bluuebunny/crossref_metadata_2025 huggingface dataset:
Multiwaveband Studies of X-ray Selected Active Galactic Nuclei
Authors: Brissenden R. J. V. , Tuohy I. R. , Remillard R. A. , Buckley D. A. H. , Bicknell G. V. , Bradt H. V. , Schwartz D. A.
Published: July 2016

We report on the identifications of 15 new X-ray selected Active Galactic Nuclei (AGN). The AGN have been discovered during an ongoing program to identify and study the optical counterparts of X-ray sources detected by the HEAO-1 satellite. The new AGN add to our existing data base of 26 making a sample of 41 objects which are the subject of a multiwavelength study including radio, infrared, optical, UV and X-ray observations. As part of this study 8.4 GHz flux measurements have been made at Parkes. Radio-optical-X-ray continuum spectral index comparisons are presented.
Science with the Australia Telescope (Invited Paper)
Authors: Robinson B. J.
Published: July 2016

The research now under way with the real-time 275 km Parkes-Tidbinbila interferometer is used as a guide to the initial science to be undertaken with the 319 km Australia Telescope (AT) Long Baseline Array. On the other hand, it is risky to guess at the new science likely to be attempted with the 6 km AT Compact Array at Culgoora; instead the potential that has been built into this array is discussed and a selection of basic questions in astrophysics is posed as a guide to significant science that might yield to new observers on a fresh instrument under the southern skies. In conclusion two questions are probed: Can discoveries be made by users of national facilities? Does the AT cross into new domains in the phase space of observations?
SN 1987A: an Overview
Authors: Dopita Michael A.
Published: July 2016

A great deal has been learnt about supernovae over the last 500 days, or so. The major deficiencies in theory highlighted by the case of SN 1987A are briefly reviewed, as are the sucesses.
SN 1987A: Interpretation of Radio Observations
Authors: Manchester R.N. , Storey M.C.
Published: July 2016

The interpretation of the radio burst from SN 1987A as an expanding synchrotron source is briefly reviewed.
Recent Observational Investigations of SN 1987A at ESO
Authors: Lucy L.B.
Published: July 2016

The following are brief summaries of recent observational investigations of SN 1987A by ESO staff and their collaborators, which were reported at the Conference.
Spectral Analysis of SN 1987A: the First 7 Months
Authors: Höflich P.
Published: July 2016

Model calculations for the photospheres of SN 1987A are presented. Spherical symmetry and density profiles are assumed to be given by the homologous expansion of the stellar structure of a B3I supergiant. For later stages the density slopes are determined. For a number of elements (H, He, C, N, O, Ne, Na, Mg, K, Ca, Ba) detailed atomic models are used. The statistical equations and the radiation transport are treated consistently as well for the lines as for the continua. In addition, line blanketing due to other elements are included under the assumption of pure scattering. The importance of a sophisticated NLTE-treatment is demonstrated. Chemical metal abundances are derived by comparing the observed and synthetic spectra. Good agreement is found if a third of solar abundance for all elements with the exception of the s-process elements is assumed. An overabundance of He by a factor of 1-2 is indicated by the models corresponding to the time before June 87. No gradient in the chemical abundances of the hydrogen rich layers has to be assumed. Up to October 87 the He abundance at the photosphere is increased to 5 times solar, i.e. the continua are formed in helium rich layers. The chemical profile indicates strong mixing processes of the different layers of the progenitor during the explosion. Additionally, pecularities of hydrogen line profiles are discussed. Mainly, they can be understood by selective line blanketing effects. The total mass of the hydrogen rich shell is estimated to amount to be 9-11 M⊙.
Observations of SN 1987A in the Mid-infrared
Authors: Aitken D.K.
Published: July 2016

Mid-infrared spectroscopic data on SN 1987A are reviewed. This spectral region contains the fine structure lines of a number of ions, incuding the iron group elements, together with recombination lines of hydrogen and helium. From about 9 months all these lines and the continuum have been effectively optically thin, and the [CoII] line strength and development yields an estimate of the parental 56Ni mass of 0.071 M⊙, very similar to the light curve estimates. At one year after the explosion the velocities appropriate to the hydrogenic and ionic regions are ∼ 2000 km s−1 and ∼ 1500 km s−1, respectively.

Apart from an excess between 8–9 μm which appears to be due to molecular SiO, there is no evidence of departure of the continuum from free-free emission, and no sign of any emission from dust. From the free-free continuum an ionization fraction of a few percent is derived for the hydrogen/helium envelope; this provides relative transparency in the mid infrared while the bound electrons provide the X and γ-ray opacity which is still considerable at 15 months.

