bluuebunny/crossref_metadata_2025 huggingface dataset:
Ultraviolet Variability of AX Persei
Authors: Mikolajewska Joanna
Published: July 2016

Recent photometric and spectroscopic observations suggest AX Per might be an eclipsing binary with a period of about 682 days (Kenyon 1986 and references therein). The analysis of optical spectra taken during 1979-1986 has shown periodic minima in all observed permitted lines and a lack of any periodicity in the forbidden lines (Mikolajewska 1987; Mikolajewska & lijima 1987). A comparison of the available radial velocities with these intensity variations shows that the behaviour of emission lines is consistent with the eclipse interpretation, however the minima (especially in HI and HeI) are too broad to be consistent with eclipses even by a Roche lobe filling red giant. In the following, the UV behaviour of AX Per is analysed using IUE spectra collected during the period 1979-1984.
Concluding Remarks
Authors: Friedjung M.
Published: July 2016

After a brief description of the difficulties and pitfalls of finding a correct interpretation of the symbiotic phenomenon, I emphasize what I consider to be the highlights of the meeting. Directions for future research are indicated.
Remarks on the MK System
Authors: Morgan W. W.
Published: July 2016

The principal domain for the determination of the fundamental reference stars is K - Hβ (3930 - 4860 Å/mm). A certain amount of classification has been carried out in the visual and near ultraviolet regions; however, in neither case has a serious attempt been made to go to the practicable limit in accuracy. It can thus be said that the “field” for the determination of the fundamental MK standards has been K - Hβ.
Changing Emphases in Spectral Classification
Authors: Keenan P. C.
Published: July 2016

The definitions and general principles of the MK system given in the statement by Dr. Morgan, which Dr. McCarthy has read to you, are an expression of my views also.

It is mainly in specifying the MK domains that modifications are necessary for the cooler stars - and these for rather obvious reasons. For example, the spectral range has been extended to longer wavelengths, particularly for stars showing strong molecular bands. The lines and bands in the visual and far red regions are particularly useful in defining temperature and chemical composition, but the blue region remains important as having the features most sensitive to luminosity.
Comments on the Detection and Classification of Compact Emission-Line Galaxies
Authors: Kinman T. D.
Published: July 2016

Four methods for finding emission-line galaxies have been compared. Method (a) uses the ultraviolet excess, as found either by filter photography (Haro 1956) or by objective prism spectra (Markarian 1967). glanco (1974) introduced a thin prism with the CTIO Schmidt (1740 Å mm-1 at Hβ) which with IIIa-J plates [Method (b)] gave enough resolution for Smith (1975) and MacAlpine et al. (1977a, 1977b) to detect and classify galaxies by strong emission lines. Following a suggestion by McCarthy that even higher dispersion might be useful, I have used the CTIO Schmidt with [Method (c)] the 4° prism, a GGl+55 filter and IIIa-J emulsion and with [Method (d)] the 10° prism, an RG630 filter and IIIa-F emulsion. These latter give about 400 Å mm-1 at Hβ and Hα respectively which improves the visibility of emission lines against the galaxy continuum so that [0111] 5007 and 4959 and Hβ can be seen on the green plates and Hα and [SII] 6725 can be seen on the red plates.
Observation of the Spectra of Stars in the Same Photometric Boxes
Authors: Jaschek M. , Jaschek C. , Chmielewski I.
Published: July 2016

We have started at the OHP observatory an observing program for classifying stars in Golay’s boxes of photometrically identical stars. So far 380 stars have been observed at 80 Å/mm dispersion, covering the range from BO to G8. The main result is that stars belonging to the same box are spectroscopically identical at this dispersion if one considers classifications taken from different well experienced observers. This remains true within the current errors of spectral classification. The problem presented by the Ap and Am stars is discussed in detail.
Spectroscopy with New Detectors
Authors: Spinrad H.
Published: July 2016

Modern digital spectrophotometric devices allow for a much more rapid gathering of spectroscopic data on stars and galaxies. Colors and line strengths can lead to new classification schemes, and/or physical interpretations of much fainter objects than previously possible. However, the same old conceptual problems of interpretation (e.g. in abundances of G and K stars) remain a serious difficulty. Illustrations of these accomplishments and problems are given.
Future Developments in Classification
Authors: Code A. D.
Published: July 2016

Future advances in spectral classification are considered in terms of the likely effects of the following four factors: 1. observation from space; 2. new instrumentation developments; 3. modern data processing techniques; 4. the impact of new observations and astrophysical theory.
The Effective Temperature Distribution Function of Cataclysmic Variable White Dwarfs
Authors: Sion E.M.
Published: July 2016

With the recent detection of direct white dwarf photospheric radiation from certain cataclysmic variables in quiescent (low accretion) states, important implications and clues about the nature and long-term evolution of cataclysmic variables can emerge from an analysis of their physical properties. Detection of the underlying white dwarfs has led to a preliminary empirical CV white dwarf temperature distribution function and, in a few cases, the first detailed look at a freshly accreted while dwarf photosphere. The effective temperatures of CV white dwarfs plotted versus orbital period for each type of CV appears to reveal a tendency for the cooler white dwarf primaries to reside in the shorter period systems. Possible implications are briefly discussed.
A Photometric and Spectroscopic Comparison of the Cataclysmic Variables on the 2 Sides of the Period Gap and at a Specific Orbital Period
Authors: Szkody P.
Published: July 2016

