreliminary results of 1– and 2– dimensional hydrodynamical calculations of the common envelope phase in very slow classical novae are presented. We show that frictional deposition of orbital energy and angular momentum into the envelope can potentially induce mass loss. Specifically, we find that despite rapid initial spin–up of the envelope, ejection of mass in the orbital plane continues at a substantial rate.
Theoretical Implications of Nova Abundances
Authors: Truran James W. 
Published: July 2016

AbstractAbundance determinations for the ejected shells of classical novae are reviewed. Substantial enrichments (relative to hydrogen) of helium, the CNO elements, and elements in the range from neon to aluminum are found to be characteristic of nova ejecta. The source of these enrichments is believed to be the dredge-up of underlying white dwarf core matter, thus reflecting the white dwarf composition and confirming the presence of oxygen-neon-magnesium (ONeMg) as well as carbon-oxygen (CO) degenerate dwarfs in cataclysmic variable systems. The implications of these abundance enrichments, for the behavior of nova systems in outburst and for nucleosynthesis, are examined.
The 1989 Outburst of V404 Cygni: A Very Unusual X-Ray Nova
Authors: Wagner R. M. , Starrfield S. , Cassatella A. , Gonzalez-Riestra R. , Kreidl T. J. , Howell S. B. , Hjellming R. M. , Han X.-H. , Shrader C. , Sonneborn G. , Collins G. W. , Bertram R. , Buie M. W. , Bond H. E. , Johnson J. , Harrison T. , Gehrz R. D. , Córdova F. A. , Szkody P. , Margon B. , MacDonald J. , Fried R. 
Published: July 2016

AbstractOn May 22, 1989 the Japanese Ginga Team discovered a new X-ray source that was cataloged as GS 2023+338. This source was subsequently identified as coincident in position with a previously known nova cataloged as V404 Cygni. Its last recorded outburst was in 1938 when it rose to about 12th mag. Spectroscopic data were obtained and confirmed the nature of the outburst. Additional ground based data were obtained by us at CTIO and the VLA. The X-ray behavior of this object has been reported to be very unusual and it reached a peak of about 17 crab about one week after discovery. Since then it has varied widely in magnitude at all wavelengths at which it has been studied. We present a brief summary of the observations that have been obtained up to the time of the meeting and shortly thereafter.