The appearance of neutral ions at 15 months indicates that the ejecta temperatures are cooling, and that dust formation may be imminent.
The Circumstellar Emission from SN 1987A
Authors: Fransson Claes
Published: July 2016

In the first part the UV and optical observations of the circumstellar gas of SN 1987A are reviewed, and the physical properties of the gas discussed. In the second part models of the emission are treated, as well as their use as a diagnostic of the radiation from the supernova during the first, unobserved hours after the explosion.
AAT Observations of the Interstellar Medium towards SN 1987A
Authors: Pettini M.
Published: July 2016

The exceptional brightness of SN 1987A has provided a unique opportunity to probe intervening gas clouds in the disk and halo of our Galaxy and in the Large Magellanic Cloud, as well as intergalactic matter between the two. At the AAO we have exploited this opportunity in two ways: in searches for very weak interstellar features requiring exceptionally high signal-to-noise ratio spectra, and in recording known interstellar lines with unprecedentedly high spectral resolution. We are also monitoring photographically the evolution of the light-echoes to map the three-dimensional distribution of interstellar matter near the supernova. Surprisingly high column densities of million-degree gas have been found in the LMC through the first detection of [Fe X] in absorption. The hot gas may fill the interior of a ‘superbubble’, created by the combined effects of previous supernovae in this active region of star-formation; this cavity may be related to the shells of interstellar matter giving rise to the light-echoes. The ultra-high resolution observations, which required the rapid construction of a dedicated new spectrograph, were successful in resolving the hyperfine structure of the sodium D lines in several interstellar clouds. This implies that the clouds are at temperatures of at most 170 K and have internal turbulent velocities of no more than 0.3 km s−1, even though some are moving with high velocities relative to the Sun.
Searches for a Pulsar in SN 1987A
Authors: Manchester R.N.
Published: July 2016

Expectations and results of searches at radio and optical wavelengths for a pulsar in SN 1987A are described.
Search for Bursts of Ultra-High-Energy Photons from Astrophysical Sources
Authors: Ciampa D. , Clay R. W.
Published: July 2016

The Buckland Park air shower array has been used for some time as an ultra-high-energy gamma-ray telescope operating at photon energies of about 1015 eV. Other such telescopes have reported apparent bursts of events from astrophysical objects under study. We report here searches for UHE bursts from 14 southern hemisphere objects studied in our UHE programme. No conclusive evidence has been found for any UHE burst activity from these sources in the period 1986-1988. There is possible evidence for activity associated with 1700-377 and SN1987A.
Do All Stars Have Magnetic Fields?
Authors: Stewart R. T.
Published: July 2016

Recent observational results are presented which strongly suggest that a much wider range of upper-main-sequence stars have appreciable surface magnetic fields than has previously been believed.
On viewgraphs and posters
Authors: Allen David
Published: July 2016

This paper discusses the techniques of presenting data both verbally, with emphasis on the use of viewgraphs, and as posters. The views expressed summarise a discussion which involved about 40 young astronomers: they are of particular relevance to those amongst us of the generation which has had these media thrust upon it without training.
History and Propaganda in Astronomy
Authors: Christiansen W. N.
Published: July 2016

‘History is Bunk’ said Henry Ford. He was exaggerating but it is well recognized that the connection between history and truth is tenuous. Even very recent history dependent on human memory is notoriously unreliable despite the intention of the historian to tell the truth.

In radio astronomy we are fortunate in having a dedicated historian-astronomer by the name of Woody Sullivan who has spent years in interviewing and reinterviewing astronomers to find out the real facts about the early years of the subject. Because of Sullivan’s work (e.g. Sullivan 1988) and because so many of my former colleagues have written histories of the period I felt very doubtful about adding my piece to the saga when asked to do so. However, I did accept the invitation to do so after I had read a statement about radio astronomy written by our usually very well informed Minister for Science, Barry Jones (Jones 1987). This statement which I shall quote later is an example of what we may call popular history.
Period Changes in the X-ray Pulsar GX 1 + 4
Authors: Greenhill J. G. , Giles A. B. , Sharma D. P. , Warren D. M. , Sprent A. , Emery M. W. , Dieters S. W. B. , Fenton K. B. , Sood R. K. , Waldron L. M. , Thomas J. A. , Mace O. , Manchanda R. K.
Published: July 2016