New and previously existing photometric colors and spectroscopic H and He line strengths are used to compare CV disk systems below the period gap (P=80–130 min) with those directly above (P=190–240 min). Significant differences are found in the mean U-B,V-J colors and in the Hβ equivalent widths on the 2 sides of the gap. A detailed comparison from UV-IR of 3 high inclination novalike systems with periods near 3.3 hr (PG1012−029, PG1030+590 and V1315 Aql) shows similar continuum distributions (and implied mass accretion rates) but large differences in high excitation lines (HeII1640,4686;CIV1550).
Observations of Eclipsing Dwarf Novae
Authors: Wood J.
Published: July 2016

High Speed Photometry of four eclipsing dwarf novae, Z Cha, OY Car, HT Cas and IP Peg, is used to determine the orbital parameters and the masses of the two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in the ingress and egress of the eclipse of the compact part of the bright spot. The theoretical stream width indicates that the centre of the stream must intersect the bright spot close to this point.
Continuum Distributions and Line Profiles of UX UMa-Type Novalike Systems
Authors: Haug K.
Published: July 2016

Combined UV, optical and, in part, IR continuum distributions of the UX UMa-systems CPD-48°1577, V3885 Sgr, RW Sex and of the recently discovered cataclysmic system PHL 227 were determined from multi-wavelength spectroscopic and photometric data to search for general characteristics of these systems. The observed variations of the UV to IR spectral indices are qualitatively very similar for all systems, whereas the absolute values show significant differences in the far and near UV ranges. The wavelength dependence of the optical and IR spectral indices as well as the variations of the Balmer line profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.
The Ultrashort Period Dwarf Nova SW Ursae Majoris
Authors: Shafter A.W. , Hill J.A. , Robinson E.L. , Szkody P. , Thorstensen J.R. , Wood M.A.
Published: July 2016

SW UMa is an unusual dwarf nova in several respects. Recent observations by Robinson et al. (1986) have established that SW UMa is an SU UMa system, while Shafter, Szkody, and Thorstensen (1986) have presented evidence suggesting that SW UMa may be a DQ Her system as well. If the DQ Her classification is confirmed then SW UMa will be the only system to have this dual classification. Finally, time resolved spectroscopy of SW UMa has revealed the presence of an S-wave component in the Ha emission which has an unexpected phasing relative to the line wings.
Red Spectroscopy of IP Pegasi
Authors: Martin J.S. , Jones D.H.P. , Smith R.C
Published: July 2016

Time resolved spectroscopy of the dwarf nova IP Pegasi in the range λλ 7670–8320Å shows absorption lines originating from the cool secondary. A radial velocity curve for this component has been derived by cross-correlation with a normal M star. The curve has semi-amplitude K2 = 288.3 ± 4 km s−1, and is slightly distorted. This distortion is equivalent to an orbit with an apparent eccentricity of 0.075 ± 0.024. The mass function of the primary is 0.394 ± 0.016M⊙. From this we derive constraints on the component masses of 0.62 < M1 < 1.14M⊙ and 0.17 < M2 < 0.71M⊙. The red star has a radius in the range 0.32 < R2 < 0.51R⊙ and is probably on the main sequence.
Mass Transfer and Line Profiles - WZ Sge
Authors: Šima Z. , Hadrava P.
Published: July 2016

The calculation of a gas stream offers two modes of the stream. In any case the stream cannot be detected optically. The calculated line profiles caused by the disc are demonstrated.
Spectroscopic Evolution of Nova Vul 1984 No. 1 (PW Vul) and No. 2
Authors: Rosino L. , Iijima T.
Published: July 2016

Spectroscopic observations of two novae (Nova Vul 1984 No. 1 and No. 2) have been carried out at the Asiago Observatory from the moment of their discovery up to now. A short preliminary description of the spectral characteristics and evolution of these two novae is reported together with a brief comparison of their properties.
X-Ray Observations of Cataclysmic Variables
Authors: Osborne J.P.
Published: July 2016

The X-ray observatory EXOSAT spent over 1000 hours observing cataclysmic variables. Some of the major results reviewed here are: soft X-ray light curve changes in AM Her objects, orbital effects in the X-ray light curves of intermediate polars and U Gem, regular behaviour in the inter-outburst X-ray flux of VW Hyi, and X-ray emission from the tenuous remnant of the recent recurrent nova RS Oph. The ability of EXOSAT to make long uninterupted observations at high sensitivity over a broad spectral range and to react quickly to cosmic events has yielded a dataset of a quality that will not be surpassed for many years.
A Simultaneous X-Ray and Optical Study of TT Arietis
Authors: Hudec R. , Valníček B. , Peřesty R. , Wenzel W. , Richter G.A. , Goetz W. , Hacke G. , Huth H. , Schult R. , Pfau W. , Reimann G.-H. , Stecklum B. , Tremko J. , Mrkos A. , Schpitshka I.V. , Kojevnikov V.P. , Kumshiashvili M.I. , Oprescu G. , Dumitrescu A. , Cristescu C. , Bojack W. , Patkós L. , Toth I. , Oláh K.
Published: July 2016

Prelimary results of an extended program of coordinated X-ray and optical observations of TT Ari are presented. The object was observed on August 21/22 1985 both in X-rays (EXOSAT) and optical range, about 100 days after the return to the active state. The first detailed simultaneous study of TT Ari in active state indicates the presence of strongly absorbing structure in the system.
Implications from the Shape of the Viscosity-Surface Density Relation
Authors: Meyer-Hofmeister E.
Published: July 2016

