bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Development of Advanced-Technology Automated/Robotic Telescope Systems and the Future of Small-Telescope Astronomy
Authors: Williams Richard J. , Mulherin James 
Published: July 2016

AbstractDuring the 1990s groups at universities around the world developed small working automated/robotic telescopes that proved the feasibility of using such systems for education and research projects. A few of the more successful projects such as the Bradford Robotic Observatory in the United Kingdom and the University of Iowa’s Automated Telescope Facility (AFT) and Iowa Robotic Observatory (IRO) programs proved how useful and powerful these systems can be in practice. This paper describes how one company, Torus Technologies, developed hardware and software technologies to create the most advanced integrated small automated/robotic telescope systems in the world. These systems were designed from the “bottom up” to be automated/robotic telescopes capable of operating an entire observatory including domes, CCD cameras, and other peripheral equipment.Automated/robotic telescopes can play a major role in enabling small colleges and universities, especially in developing countries, to actively participate in serious “hands on” research and education projects that otherwise would not be practical. A commercially available affordable, high-precision, and proven turnkey automated/robotic small telescope system capable of operating remotely via the Internet is crucial for bringing this technology into widespread use. Today Torus Technologies telescopes are installed at locations worldwide as primary instruments for research programs, discovery and monitoring programs, and education programs. This paper describes some of the current applications for using these telescopes and how these telescope systems will be used in the future in standalone installations and in global networks.
The Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope
Authors: Filippenko Alexei V. , Li W. D. , Treffers R. R. , Modjaz Maryam 
Published: July 2016

AbstractThe Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory is a fully robotic 0.76-m reflector equipped with a CCD imaging camera. Its telescope control system checks the weather, opens the dome, points to the desired objects, finds and acquires guide stars, exposes, stores the data, and manipulates the data without human intervention. There is a 20-slot filter wheel, including UBV RI. Five-minute guided exposures yield detections of stars at R ≈ 20 mag when the seeing is good (≤2″).One of our main goals is to discover nearby supernovae (SNe; redshifts generally less than 5000 km s−1), to be used for a variety of studies. Special emphasis is placed on finding them well before maximum brightness. A limit of ~ 19 mag is reached in the 25-sec unfiltered, unguided exposures of our Lick Observatory Supernova Search (LOSS). We can observe over 1200 galaxies in a long night, and we try to cycle back to the same galaxies after 3 to 4 nights. Our software automatically subtracts template images from new observations and identifies supernova candidates that are subsequently examined by student research assistants. LOSS found 20 SNe in 1998, 40 in 1999, and 36 in 2000, making KAIT the world’s most successful search engine for nearby SNe. We also find novae in the Local Group, comets, asteroids, and cataclysmic variables. Multifilter follow-up photometry is conducted of the most important SNe, and all objects are monitored in unfiltered mode. A Web page describing LOSS is at http://astro.berkeley.edu/~bait/kait.html.
Optical Identification of Gamma-Ray Bursts at Kenting Observatory
Authors: Sun Wei-Hsin , Tseng Shun-Tang 
Published: July 2016

AbstractA remotely-controlled observing station, the Kenting Observatory, has been established in the Kenting National Park, at the southern tip of Taiwan. There are four observing systems at the Observatory: (1) a Meade 16-inch reflector with an SBIG spectrograph plus an SBIG STV; (2) an RC-16inch reflector with an FLI CCD; (3) a Celestron 14-inch with an ST-7E CCD; and (4) a Binocular system of two Canon F1.8 telephoto lens with two FLI CCDs. One of the scientific tasks of this observatory is to provide fast response to satellite alerts in the hopes of identifying the optical counterparts of Gamma-Ray Bursts (GRBs) via the global effort of GRB Coordinated Network (GCN). In this conference proceedings, we describe the instruments and the science projects being carried out in the Observatory.
Observations of Variable Stars by the 76-cm SuperLight Telescope of NCU
Authors: Li J.Z. , Wu C.H. , Zhang Z.W. , Chang C.P. , Lin C.Y. , Li H.H. , Tsay W.H. , Ip W.H. , Chen W.P. 
Published: July 2016