The binary X-ray source GX 1 + 4 was observed during a balloon flight in 1986, November. The source was in a relatively high intensity state. Time analysis of the data shows that the pulsation period was 111.8 ± 1.0 s indicating that one or more episodes of spin-down occurred between 1980 and 1986. Folded pulse profiles are very broad with an indication of a notch at the peak. Evidence has been found for a correlation between hard X-ray intensity and phase of the proposed 304 day orbital period. The time averaged intensity since 1980 is an order of magnitude lower than during the 1970’s. A survey of the post 1980 data shows that several reversals of the period derivative have occurred. Spin-up at the rates typical of the 1970’s has been followed by a dramatic spin-down episode with dP/dt>2.4 × 10−7 s/s.
A Search for and Optical Pulsar in SN 1987A using Real-Time FFT Techniques
Authors: Kroupa P. , Blair D. G.
Published: July 2016

It is shown that real-time FFT techniques used in conjunction with a small telescope can yield useful sensitivity. The suitability of the Crab pulsar as a calibrator is assessed. The mains frequency modulation in the night sky above Perth is clearly discerned, with several harmonics. Detectable signal modulation limits for SN 1987A are derived as a function of frequency in the range 10-2000 Hz.
A Southern Galactic Survey at 843 MHz
Authors: Whiteoak J. B. Z. , Large M. I. , Cram L. E. , Piestryzynski B.
Published: July 2016

The Molonglo Observatory Synthesis Telescope (MOST), operating at 843 MHz, is currently surveying the southern galactic plane (245° <l<360°, −1.5° ≤b≤ +1.5°). The resulting maps provide images of the radio continuum with a synthesised beamwidth of 43′′ × 43′′ cosec δ and a noise level of about 1mJy. The survey involves 12-hour synthesis observations of over four hundred fields on a predefined set of field centres. About half the fields have been observed to date, and the survey is scheduled for completion in 1990. A noteable feature in many of the fields is the occurrence of widespread diffuse filamentary structure, in addition to the expected supernova remants and HII regions.
G357.7-0.1—a Double-lobed Radio Source?
Authors: Caswell J. L. , Kesteven M. J. , Bedding T. R. , Turtle A. J.
Published: July 2016

The radio source G357.7-0.1 has commonly been regarded as a galactic supernova remnant; alternative interpretations have concentrated on the pronounced brightness gradient along its major axis. Analysis of our new map shows that this brightness gradient masks an even more crucial characteristic – symmetry about the centre – the key to a totally different interpretation.
A High-Resolution Acousto-Optical Spectrograph Suitable for CO Observations of Dark Clouds
Authors: Wang Jing-sheng , Robinson B. J. , Huang Geng-chen , Otrupcek Robina E.
Published: July 2016

An acousto-optical spectrograph (AOS) with a high spectral resolution of 28 kHz has been developed for spectral line observations of objects, such as dark clouds, where the line-widths are low. It has been mounted on the 4-m-diameter millimetre-wave telescope at CSIRO Division of Radiophysics at Epping, NSW and successfully tested using 115 GHz Co observations of a sample of southern dark clouds. At 115 GHz the velocity resolution is 0.07 km s-1.
What are IRAS Galaxies? An Optical Answer
Authors: Meadows V. S. , Allen D. A. , Norris R. P. , Roche P. F.
Published: July 2016

A survey of the optical spectra of IRAS galaxies, made with the AAT, has shown that the majority have strong emission lines. Ratios of the emission lines have been plotted on the Veilleux-Osterbrock diagram ([O III]/Hβ against [N II]/Hα); this shows that the IRAS galaxies comprise several classes. In our sample the majority appear to be starburst galaxies, but Seyfert, Liner and narrow-line galaxies are also represented. Co-added spectra of the galaxy classes are presented. On the basis of optical spectroscopy, it appears that the starburst phenomenon is capable of generating luminosities exceeding 1012L⊙.
2152–69: The First Image from the Australia Telescope
Authors: Norris R. P. , Kesteven M. J. , Sramek R. A. , Wilson W. E. , Brooks J. W. , Calabretta M. R. , Ekers R. D. , Nelson G. J. , Sinclair M. W. , Young A. C.
Published: July 2016

Although only three antennas of the Australia Telescope Compact Array are currently operational, we have made use of the technique of bandwidth synthesis to make an image of the radio galaxy 2152 – 69. The three baselines were used to observe the source at three different frequencies, effectively resulting in nine baselines, which have been used to produce an image with a surprisingly high dynamic range, and with a slightly higher resolution than any existing image.