We present results of new vertical structure computations for cool, convective accretion disks. The influence of the uncertainty in the low temperature opacities on the cool branch of the viscosity-surface density relation is investigated. We discuss how the shape of this relation allows a prediction of temperatures in the accretion disk during the onset of an outburst and we compare this with observations for VW Hydri by Hassall (1984).
White Dwarf Models of Supernovae and Cataclysmic Variables
Authors: Nomoto K. , Hashimoto M.
Published: July 2016

If the accreting white dwarf increases its mass to the Chandrasekhar mass, it will either explode as a Type I supernova or collapse to form a neutron star. In fact, there is a good agreement between the exploding white dwarf model for Type I supernovae and observations. We describe various types of evolution of accreting white dwarfs as a function of binary parameters (i.e, composition, mass, and age of the white dwarf, its companion star, and mass accretion rate), and discuss the conditions for the precursors of exploding or collapsing white dwarfs, and their relevance to cataclysmic variables. Particular attention is given to helium star cataclysmics which might be the precursors of some Type I supernovae or ultrashort period X-ray binaries. Finally we present new evolutionary calculations using the updated nuclear reaction rates for the formation of O+Ne+Mg white dwarfs, and discuss the composition structure and their relevance to the model for neon novae.
Possible Role of the White Dwarf in Grain Formation in Cataclysmic Variable Systems
Authors: Albinson J.S. , Evans A.
Published: July 2016

We consider the possibility that carbon, in the form of the allotrope carbyne, might form in the atmosphere of the white dwarf in a cataclysmic variable system, and be expelled from the system by radiation pressure. It seems that, under some circumstances, cataclysmic variable systems may indeed have carbon dust in their vicinity.
The Kukarkin-Parenago Relation for Dwarf Novae and Novae
Authors: Antipova L.I.
Published: July 2016

The period-amplitude relation and the period-energy relation for dwarf novae and novae are discussed. The total outbursts energy is shown to be a more suitable characteristic of the outburst than its amplitude.
Optical Short-Time Variations in GK Persei during the 1983 Outburst
Authors: Steinle H. , Pietsck W.
Published: July 2016

During the August 1983 outburst of the old nova GK Persei observations with EXOSAT showed for the first time a 351 second periodicity in X-rays.

Our fast photometry (U(B)V with 25 sec time resolution) was made at the end of the outburst in the nights of September 29 , and October 1–3 , using the 2.2 meter telescope at Calar Alto (Spain).

Optical variations up to 10% in U and 4% in V with periodicities in the range 350 to 360 seconds were found, lasting only for few cycles.

A comparison with the extrapolated prediction of the X-ray maxima did not show a coincidence, but rather an anticoincidence in several cases. This supports a model of reprocessed X-rays at the inner edge of an accretion disk.
The Nature of Recurrent Novae
Authors: Webbink R.F. , Livio M. , Truran J.W. , Orio M.
Published: July 2016

The observational properties and outburst histories of each member of the small class of recurrent novae are reviewed, with the objective of identifying the outburst mechanisms for these systems. Examples are found of both accretion-powered outbursts (T CrB and RS Oph) and thermonuclear-powered outbursts (T Pyx and U Sco). Outburst properties which might be used in future to distinguish between these mechanisms are identified. Many erstwhile recurrent novae (VY Aqr, RZ Leo, V616 Mon, V1195 Oph, V529 Ori, WZ Sge, and V1017 Sgr) appear to be misclassified examples of other types of cataclysmic variables.
Observational Evidence for the Two Types of Dwarf Nova Outbursts
Authors: Smak J.
Published: July 2016

Observed characteristics of outbursts of eight dwarf novae are compared with those predicted for the two types of outbursts by the disk instability theory. OY Car, U Gem, VW Hyi, and WX Hyi are identified as Type A, while RX and, SS Cyg, AH Her, and CN Ori - as Type B.
Zeeman Features from Accretion Columns in AM Herculis-Type Systems
Authors: Wickramasinghe D.T. , Tuohy I.R. , Visvanathan N.
Published: July 2016

Absorption features seen in the bright phase spectra of E1405−451 are identified with Zeeman features of Hα originating from cool (T-104-105 °K) material surrounding the accretion shock. The presence of apparently unshocked material surrounding the cyclotron emission region is surprising and may indicate that accretion occurs onto a larger fraction of the stellar surface than had previously been thought possible.
Changes in the Soft and Hard X-Ray Light Curves of the AM Her Object E1405−451
Authors: Osborne J.P. , Cropper M. , Cristiani S.
Published: July 2016

The preliminary results of EXOSAT and contemporaneous optical observations of E1405−451 (V834 Cen) in 1985 and 1986 are presented. In the latter of the two observations the soft X-ray light curve was observed to be quite different to that seen in all previous observations, but similar to the optical light curve and the new soft X-ray light curve of E2003+225. A phase shift of the broad soft X-ray eclipse was also observed. The hard X-ray and optical light curves have also undergone small changes.
Polarimetry of ST LMi (CW1103+254)
Authors: Cropper M.
Published: July 2016