AbstractThe self-constructed Super-Light telescope of the National Central University is now ready for open use. Systematic studies of RR Lyraes stars and other variables are outlined and some preliminary results are introduced.
The Role of Small Telescopes in the Discovery and Follow-up of Near Earth Objects
Authors: Boattini Andrea 
Published: July 2016

AbstractThe discovered population of Near Earth Objects (asteroids and comets) consists of more than 1,300 bodies. Small telescopes provided with a large field of view have played a major role in the field, contributing to the discovery of about 95% of the total known population. We present a brief summary of the steps that have led to the present knowledge and suggestions to improve it. A proposal for accessing archival images to search for previous apparitions is presented.
The Confrontation of Mean-Field Theories with Numerical Simulations
Authors: Krause Fritz 
Published: July 2016

AbstractThe investigation of magnetic phenomena on the Sun is confronted with the problem of turbulently moving electrically conducting media in rotating objects. One way of attacking this complicated problem, which was at first successful, was the development of mean-field magnetohydrodynamics, where the cooperative action of the small-scale turbulence was taken into account by certain average effects. The development of more and more powerful computers now offers possibilities of calculating the small-scale phenomena in a direct way. This paper is an attempt to compare these approaches, at least as far as there are comparable results.
Convective Overshoot as a Source of Helicity
Authors: Jennings R. L. 
Published: July 2016

AbstractIn order to understand what happens in the Sun when convection overshoots into the radiation zone an idealized model of penetrative convection with rotation is studied. Here we highlight two properties of the model which occur with parameters relevant to the Sun. Firstly rotation allows motions to persist far beneath the convection zone, and secondly the profile of helicity with depth is dominated by a local maxima just beneath the convection zone. This second result has consequences in dynamo theory.
Diffusion of Particles, Heat and Magnetic Fields in Compressible Turbulent Media
Authors: Dolginov A.Z. , Silant’ev N.A. 
Published: July 2016

AbstractA new method for the calculation of kinetic coefficients is presented. This method allows us to obtain the distribution of scalar and vector fields (such as the temperature, the admixture particle number density and the magnetic field) in turbulent cosmic media with any value of S = u0т0/R0. The explicit expression for the “turbulent” diffusivity DT is obtained. In some cases DT becomes negative, implying the clustering of the admixture particles in patches (a local increase of the temperature and magnetic fields). The magnetic α-effect is considered for the case S ~ 1.
The Role of Overshoot in Solar Activity: A Direct Simulation of the Dynamo
Authors: Brandenburg A. , Jennings R.L. , Nordlund Å. , Stein R.F. , Tuominen I. 
Published: July 2016

AbstractWe investigate convective overshoot in a layer of electrically conducting fluid. The radiative conductivity is assumed to be larger in the lower part of the layer which makes it stable to convective motions, yet penetrative convection from the upper layer can occur. The numerical resolution is 633 gridpoints. We observe a dynamo effect for magnetic Reynolds numbers around one thousand when a magnetic seed field is rapidly concentrated to form flux tubes. Later the average magnetic field is expelled from the convectively unstable regions, but it accumulates in the interface between the convection zone and the radiative interior.
Fractal Flux Tubes of the Solar Magnetic Field
Authors: Ruzmaikin Alexander , Sokoloff Dmitry , Tarbell Theodore 
Published: July 2016

Abstract The small-scale solar magnetic field exceeding a given threshold forms a fractal set. A dimension of this fractal is found from magnetograms with varying linear resolution. The dimension depends on the value of the threshold magnetic field (multifractality). A simple dynamo model explaining the origin of the fractal magnetic structure is considered. The dynamo produces a magnetic field in the form of flux tubes with a fractal distribution of magnetic field across the tube. The observed dimension gives a possibility of estimating a degree of structuredness of the solar velocity field.
Learning about Stellar Dynamos from Long–term Photometry of Starspots
Authors: Hall Douglas S. 
Published: July 2016