The production of such a worthwhile result, despite being made with a small subset of the capabilities of the Australia Telescope, bodes well for the future operation of the instrument.
Enhanced Cosmic Ray Diurnal Variations in Mawson and Hobart Neutron Monitor and Underground Data Records
Authors: Duldig M. L. , Humble J. E.
Published: July 2016

Analysis of surface and underground detector data from Mawson and Hobart for the period 1982 to 1988 has revealed a number of episodes of enhanced diurnal variation lasting more than 5 days. A preliminary study of these enhancements shows that variations in the rigidity spectrum and in the upper limiting rigidity must be present to explain the phenomenon.
The Asteroidal Impact Rate upon the Terrestrial Planets: An Update
Authors: Olsson-Steel Duncan
Published: July 2016

The probability of a collision with each of the terrestrial planets due to each of the Aten-Apollo-Amor asteroids discovered through to 1989 May is calculated; the range of possible impact velocities is also given in each case. For Mercury there are eight possible impactors known, with a mean collision probability of 1.30 × 10−9 per year; for Venus, the 32 planet-crossing asteroids give a mean collision probability of 9.63 × l0−9 per year; for the Earth the corresponding figures are 65 and 6.93 × 10−9 per year; and for Mars, 116 and 3.41 × 10−10 per year. The rate for Mars does not include the full range of Mars-crossers (i.e. those of 1.30<perihelion distance <1.67 AU are not included here), and for the interior planets any undiscovered population of asteroids would also alter the mean probability of an impact.
Wallal: The 1922 Eclipse Expedition
Authors: Burman R. R. , Jeffery P. M.
Published: July 2016

On 1922 August 20, a 20-strong scientific team, together with a naval party of 10, left Fremantle on one of the major scientific expeditions in Western Australian history. After picking up further personnel at Broome, the party proceeded to the isolated post and telegraph station of Wallal on the northern coast of Western Australia. Their task was to measure with great care the deflection of starlight by the Sun during the total solar eclipse of 1922 September 21. Specially designed photographic equipment of very high quality was used and meteorological conditions were excellent. As a result, measurements were obtained for well over a hundred stars.
The Business of Science
Authors: Cole T. W.
Published: July 2016

In science we have good, successful laboratories and scientists and we also have wasteful, inefficient and unproductive ones. The differences are not matters of chance.

It is not an accident that just one Cambridge College, Trinity, has achieved more Nobel Prizes than all of Japan. There was something in common amongst the Nobel prize winners Todd, Adrian, Perutz, Bragg, Crick, Ryle, Hewish and Mott that I was fortunate enough to meet and, in some cases, get to know well. Of course there was the personal and intellectual calibre of these people, their drive and determination. But also, there was the laboratory culture within which they worked, a culture still benefiting from the influence of Maxwell, Thomson and Rutherford.
Radio Observations of the Einstein Deep X-ray Field in Pavo
Authors: Bedding T. R. , Turtle A. J.
Published: July 2016

The most sensitive X-ray survey available is a deep exposure made by theEinstein Observatoryof a 40 arcmin field in the southern constellation of Pavo. This survey revealed 33 X-ray sources, most of which were optically identified with quasars. Here, we report radio observations of the Pavo region at 843 MHz made with the Molonglo Observatory Synthesis Telescope. Eight overlapping fields were combined to produce the most sensitive radio map of the region to date, revealing 33 radio sources above a flux density of 2.4 mJy. Only one of these radio sources corresponded to an X-ray object: a quasar atz= 1.13. We also used the Parkes-Tidbinbilla Interferometer, at 2.29 GHz and 8.41 GHz, to observe some of the stronger radio sources.

From these multi-wavelength observations of the Pavo field it is apparent that, to the sensitivity of the surveys involved, (i) there is little correlation between X-ray and radio detections, and (ii) most of the X-ray sources have optical counterparts while few of the radio ones do, and (iii) there is some confirmation that X-ray emission is higher for objects with flat radio spectra (i.e., a dominant core) than for steep spectrum sources.
Non-constant Superluminal Velocities in AGN
Authors: Coleman Colin S.
Published: July 2016

Large apparent superluminal velocities are observed in nuclear jets in Active Galaxies, indicating the presence of relativistic velocities almost along the line of sight. If the flow is well collimated, as suggested by the large scale radio structure, the inferred alignment leads to difficulties with source statistics. Here a modification of the usual relativistic beam model is proposed, in which the jet is assumed to contain azimuthal (swirling) flow. Perturbation analysis is used to show that the jet is unstable to a Kelvin-Helmholtz helical standing wave, the wavelength of which increases without bound in the limit of vanishing swirl. This instability may cause a cylindrical jet to follow a helical path in space, thereby reducing the implied alignment of a superluminal source, and providing a natural interpretation of non-constant superluminal velocities.
The Fortieth Anniversary of Extragalactic Radio Astronomy: Radiophysics in Exile
Authors: Bolton J. G.
Published: July 2016