White light simultaneous photometry and linear and circular polarimetry is presented for the AM Her variable ST LMi. Linear polarization evident throughout the faint phase is tentatively attributed to electron scattering from gas in the accretion column at heights greater than 5Rwd above the surface. The values of inclination and magnetic colatitude are revised to take into account the height and extent of the cyclotron emitting region which are also determined. A model of two closely connected emitting regions is proposed to account for the asymmetries observed in the light curve and polarization data for this and other AM Her systems. The cyclotron and hard x-ray emitting regions are found to be coincident, which eliminates the region above the shock as the source of polarized light. The shock height is found to be too low and the soft x-ray flux too large for the standard radiative shock model to apply.
Models for Optical and Infrared Polarization from CW1103+254
Authors: Chanmugam G. , Wu K.
Published: July 2016

Multiband observations of the AM Herculis-type binary CW1103+254 show significant circular polarization (~ 13%) in the J band. Recently, a model with high temperature (kT ~ 20 keV) and small dimensionless plasma parameter (Λ ~ 10 4) was suggested for the emitting region. However, it gives negligible polarization in the J band. In this paper, a method, in which the J band polarization and the peak frequency v* of the spectrum are taken into account, is used to determine T and Λ. For the viewing angle θ = 80° and the magnetic field B = 30MG, we find that kT = 5.0 keV and Λ = 106. The temperature of the emitting region is close to the value (kT = 8.7 keV) derived for the region emitting cyclotron lines in VV Puppis. If these radiations arise from the post-shock regions, then these temperatures are significantly lower than those predicted by standard accretion models or the shock structure is inhomogenous and more complex than previously assumed.
CCD Observations of X-Ray Binaries
Authors: Steinle H. , Pietsch W. , Gottwald M. , Graser U.
Published: July 2016

During two observation periods in 1984 and 1985 we monitored the faint optical counterparts of seven X-ray binaries with a CCD camera attached to the Cassegrain-focus of the 2.2 m telescope at Calar Alto , Spain. The observation periods were 1984, September 25–27 , and 1985, August 8–15.

The transient sources 4U0042+32 and 4U0115+63 showed no active state.

The search for an optical candidate of 4U0142+62 did not reveal any object mv ≤ 24 within the EXOSAT error box.

Within the EXOSAT error box of EXO2030+37 the reddest object was found to be very faint in blue in contrast to the blue Palomar plate.

The analysis of the other three observed sources 4U1837+04 , 1H1929+509 , and 4U2129+47 is not yet finalized , but no unexpected bright or faint state of the sources has been found. 4U2129+47 is still in its present low state (mv = 18) , lasting at least since 1983.
The Solution of the X-Ray Heating Light Curve for 4U2129+47/V1727 Cyg
Authors: Pavlovski K.
Published: July 2016

The X-ray heating light curve of the binary X-ray source 4U2129+47/V1727 Cgy is synthesized. A reliable solution is obtained only after accounting for the influence of an accretion disk. Model parameters achieved by the best fit are discussed. The solution is also discussed in the context of an extended OFF state.
Theoretical Line Profiles from a Symbiotic System
Authors: Schmid H.M. , Vogel M.
Published: July 2016

A model for a symbiotic system is presented which is not spherically symmetrical. The system consists of a cool, mass losing giant and a hot star. The stellar wind from the cool star is radiatively ionized by the hot companion, and the resulting nebular lines are emitted mainly close to the cool star. Due to the elliptical orbit, the line fluxes change with time because of the varying separation of the stars. The line profiles vary from symmetrical to asymmetrical, depending on the angle between the line of sight and the axis of symmetry. The calculated line profiles are compared with observed UV lines of the symbiotic star HBV 475.
Periodic Variations in the Symbiotic Star Spectra
Authors: Mikolajewska J.
Published: July 2016

Periodic variations of emission line intensities and radial velocities in three S-type symbiotic stars: BF Cyg, CI Cyg and AX Per are presented and discussed. The behavior of emission lines is different in these objects and suggests that significant differences in physical conditions and geometry may occur in these seemingly similar systems.
AG Pegasi: the Episode of Minimum 1985
Authors: Boyarchuk A.A. , Belyakina T.S. , Tarasov A.E. , Glagolevski Yu.V.
Published: July 2016

The profiles of the emission lines of Hα, HeI 587 6 and HeII 5411 in the spectrum of AG Peg obtained in the minimum of 1985 are described. The light curves in UBVRI system are presented. No indication for the presence of a magnetic field exceeding the error of observations (200 gauss) has been found.
Greek Astronomers and Their Neighbours
Authors: Pedersen Olaf
Published: July 2016

In Europe it has been customary to regard the ancient Greeks as our intellectual ancestors. Greek science was seen as the fountainhead from which modern European science ultimately derived both its existence and its characteristic features. This was not a completely empty idea. Each time a modern astronomer mentions a planet, the perigee and apogee of its orbit, its periods and their various anomalies, he is using so many Greek words. Moreover, until about a hundred years ago the extant works of the Greeks were the earliest scientific texts known to European scholars so that Greek science acquired a unique position in the European mind,and that ancient Greek culture in general became ‘classical’ and thus an ideal model or pattern for civilization as such. In consequence, the traditional European History of Science became an account of how science arose among the Greeks, how it penetrated into other cultural areas, and how it was sometimes eclipsed and again reborn in one of the so-called ‘renaissances’ of which European historians are so fond to speak.
System of Astronomical Constants in Hindu Astronomy
Authors: Bandyopadhyay Amalendu , Bhatnagar Ashok Kumar
Published: July 2016