AbstractSpottedness, as evidenced by photometric variability in 277 late-type binary and single stars, is found to occur when the Rossby number is less than about 2/3. This holds true when the convective turnover time versusB–Vrelation of Gilliland is used for dwarfs and also for subgiants and giants if their turnover times are twice and four times longer, respectively, than for dwarfs. Differential rotation is found correlated with rotation period (rapidly rotating stars approaching solid-body rotation) and also with lobe-filling factor (the differential rotation coefficientkis 2.5 times larger forF= 0 thanF= 1). Also reviewed are latitude extent of spottedness, latitude drift during a solar-type cycle, sector structure and preferential longitudes, starspot lifetimes, and the many observational manifestations of magnetic cycles.
Limits on the Magnetic Flux of a Pre-Main Sequence Star
Authors: Basri G. , Marcy G.W. 
Published: July 2016

AbstractWe attempt to detect a magnetic field on the weak T Tauri star, TAP35, via the enhanced equivalent widths of Zeeman-broadened absorption lines. We synthesize 25 Fe I lines, having a range of Zeeman sensitivities, using an LTE Stokes line-transfer calculation. The oscillator strengths of all lines are empirically determined a priori using the same line-transfer code applied to the spectrum of the magnetically quiet star, τ Ceti. The Fe abundance of TAP35 was established by synthesizing lines that are insensitive to Zeeman splitting. We find that the equivalent widths, Weq, of Zeeman-sensitive lines in TAP35 are systematically enhanced relative to the Zeeman-insensitive lines, consistent with the presence of widespread, kilogauss fields. The excess Weq can be explained by a product of field strength and surface filling factor (Bf) of 1 kiloGauss. A strong upper limit can be placed on the product of those two quantities, Bf < 2 kG. This measurement bears on the physics of T Tauri coronae, chromospheres, dynamos, and accretion-disk boundary layers.
Nuclear Processes Related to the Ap Stars and the Heaviest Chemical Elements
Authors: Kuchowicz B. 
Published: July 2016

SummaryIsotopic shifts in the lines of the heavy elements in Ap stars, and the characteristic abundance pattern of these elements point to the fact that we are observing mainly the products of rapid neutron capture. The peculiar A stars may be treated as the show windows for the products of a recent r-process in their neighbourhood. This process can be located either in Supernovae exploding in a binary system in which the present Ap stars were secondaries, or in Supernovae exploding in young clusters. Secondary processes, e.g. spontaneous fission or nuclear reactions with highly abundant fission products, may occur further with the r-processed material in the surface of the Ap stars. The role of these stars to the theory of nucleosynthesis and to nuclear physics is emphasized.
Element Identifications in Chemically Peculiar Stars of the Upper Main Sequence
Authors: Cowley Charles R. 
Published: July 2016

SummaryThe element identification procedures introduced by Hartoog et al. (1973) have now been applied to some 55 stars including 9 “normal” stars. We have searched for 92 elements, usually in two stages of ionization using, almost exclusively 2.4 Å/mm plates. The results that we wish to report are summarized below:1.A search for ten actinides, using some unpublished material generously provided by Drs. Worden, Fred and Crosswhite was entirely negative. Only uranium and probably thorium in HR 465 at rare earth (RE) maximum have statistical support for their presence, although uranium may be present in other stars.2.We have found no credible evidence for any rare earth in any manganese star. This is a rather basic difference between the spectra of the manganese stars and the Am stars. Calculations show that the rare earth abundances could be rather similar in the Am and Mn stars.3.We confirm the result of Jones, Wolff and Bonsack (1974), that Ho is present in HD 51418. HR 465, (at RE max) is the only other star for which we have statistical support for a Ho identification. We have not analyzed HD 101065. The heaviest lanthanide that we have identified is Er, again in HR 465 at RE maximum.4.Spectral similarities of some of the cool magnetic Ap stars and certain Am stars are remarkable, and deserve more consideration. For example, 32 Aqr an extreme Am, has about the same Strömgren 4-colors as γ Equ. With the exception of Call, the line spectra of the two stars are extraordinarily alike, and make it difficult to believe that the two objects are unrelated.5.We have published (or have in press) an examination of the odd - Z anomalies which appear in the manganese stars at P, Ga, and Y. These peculiarities are extremely difficult to explain with conventional nucleosynthesis. However, we note that slow rotation alone does not appear capable of producing the anomalies.6.The abundance variations among the lanthanides among the magnetic Ap stars are large and definite.The rich variety in the abundance patterns that we have observed is not readily accounted for by any of the current theories of Ap star abundances.
Positioning with the Global Positioning System
Authors: Goad Clyde C. 
Published: July 2016