In 1931 Karl Jansky established that radio noise was associated with our own galaxy–the Milky Way. For a decade and a half there was little follow-up; those of us who were associated with low frequency radar during the war regarded it as a nuisance which could limit the detection range of enemy aircraft. Grote Reber was the first to make a detailed but fairly low resolution map of the radiation from the galaxy showing, for the first time, some detailed structure. The event which we celebrate today occurred when Gordon Stanley, Bruce Slee and I showed that three of the discrete sources that we had discovered could be identified with visual objects. One was with the Crab Nebula, a supernova remnant within our own galaxy and the other two with galaxies, far beyond our own system, in the constellations of Virgo and Centaurus. Thus began extragalactic radio astronomy. In 1982 at the Noosa meeting of the ASA, I gave an account of those early years, later to be published in the ASA Proceedings. As I don’t wish to repeat myself, I propose to speak on my involvement in a later development which was to extend the observable scale of the universe to look-back times as great as the age of the oldest stars in our own system. The first important step was Graham Smith’s identification of Cygnus A with a galaxy that was much fainter than our two. The spectrum by Minkowski revealed an instrinsically highly-luminous galaxy with strong emission lines and opened up the possibility of discovering similar objects at significantly greater distance. This was achieved nine years later with the building of the Owens Valley Observatory and my title of ‘Radiophysics in Exile’ comes from the fact the observatory owed its existence and early successes very largely to past and future staff members of Radiophysics. They were, in order of appearance, J. G. Bolton, G. J. Stanley, K. C. Westfold, J. A. Roberts, V. Radhakrishnan, D. Morris and K. I. Kellermann. Some still bear . the scars–Westfold left the tip of one index finger in the Owens Valley!
The ISO Instrumentation and Expected Performances
Authors: de Graauw T.
Published: July 2016

In this paper the author describes the instrumentation for the Infrared Space Observatory to be launched in 1993.
The Megamaser Galaxy III Zw 35
Authors: Chapman Jessica M. , Staveley-Smith L. , Axon D. J. , Unger S. W. , Cohen R. J. , Pedlar A. , Davies R. D.
Published: July 2016

III Zw 35 is a pair of galaxies characterised by intense OH maser emission, and powerful far-infrared and radio continuum. We have made a detailed study of the galaxy pair based on optical, infrared and radio observations. The brighter northern component is identified as a LINER or Seyfert galaxy and contains an active nuclear region from which radio continuum, OH maser and thermal dust emission are detected. We propose that the northern component has a compact active nucleus deeply embedded in an obscured region of diameter ~ 210 pc within which enhanced star-formation occurs. The lower luminosity, southern component is of low mass and is undergoing starburst activity over an extended region of diameter ~ 5.5 kpc. The origin of the starburst and non-thermal activity appears to be an interaction between the two components.
Starbursts in Ring and Irregular Galaxies
Authors: McIntyre V. J. , Zealey W. J.
Published: July 2016

This paper presents the current status of a Ph.D. project undertaken to search for extended-scale bursts of star formation (> 1 kpc) in irregular and collisionally produced ring galaxies, principally in the southern half of the sky. Results of recent 8.4 GHz radio continuum observations and UBVRI CCD imaging of some of the program galaxies are presented.
Radio Emission and Star Formation in Dwarf Galaxies
Authors: Klein U.
Published: July 2016

This paper discusses several aspects of radio emission and star formation in dwarf galaxies.
Do Elliptical Galaxies show Warp?
Authors: Gamaleldin A. I.
Published: July 2016

Surface photometry of the elliptical galaxy NGC 1700 is presented and discussed in terms of providing evidence for warping of the outer isophotes in elliptical galaxies.
Search for Southern Open Cluster Flare Stars: M7, IC 2602, IC 2391 and NGC 2516
Authors: Jones K. L. , Page A. A.
Published: July 2016

We summarise the results, to date, of a long-term program of searching for flare stars in the region of open clusters selected on the basis of distance and age.
Winds in Central Stars of Planetary Nebulae
Authors: Patriarchi P. , Perinotto M.
Published: July 2016

We present the results of an examination of low-resolution IUE spectra of Galactic planetary nebulae in an effort to determine the occurence of stellar winds in their central stars. Our analysis confirms the results obtained in previous studies.
Radar and Spacecraft Ranging to Mercury between 1966 and 1988
Authors: Anderson John D. , Slade Martin A. , Jurgens Raymond F. , Lau Eunice L. , Newhall X. X. , Standish E. Myles
Published: July 2016