Astronomical constants such as the length of the solar year, sidereal and synodic periods of revolutions of the Moon and five brighter planets have been computed using the system of astronomy in ancient and mediaeval India and a comparison made with their modern values. The modern values of the Moon’s inequalities have been compared with that of the earlier Hindu astronomical reckonings. Also, the Equation of the Centre of the Sun as determined in the period 500 A.D. to 1150 A.D. has been discussed in relation to corresponding modern values.
Planetary Theories in Sanskrit Astronomical Texts
Authors: Sen S.N.
Published: July 2016

The origin and development of planetary theories in India are still imperfectly understood. It is generally believed that fullfledged planetary theories capable of predicting the true positions of the Sun, Moon and Star-planets appeared in India along with the emergence of the siddhāntic astronomical literature. Before this siddhāntic astronomy there had existed the Vedāṅga Jyotiṣa of Lagadha, prepared around circa 400 B.C. in the Sūtra period more or less on the basis of astronomical elements developed in the time of the Saṃhitās and the Brāhmaṇas. This Jyotiṣa propounded a luni-solar calendar based on a five-year period or yuga in which the Sun made 5 complete revolutions. Moreover, this quinquennial cycle contained 67 sidereal and 62 synodic revolutions of the Moon, 1830 sāvana or civil days, 1835 sidereal days, 1800 solar days and 1860 lunar days. An important feature of the Jyotiṣa is its concept of the lunar day or tithi which is a thirtieth part of the synodic month. The tithi concept was also used in Babylonian astronomy of the Seleucid period. To trace the motion of the Sun and the Moon and to locate the positions of fullmoons and newmoons in the sky a stellar zodiac or a nakṣatra system coming down from the times of the Saṃhitās and the Brāhmaṇas was used. The Jyotiṣa was acquainted with the solstices and equinoxes, the variation in day-length of which a correct ratio was given. It is, however, silent about the inclination of the ecliptic, the non-uniform and irregular motion of the Sun and the Moon and various other important elements.
The Hsiu-Yao Ching and its Sanskrit Sources
Authors: Yano M.
Published: July 2016

The Hsiu-yao Ching ( HYC) is a Chinese text on Indian astrology composed in the middle of the eighth century. Its full title can be rendered as 'Good and bad time and day and beneficient and maleficient mansions and planets promulgated by Bodhisattva-Mañjuśrī and other sages'. As the title shows the book is ascribed to the legendary Mañjuśrī and other sages, but the actual author is the Buddhist monk Amoghavajra (A.0.705-774) whose native place was somewhere in north India. His Chinese name Pu-k'ung Ching-kang is a literal translation of the Sanskrit name. Like most of the texts on Buddhist astrology and astronomy, HYC is contained in Vol.21 of the Taisho Tripitaka compiled by the Japanese Buddhist scholars during the Taisho Period (1912-1926). From many corruptions in the texts it seems that the compilers were not much interested in Buddhist astrology and astronomy in general, and that they did not try to secure better manuscripts either. Specifically in the case of HYC they simply based their edition on the text of the Korean Tripitaka and put in the footnotes the variant readings found in the Chinese Tripitaka of the Ming Dynasty.
Al‘suphi’s Star-Atlases and Middle Europe
Authors: Fischer Karl A.F.
Published: July 2016

The oldest European mythological figures of the star constellations originate from the Farnesian Globe of the 3rd century B.C. The “Centaurus” with the Therion “Lupus” is the most important constellation from which I derive all the series specified. Centaurus holds the wolf with one hand on the hind leg; in the other hand he holds a lance with which he cuts the wolf’s throat. This constellation is incorrectly drawn in the first publication of the Farnesian Globe by Bianchini. These antique figures were the pattern for Cod. Vind. 5415, probably by John Dorn, a Dominican, who made also the globe of Bylica at the Budinian court of the king Mathias. This globe is at present the property of the University-Museum of Krakau. The antique constellation-forms were the pattern for the celestial maps of Sebastian Sperantius of Nurnberg in 1503. Due to Albrecht Durer these mythological figures of the constellations re-appeared in the renaissance. We can find them by John Honterus, John Middoch, on many globes for example that of Coronelli, or of the manuscript globe of the Bibiliotheca Cassanatense in Rome of Moroncelli from the year 1716. They survived till modern times in the “Uranometria” of John Bayer, in the star-atlases of John Flamsteed, John Erlet Bode as well as in the latest star atlas with allegoric figures of Rudiger-Meisner from the year 1805.
A Moorish Astrolabe from Granada
Authors: Firneis Maria G.
Published: July 2016

In the course of a systematic search in the “Technical Museum” of Vienna for instruments of astronomical importance, a Moorish astrolabe with Cufic lettering was discovered by the present author. Being labelled as “sun-moon-dial” its correct function had not been recognized before or forgotten. The device came into the museum’s possession in April 1937 through exchange with a theodolite from the Jesuit College at Kalksburg where the astrolabe had been kept after it remained in Vienna during one of the two Turkish sieges of the city (probably in 1683). The brass instrument has a diameter of 15,7 cm and is well equipped with 8 ṣafīḥas ( = tympans). Its conservation state is rather good, even the original red and gold ‘ilāqa ( = cord) is in place. The specimen is of undated planispheric northern type (shamālī musattah). It shows the typical small kursī ( = throne) of occidental instruments, cast in one piece with the ḥajra (= limb) and umm ( = mater) forming the main body of the astrolabe. This fact sets it apart from instruments of European origin where the kursī sometimes was fastened with screws to the main body (W. Morley, reprinted in R. Gunther, 1976).
Old Sunspot Records
Authors: Venugopal V.R.
Published: July 2016