AbstractThis year (1980) the U. S. Department of Defense has scheduled to have in operation six satellites of the Global Positioning System (GPS), which will provide timing and three dimensional position recovery potential to North America during certain segments of a day. By the mid-eighties, continuous timing and three dimensional recovery from 18 GPS satellites are planned. Although the GPS is designed for fast position recovery to the 10-meter level, extended data collection periods could yield subdecimeter relative positioning on a routine basis.
Relationship between Terrestrial and Satellite Doppler Systems
Authors: Lachapelle Gérard , Kouba Jan 
Published: July 2016

AbstractClassical horizontal geodetic networks are commonly combined with space observations, mostly satellite Doppler, in order to optimize the accuracy of geodetic control points and, thus, satisfy as many types of users as possible. Since satellite Doppler observations refer to a fully defined three-dimensional reference system and terrestrial observations, through the presence of Laplace stations (astronomical longitude and azimuth), contribute also to the pole and longitude orientations, it is imperative to ensure the highest possible degree of compatibility between the astronomical and satellite Doppler systems to maintain optimization of the accuracy of control points. Since gravity and geopotential (in the form of spherical harmonics) data are usually combined to evaluate geoid undulations and deflections of the vertical which are in turn used to reduce terrestrial angular and range observations, it is equally imperative to ensure that the satellite Doppler system and that of the geopotential solution are truly geocentric and thus compatible with the gravity data which should refer to a single equipotential surface. In order to estimate the degree of compatibility in terms of longitude orientation between satellite Doppler and geodetic astronomical systems as realized by current observations, astrogeodetic (based on CIO pole, BIH longitudes, and NWL9D satellite Doppler system) and gravimetric deflections of the vertical were compared at several hundred stations of the Canadian geodetic framework and U.S. transcontinental traverse. It was found that, when using the U.S. data subset only, incompatibility between the zero geodetic meridian plane of the NWL9D system and the zero astronomic meridian plane of the BIH was of the order of 08, which is in good agreement with previous results. However, inter-comparisons between various North American subsets revealed inconsistencies between areas of up to 08 (between Canadian and U.S. geodetic astronomical longitude observations). These results are based on the assumption that gravimetric deflections are bias free. The geocentricity of the NWL9D system with respect to other systems such as the Goddard Earth Models and SAO Standard Earths is also analyzed by comparing satellite Doppler derived geoid undulations with GEM and SAO SE undulations. An incompatibility of 4 m in Z (axis) exists between the origin of the NWL9D system and that of the other systems.
The Reference Frames and a Transformation of the Spherical Functions
Authors: Shkodrov V. G. 
Published: July 2016

AbstractThe use of spherical functions in dynamical problems is very common. As a rule, they arise in perturbing functions. It is well known that passing from one reference frame to another is accompanied by a double transformation of the perturbation function. That is why problems lose their simplicity and elegance. The problem of two solid bodies is a typical example in this respect.In the present paper the questions connected with the transformation of the spherical functions when passing from one reference frame to another frame are considered. Traditional functions are generally unsuitable as they introduce a series of difficulties in the problems. That is why complex spherical functions are used. The transformation of spherical functions due to rotation of the coordinate frame is made by means of the Wigner’s functions. When translating the frame the Clebsch-Gordon’s coefficients are used.
The Application of Faint Minor Planet Dynamics to the Problems of Improving the Fundamental Reference System
Authors: Hemenway P. D. , Duncombe R. L. 
Published: July 2016