Improved solutions have been obtained for the orbit and equatorial cross-section of Mercury using radar ranging data spanning 22 years. These data have yielded new results on the precession of Mercury’s perihelion and better limits on a possible time variation in the gravitational constant G.
Unneutralised Currents in Solar Flares
Authors: Melrose D. B.
Published: July 2016

Observations of the vector magnetic field imply that there is a net current flowing through the corona, and there is also evidence that this current is directly related to flares. It is argued that if the currents are unneutralised, then this requires a radical rethinking of several widely accepted ideas on solar magnetic fields and their role in solar flares.
The Downturn in Solar Activity during Solar Cycles 5 and 6
Authors: Murphy J. O.
Published: July 2016

The atmospheric 14C record, the corresponding WM values derived from a carbon reservoir model, auroral numbers and the Zurich relative annual sunspot numbers all demonstrate a substantial downturn in solar activity for the duration of solar cycles 5 and 6. This reduction is also imbedded in some dendrochronological proxy data sets, which describe an annual index radial growth rate for trees at high-altitude sites. A significant lagged correlation can exist between tree-ring indices and the 11–year solar cycle during periods of high solar activity, a feature which is not evident during quiescent periods.
Non-Thermal Emission Mechanisms in Astronomy
Authors: Westfold K. C.
Published: July 2016

Whether a mechanism for the emission of radiation can properly be regarded as thermal or non-thermal depends on the nature and extent of the interactions that take place between the radiation resulting from such a process and the surrounding medium. Thus, no matter what the emission mechanism there can be a balance between emission and absorption processes such as to produce a state of local thermodynamic equilibrium (LTE), so that the net radiation available for transport through the source region is thermal.
Recent work with the UK Schmidt Telescope
Authors: Tritton S. B.
Published: July 2016

The UK 1.2 metre Schmidt Telescope came into operation in 1973 with the primary purpose of extending to southern declinations the Sky Survey carried out with the Palomar 1.2 metre (48 inch) Schmidt Telescope. This telescope is, in most respects, an exact copy of the Palomar telescope, but several recent developments result in a much fainter limiting magnitude (by about 2 magnitudes) for the Southern Survey. The UK Schmidt Telescope has an aperture of 1.2m, and the spherical primary has a diameter of 1.83m and focal length 3.07m. The plates have the dimensions 356 x 356mm, giving a field of view of 61/2°; the plate scale is 67″ 1/mm.
Boundary Effects and the Circular Polarization of Synchrotron Sources
Authors: Melrose D. B.
Published: July 2016

Some self-absorbed synchrotron sources have, a small but observable degree of circular polarization rc near the absorption turnover (Roberts et al. 1975). The simplest interpretation of the circular component is in terms of the intrinsic degree of circular polarization of synchrotron radiation (Legg and Westfold 1968); this provides a relation (Roberts et al. 1975)
Solar Flare Increase of Cosmic Ray Intensity on November 22, 1977
Authors: Fenton A. G. , Fenton K. B. , Humble J. E.
Published: July 2016

Solar flares for which protons of relativistic energies reach Earth are rare events compared with the number in which non-relativistic protons are produced. For instance, Shea and Smart (1978) have listed 139 proton events for the interval 1955-69 of which 17 were GLE’s (i.e. “ground level events” detected by the world network of cosmic ray neutron monitors). We have tentatively identified a further 11 GLE’s in the interval 1970-1977, of which 3 were in 1977 in the sunspot cycle which commenced about mid-1976 (cycle 21). Thus the average rate over the past two solar cycles has been a little over one per year.
Optical and Near-infrared Observations of Supernova 1987A
Authors: Spyromilio Jason
Published: July 2016

We present observational results obtained during the first three years following the explosion of Supernova 1987 A. We discuss aspects of the optical and near infrared spectra as well as results from spectropolarimetric observations. The observations of the circumstellar and interstellar medium are also briefly discussed.
Stellar Convection
Authors: Xiong Da Run
Published: July 2016

Time-dependent convection theory and non-local convection theory are described. The difference between the convection theories results from the different treatment of the non-linear terms of the hydrodynamic equations. We have obtained a better understanding of the thermodynamic coupling between convection and oscillations in comparison to the dynamic coupling.
The Japanese National Large Telescope
Authors: Kogure Tomakazu , Kodaira Keiichi
Published: July 2016

The Japanese National Large Telescope is an 8-metre class optical-infrared reflector with a monolithic thin meniscus mirror, to be constructed at the Mauna Kea summit, Hawaii. The JNLT will be characterised by high quality performance in the optical and infrared regions, achieved by adopting new technologies such as active mirror support, fast optics and a thermally controlled dome. In particular, high infrared qualities are regarded as the most important characteristics among various design goals.