The works of Eddy (1976) and Clark and Stephenson (1978) on the ancient sunspot records are reviewed and a plea is made for the search for ancient records of astronomical events and phenomena in India.
Stellar Photometry with an Automated Measuring Machine
Authors: Gilmore Gerard
Published: July 2016

The combination of wide field high quality telescopes, fine grain emulsions and fast automated measuring machines offers an unrivalled opportunity for progress in statistical astronomy. This review illustrates, with examples, the many steps which are necessary to realise this potential.
Analysis of Images with the APM System at Cambridge
Authors: Kibblewhite E. , Bridgeland M. , Bunclark P. , Cawson M. , Irwin M.
Published: July 2016

The Automated Photographic Measuring (APM) system at Cambridge was started many years ago to analyse Schmidt plates, and its progress has been reported at a number of these conferences. Only brief details of its design will be given in this paper.

The system consists of a very accurate laser-beam scanning microdensitometer connected to a series of on-line computers. The microdensitometer (Figure 1) uses a 5500 kg x-y table to position the plate. The plate transmission is digitised to 12-bit accuracy at a rate of one sample every 4 microseconds, although the image processing hardware limits this speed in practice. Special-purpose hardware exists to convert the transmission measurements into density or intensity estimates, to smooth the spot-size digitally, to measure the background and to compute image parameters.
Microspots on IIIa-J Plates (“Gold Spot Disease”)
Authors: Sim M. Elizabeth
Published: July 2016

The UK 1.2 metre Schmidt Telescope at Siding Spring Observatory, Australia, has taken about 8500 plates since it was commissioned in 1973. A large fraction of these plates, including those for the southern and equatorial Sky Surveys, are on Eastman Kodak Illa-J emulsion. A significant number of these processed Illa-J plates have developed many small gold spots similar in size to faint star images. They are most likely to occur in areas of relatively high density, such as in bright star images or on the stepwedges, and are sometimes scattered around in non-image areas (fig. 1). An alarmingly high proportion of plates taken in 1974-75 (about 50 per cent) have developed gold spots, and the most recent affected plate found so far is J6517, taken in October 1980. Four early IIIa-F plates have also been found to have gold spots.
M.A.M.A. Project: A New Measuring Machine in Paris
Authors: Guibert Jean , Charvin Pierre , Stoclet Patrick
Published: July 2016

A new photographic measuring machine is under construction at Paris Observatory. The amount of transmitted light is measured by a linear array of 1024 photodiodes. Carriage control, data acquisition and on line processing are performed by microprocessors,a S.E.L. 32/27 computer, and an AP 120-B Array Processor. It is expected that a Schmidt telescope plate of size 360 mm square will be scanned in about one hour with pixel size of ten microns.
Images From Large Schmidt Telescopes
Authors: Brown D.S. , Dunlop C.N. , Major J.V.
Published: July 2016

Calculations have been made of the intensity distribution of star images formed at the focal surface of large Schmidt telescopes. The calculations take account of atmaspheric seeing, aperture diffraction, manufacturing errors, chromatic errors in the corrector plate, scattering in the emulsion, photographic response and grain structure. The results are expressed in terms of simulated microdensitometer scans across the processed emulsion.

Results are given for a system S1(1.24m, f/2.5) similar to the 48" U.K. Schmidt (with both singlet and achromat corrector plates) for several combinations of correctors and filters using Illa-J emulsion for recording. The improvement in performance expected from the use of larger Schmidt telescopes is discussed and results are given for two designs with 2.5 metres aperture, S2(2.5m, f/2.5) and S3(2.5m, f/3).
The Hipparcos Image
Authors: Gall J-Y. Le , Saisse M.
Published: July 2016

One presents hereafter the HIPPARCOS satellite payload which is mainly constituted by a Schmidt telescope; a possible way to approximate the Schmidt mirror elliptic deformation profile is explained. Then, the signal expected from the optical chain is briefly described and one displays a residual chromatic effect which may introduce errors in the measure. To conclude, numerical values of this effect are given and one shows the necessity to take it into account in the data reduction process.
Discovery of New Bright Peculiar Stars of the Northern Sky
Authors: Bidelman William P.
Published: July 2016

I am now engaged in an objective-prism program directed toward the discovery of new peculiar and interesting stars in most of the northern sky. The plates utilized are 20-min. blue exposures taken with the Warner & Swasey Observatory’s Burrell Schmidt telescope, now located on Kitt Peak. The dispersion of the spectra is 108 A/mm at Hγ, the limiting magnitude about mpg =10.5, and the plate quality generally excellent. This paper discusses the history and status of the project and gives examples of the variety of objects being found.
Present State of the Work on Automatic Spectral Classification at Tartu
Authors: Malyuto V.
Published: July 2016

An automatic spectral classification technique for objective-prism spectra is being developed.The procedure of selecting standard stars is described.The applicability of a linear polynomial regression model for choosing and calibrating the spectral criteria for Teff, Mv, [Fe/H] is demonstrated.
La Mesure Des Vitesses Radiales Avec Un Prisme Objectif Associe A Un Telescope De Schmidt
Authors: Fehrenbach Ch. , Burnage R.
Published: July 2016

Radial velocity measurements with an objective-prism mounted on a Schmidt telescope.