AbstractThe underlying method of forming the adopted Fundamental Reference System is the compilation of observations referred to some (independent) well defined coordinate systems. If the observations themselves are used to define the independent coordinate system, they may be used to help establish the Fundamental System. If the observations are differential, they may be used to refer star positions to the Fundamental System and/or smooth systematic irregularities within the Fundamental System.
Comments on Conventional Terrestrial and Quasi-Inertial Reference Systems
Authors: Kovalevsky Jean , Mueller Ivan I. 
Published: July 2016

AbstractAfter commenting on certain definitions related to both the terrestrial and celestial (quasi-inertial reference systems (CTS and CIS) to clarify terminology, the geodynamic requirements for such systems are reviewed. This is followed by a discussion of certain problematic aspects of the two systems. The article concludes with a list of required actions aimed to assure that the reference system issue is resolved early. The list is proposed for the joint IAG/IAU working group to be established in accordance with the Colloquium resolution printed elsewhere in this volume.
A Wave Model for Dwarf Novae
Authors: Sparks Warren M. , Kutter G. Siegfried 
Published: July 2016

AbstractThe rapid coherent oscillation during a dwarf nova outburst is attributed to an accretion-driven wave going around the white dwarf component of the binary system. The increase and decrease in the period of this oscillation is due to the change in the velocity of the wave as it is first being driven and then damped. Qualitatively, a large number of observations can be explained with such a model. The beginnings of a mathematical representation of this model are developed.
α-Stability Analysis of Hydromagnetic Instabilities in Stars with Toroidal Magnetic Fields
Authors: Goossens M. , Biront D. 
Published: July 2016

Abstractα-stability analysis is used to investigate the adiabatic stability of a star containing an axisymmetric toroidal magnetic field. Necessary and sufficient conditions for α-stability are derived. Special attention is devoted to the typical hydromagnetic instabilities that can be introduced by a weak toroidal magnetic field in a star that is stably stratified in the absence of any magnetic field. An expression for the maximum growth rate of instability is derived and the basic properties of the displacement fields associated with the instabilities are indicated.
The system Spora
Authors: Lavrov S. 
Published: July 2016

“SPORA” is an abbreviation for “Software Package Oriented to Research in Astronomy” (in Russian – “Specializirowannoie Programmnoie Obespechniie Rabot po Astronomii”).The system is designed for the wide range for users who are not inclined to call themselves computer programmers. We assume that most of them only wish to state their problems as simply as possible – just to say which information they have and what they want to get. On the other hand some of these users have rich programming experience and they are fond of using sophisticated languages, like PL/1 or ALGOL 68, and writing complicated programs.
Catalogue of planetary nebulae and their nuclei
Authors: Acker A. , Marcout J. 
Published: July 2016

Since the catalogue by Perek and Kohoutek (PK) has been printed in 1967, numerous observations and theoretical studies have been made, and new planetary nebulae (NP) have been discovered, in addition to the 1036 PN indexed by PK. We have compiled a bibliographic index from 1965, covering about 80 papers per year; a catalogue of 1455 PN and a bibliographic index have been established (Acker, Marcout, Ochsenbein, 1981).Now, two important catalogues are being compiled which result from the joint work of the Observatories of Strasbourg, Bordeaux, Marseille, the Laboratory of Astronomy of Montpellier, and the Observatory of Haute Provence.
The Canada-France-Hawaii Telescope
Authors: Bely Pierre Y. , Lelièvre Gérard 
Published: July 2016

AbstractVisiting astronomers have now used the CFH telescope for 18 months in the prime focus and coudé configurations. Many observers have reported very good image quality and high resolution plates have already been obtained. The general concepts and technical details of the telescope and observatory are discussed. The focal plane instrumentation includes more than 25 instruments and detectors, and these are also discussed.
Un Spectrographe a Reseau Aspherique pour Telescope f/4
Authors: Lemaître G. 
Published: July 2016

AbstractAspheric diffraction gratings have been produced by the elastic relaxation method. These gratings lead to more efficient spectrograph mounting arrangements since, for a wide field instrument of fast aperture ratio, a smaller number of optical surfaces are required. The UV-PRIM spectrograph is the first instrument of this type to have been constructed.