The JNLT project is now close to the final study phase before construction. This paper reviews the scientific motivations and the special technical features of the JNLT. Finally, the promotion of international collaboration around the JNLT is emphasised.
Asian-Pacific Co-operation in Optical Astronomy
Authors: Cannon Russell
Published: July 2016

This paper discusses opportunities for collaboration in astronomy among the countries of the Asian–Pacific region.
Science Education in a Planetarium
Authors: Othman Mazlan
Published: July 2016

This paper discusses the role of the planetarium as an indispensable means of teaching astronomy and as an increasingly popular way of teaching science.
Proposed Structure of Education in Astronomy
Authors: Isobe Syuzo
Published: July 2016

This paper discusses the importance of having a structured approach to educating the general public in astronomy. It outlines the role schools, planetaria and national observatories must play in this process. It also addresses the question of how astronomical events are best exploited to activate the public’s interest in astronomy.
Science in the Public Eye
Authors: Pockley Peter
Published: July 2016

A few days ago a prominent physicist, Professor Frank Stacey of the University of Queensland, made a public statement on his retirement that he was burying a theory. He had believed he had measured a new gravitational constant for close objects. Over 12 years he and colleagues in Australia and overseas had tried to confirm a theory of a fifth fundamental force of nature to explain the observations. His claim had gained a great deal of publicity as, if true, it would have extended Newton’s law of gravity and Einstein’s theory of general relativity.
The Geometry of the SMC
Authors: Gardiner L. T. , Hatzidimitriou D. , Hawkins M. R. S.
Published: July 2016

We have undertaken a study of the 3-D spatial distribution of the older (τ ≥ 1–2 Gyr) stellar population lying beyond ~ 2 kpc in projected radial distance from the centre of the SMC. The study will eventually cover 120 square degrees including six overlapping Schmidt fields. Here we present the results from an area of 80 square degrees including the western, northern and north-eastern outer parts of the SMC.
Global Magnetic Structure In Spiral Galaxies
Authors: Spencer S. J.
Published: July 2016

Global magnetic structure has been inferred in spiral galaxies from radio and optical observations. The author has developed a three dimensional, quasi-global kinematic dynamo model which demonstrates the possibility of maintaining large-scale magnetic fields by the αω mechanism. Analytical expressions for large-scale galactic magnetic fields near temporal steady states have been derived. Illustrations of the spatial distribution of vector and absolute large-scale magnetic field strength are presented. When coupled with observations this model may help in understanding the maintenance and morphologies inferred for disk and halo global magnetic fields in spiral galaxies.
Photometric and Spectroscopic Analyses of Cool HdC Stars
Authors: Cottrell P. L. , Lawson W. A.
Published: July 2016

A photometric and spectroscopic survey of many of the cool H-deficient Carbon (HdC) stars, including the R Coronae Borealis (RCB) stars, has been undertaken. For the RCB stars we have data on both the low amplitude photometric variations at maximum light and the major declines, the latter being the most distinguishing feature between the RCB and HdC stars.

The photometric data at maximum light have been analysed using the Lomb-Scargle Fourier method, which has revealed many significant periodicities. From estimates of the temperature of these stars, an observational period-temperature diagram can be compared with theoretical models. These models have also enabled us to determine the evolutionary lifetime of these stars for comparison with observational parameters, e.g., period changes.

Over the last several years we have photoelectrically covered the declines (and the recovery from some of these declines) of a number of RCB stars, from which we have been able to characterise two extreme types of decline behaviour. In addition, we have for the very first time spectroscopically recorded the initial decline phase of one (the prototype, R CrB) of these stars.
Automated Computation of General Perturbations for the Flora Asteroidal Group
Authors: He M. F. , Zhangjie
Published: July 2016

The general perturbations of the asteroids of the Flora group (975″ < n < 1150″, n - the mean daily motion) due to Jupiter have been automatically computed on an IBM 4341 computer with the Hansen method by manipulating Broucke’s Symbolic Poisson Series Processor, and the results have been compared with that computed previously with the Bohlin group method.
A Coudé Auxiliary Feed for the AAT: a Focus for International Co-operation in Optical Astronomy
Authors: Gillingham P. , Pettini M. , Bessell M. , Cram L. , Ogura K.
Published: July 2016

In 1988, a very powerful and versatile coudé echelle spectrograph was installed at the Anglo-Australian Telescope. Since then it has been winning about 30% of AAT time and has been highly productive scientifically. Therefore, using a coudé auxiliary telescope (CAT) to give the spectrograph more use and to free the AAT for other work is a very attractive possibility, particularly if the CAT can give a sensitivity similar to that obtained with the 3.9-metre telescope. While a conventional CAT with such performance would be very expensive, a much cheaper instrument should approach this goal, at least for high resolution spectroscopy. Even so, the cost could not be met in a reasonable time within the AAO’s budget; hence, additional international collaboration is being sought.
The Mt John CCD System: Status and First Scientific Results
Authors: Tobin William
Published: July 2016