A 62 cm diameter objective-prism is mounted on the CNRS-University of Liège Schmidt telescope at the Haute Provence Observatory. The field is 4 x 4° and the limiting magnitude is 12.5 on IllaJ hyper-sensitised plates. The dispersion is 200 A mm-1 at 4220 A. The plates are measured with a special machine and data are reduced by means of a computer with a correlation method. Stars of all spectral types are measured. The probable error is of some 4 km sec -1 over a mean of at least 3 plates. Already several lists of radial velocities of stars belonging to field situated at -30° of galactic latitude have been published. We have also started radial velocity observations for the Hipparcos Program.
Surface Photometry of Pure Disk Galaxies
Authors: Carignan C.
Published: July 2016

Surface photometry from U.K.S.T.U. plates in U, BJ and RF is presented for the three Sculptor Group galaxies NGC 7793, NGC 247 and NGC 300. Their photometric parameters are derived and compared to those of M33. Our color maps are used to sort out the data into blue and red pixels where the blue pixels profiles are expected to be rather irregular, representative of the clumpy locations of areas of recent star formation while the red pixels profiles should approximate the smoother distribution of the old disk population.
A Survey of Southern Compact and Bright Nucleus Galaxies
Authors: Fairall A.P.
Published: July 2016

During the 1960's, Zwicky made an intensive examination of the Palomar Sky Survey plates that resulted in his “Catalogue of Galaxies and of Clusters of Galaxies” (Zwicky et al. , 1961-1968). In the course of this study, he picked up numerous examples of what he labelled as “compact galaxies and compact parts of galaxies”; five lists were initially circulated and later presented as a catalogue (Zwicky 1971). To Zwicky the “compact” connotation suggested extremely high stellar densities, but line profiles failed to reveal the large velocity distributions expected of such concentrations of stars. Nevertheless an unexpected benefit was that many of his “compact parts” turned out to be the nuclei of actives galaxies, particularly Seyfert galaxies. Furthermore, since the nuclei have to stand out to gain “compact part” status, Seyfert nuclei from Zwicky’s lists tend to be fairly extreme specimens.
The Optical Variability of 3C 446
Authors: Barbieri C. , Cristiani S. , Romano G.
Published: July 2016

3C 446 is one of the most violently variable quasars.

Its optical variability has been studied for instance by Barbieri et al. (1978), by Pollock et al. (1979) and by Miller (1981). The quasar exibits periods of prolonged activity, with amplitude exceeding 3 mag, and with intraday significant variations. We observed 3C kkG in the last month of Aug. 1983, finding the quasar of unpreceeded brightness.

Three plates were obtained with the 67/92 cm Schmidt telescope on Aug. k, 9 and 11, and in all three the quasar is seen at B=15.1, the brightest value ever recorded. We have only one previous plate of low quality taken on July 31, and 3C kkG is fainter by approximately 0.7 mag. Finally, on two plates taken the 27th of Aug. with the 182 cm telescope at Cima Ekar we see it again down to B=16.2.
The Physical Nature of the Blue Objects in the Field Of BD+15°2469 (Virgo Cluster)
Authors: Erculiani L. Abati , Lorenz H.
Published: July 2016

This is the second Asiago blue objects field studied to determine the physical nature of ultraviolet excess objects (UVX) at high galactic latitudes using low dispersion objective prism plates. As the first of this series ( Abati 1982 )this work has a double aim:

1.

to determine the proportions in the component populations of UVX objects selected by the two-colour method on Schmidt telescope plates;

2.

to determine the surface density of quasars down to a limiting magnitude m = 18 mag.
Optical Identifications of Radio Sources with Accurate Positions Using the UKST IIIa-J Plates
Authors: Savage Ann , Jauncey David L. , Batty Michael J. , Gulkis S. , Morabito D.D. , Preston R.A.
Published: July 2016

Three radio identification programmes are described which are drawn from radio samples with accurate radio positions (< 2" arc rms). Optical identifications are being made on the basis of radio-optical positional coincidence alone, without regard to colour or morphology, using the UKST IIIa-J sky survey to a limiting magnitude of 22.5. Some preliminary results are presented.
Galaxy Counts
Authors: Tyson J.A.
Published: July 2016

Counts of faint galaxies should reveal any evidence of galaxy luminosity or color evolution, as well as new information on the faint end of the galaxy luminosity function. The FOCAS automated detection and classification software is reviewed, and results of the deep 4m PF photographic survey to 24th magnitude in 23 fields covering 9 sq. degrees are presented. Color-magnitude plots for stars and galaxies are shown, and galaxy color evolution is discussed. Evidence is found for a faint galaxy blue trend at 22-24 J mag. However, the k-correction becomes so severe at redshift ~1 that the intrinsically fainter galaxies are emphasized in any magnitude-limited survey. No unambiguous evidence is found for evolution. New 4m limit CCD multi-color data are shown and discussed. The limiting magnitude for detection is 27th J magnitude in 2 hours integration. The data exclude evolution starting at any one epoch for z<10.
Superclustering and Substructures
Authors: Chincarini Guido
Published: July 2016

The history of the Universe is infinitely more interesting than the history of the study of the Universe.

- Zel'dovich and Novikov (1983) -

PROLOGUE

The understanding we have today of the distribution of galaxies resolves some of the debates which were going on in the seventies. Future data and analysis may allow us to discriminate among cosmological models.
Cosmology with the Space Schmidt Telescope - Galaxy Colors and Color Distributions
Authors: Bruzual A. Gustavo
Published: July 2016

Galaxy spectral evolutionary models are used to compute the following quantities in optical and UV bandpasses: (a) galaxy color, luminosity, two-color diagrams, and surface brightness profiles as functions of redshifty and (b) galaxy counts, and color and redshift distributions as functions of apparent magnitude. These predictions may be used as a guide to prepare and interpret observing runs with the Space Telescope, the Space Schmidt Telescope, and the Starlab Observatory.
Schmidt Astronomy and the Space Telescope
Authors: Lasker Barry M.
Published: July 2016

The Space Telescope is described from the viewpoint of its interaction with Schmidt telescopes, specifically with regard to the planning and interpretation of observations and to the construction of the Guide Star Selection System.
Iron K-Line Emission from X-Ray Binaries
Authors: Masai K. , Hayakawa S. , Nagase F.
Published: July 2016

Emission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Txof continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ∼ 100 eV formed above the accretion disk. This mechanism is attained for Tx≲ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx> 10 keV is likely due to fluorescence outside the He II ionization front.
Laser-Driven Soft X-Ray Lasing in Copper and Germanium Plasmas
Authors: Mclean E.A. , Lee T.N. , Elton R.C.
Published: July 2016

Soft x-ray lasing has been achieved for the first time on 3p-3s transitions in neon-like copper (Cu19+) and germanium (Ge22+). The elongated lasant plasma was produced using the NRL Pharos III laser operating atλ= 1.05 μm, 300–480 J with a pulse duration of 2 ns. Lasing was observed in the wavelength interval 196 to 286 Å for J = 2 → 1 and J = 0 → 1 lines, using both thin film and thick slab targets.
The Measurement and Interpretation of NeV 2–2 Line Intensity Ratios
Authors: Lang J.
Published: July 2016

A theta-pinch was used to produce NeV 2–2 spectral lines. The intensities of the lines were measured using a grazing incidence spectrometer which had been intensity calibrated by the branching ratios method. The electron temperature and density of the theta-pinch discharge were found by laser scattering. The measured intensity ratios are compared to theoretical predictions based on electron excitation rate coefficients calculated using the R-matrix close coupling method. For two of the measured ratios experiment and theory agree within the experimental uncertainty, For the other two ratios the theoretical prediction is greater than the experimental result.
Spectral Observations of the Extreme Ultraviolet Astronomical Background Radiation
Authors: Labov S. , Bowyer S.
Published: July 2016

Observations in the far ultraviolet and soft x-ray bands suggest that the interstellar medium contains several components of high temperature gas (105to 106K). If large volumes of local interstellar space are filled with this hot plasma, emission lines will be produced in the extreme ultraviolet (EUV). Diffuse EUV radiation, however, has only been detected with photometric instruments; no spectral measurements exist below 520Å. We have designed a unique grazing incidence spectrometer to study the diffuse emission between 80 and 650Å with 10 to 30Å resolution. This instrument was successfully flown on a sounding rocket in April of 1986 and a preliminary analysis reveals several features. In addition to the expected interplanetary He I 584Å emission and the geocoronal He II 304Å emission, other features appear which may originate in the hot ionized interstellar gas. These features are discussed along with the possible implications to the hot phase of the interstellar medium.
High Resolution Spectroscopy of Dite Tokamak in the 10Å Region
Authors: Dunn J. , Barnsley R. , Evans K.D. , Peacock N.J.
Published: July 2016

An account is given of the X-Ray emission from the DITE tokamak in the spectral region 4Å–10Å measured by a Johann curved crystal photographic spectrometer. This high resolution instrument has been used for detailed line identifications eg. of L-shell transitions in the Fe spectrum at wavelengths ∼8Å and of the He-like ion spectra of Al, Si and Ar. The fine structure has been resolved for H-like Mg, Al and Si. Departures from the statistical value of 0.5 forβ, the intensity ratio of the Lyman-αdoublet, have been observed. Experimental values for the fine structure separation are presented for these medium Z metals.
Spectroscopy in Ne-Like Plasmas. Z-Dependence of the Atomic Data Used in a Collisional-Radiative Model
Authors: Cornille M. , Dubau J. , Loulergue M. , Jacquemot S.
Published: July 2016

The Livermore X-ray Laser experiments in 1984 have shown the existence of Ne-like 3p-3s population inversions in a collisional Se plasma (Z=34) with significant gains (5 cm-1). We have focused our efforts on the behavior of the gains along the target neon Isoelectronic sequence. This study implies the determination of the Z-dependance of the rate coefficients of all the Involved atomic processes: collisional excitation (C). radiative decay (A) and dielectronic recombination (αd). Thus we use atomic structure and electron-ion collisional codes (SUPERSTRUCTURE. Distorted Waves. AUTOLSJ and JJOM). The different calculations have been done on a large selection of ions, from Ar to Ag. They Include relatlvistic effects in a fine structure scheme. The Z-dependance of the numerical results is expressed as polynomial or rational forms.