A Photometrics CCD system containing a TH7882 chip has been in use at Mt John since 1989 October for imaging photometry. Extra control software has increased observing ease and image-header information. Photometrically the system appears to be performing satisfactorily. The blue helium star LSS 99 showed no variation exceeding ~ 1% over 40 min of observation. The blue eclipsing binary HV 1761 in the Small Magellanic Cloud is found to have approximately equal components.
Sapphire Clocks in VLBI Radioastronomy
Authors: Luiten A. N. , Blair D. G.
Published: July 2016

This paper describes a system utilising a sapphire-loaded superconductor cavity to provide a high-stability oscillator signal for use in VLBI observations.
Communicating Space Science to the Public
Authors: Dougherty Kerrie A. , James Matthew L.
Published: July 2016

A version of this paper was originally presented at the Fifth National Space Engineering Symposium at Canberra in November 1989. A copy of the full paper will be found in the text of the Proceedings. It is presented here because the authors believe that the issues raised and strategies suggested are as relevant to the astronomical community as they are to other areas of space science and technology.
Amateur-professional Co-operation in Astronomy Education: a Nineteenth Century Australian Model
Authors: Orchiston Wayne
Published: July 2016

During the second half of the nineteenth century Australian amateur and professional astronomers worked together in actively promoting astronomy among the general public. This collaboration was a product of the cordial amateur-professional relations that permeated pre-astrophysics Australian astronomy.
Astronomy Education in a Multi-lingual Rural Society
Authors: Ramadurai S.
Published: July 2016

This paper examines the importance of astronomy education for a rural society in a third world country. Some conclusions are drawn about methods of introducing astronomy to school students and, through them, the entire village. The conclusions are based on the author’s direct experience in addressing high school students in several rural towns in India.
The Origin and Composition of Pluto and Charon: Chemically Uniform Models
Authors: Prentice A.J.R.
Published: July 2016

Observations of the Pluto-Charon system using the Hubble Space Telescope are soon to provide another test of the modern Laplacian theory of solar system origin. According to this theory, Pluto, Charon and Neptune’s moon Triton are condensed remnants of the gas ring which was shed by the proto-solar cloud at Neptune’s orbit, and from which Neptune formed. Each body should have the same bulk chemical composition provided that the influence of secondary events such as physical collision can be neglected. Here we report a model for the time-dependent, surface-catalysed production of CH4, solid carbon C(s) and CO2 within the outer layers of the proto-solar cloud. This model is used to determine the condensate mix which best fits the Voyager 2 spacecraft measurements of Triton’s mean density. We suggest that Triton is a chemically homogeneous structure consisting, by mass, of 44.2% anhydrous rock, 2.1% graphite, 33.0% water ice and 20.7% dry ice (i.e., solid CO2 ice, of which a fraction nearly 2/3 is present as the clathrate hydrate CO2·5.75 H2O). On the basis of this composition, the individual mean densities of Pluto and Charon are predicted to be 2.02 ± 0.02 g/cm3 and 1.94 ± 0.02 g/cm3, respectively, assuming a mean surface temperature of 35 K. The mean density of the combined system is predicted to be 2.01 ± 0.02 g/cm3.
Identifications from the Parkes-MIT-NRAO Surveys
Authors: Tasker Niven J. , Wright Alan E. , McConnell David , Savage Ann , Kesteven Michael J. , Troup Euan , Griffith Mark
Published: July 2016

The Parkes-MIT-NRAO (PMN) 4.85 GHz continuum radio survey of the southern sky was undertaken in 1990 June and November. This survey was performed on the Parkes 64 m telescope using the NRAO seven-beam receiver. A point-source catalogue of 36,640 radio sources has been produced for the Southern Survey zone −87.5° ≤δ ≤ −37° and for the Tropical Survey zone −29° ≤δ ≤ −9.5°. The flux limit of this survey varies with declination and is typically about 30 mJy.

We have begun to cross-correlate the PMN data with sources contained in catalogues compiled at radio, and other, wavelengths. We have found associations for 96% of the PKSCAT90 2700 MHz database sources, and 95% of the Molonglo 408 MHz Catalogue sources within in the PMN Southern and Tropical Survey zones.

A program to identify the optical counterparts of PMN Southern Survey point sources, S4.85 GHz ≥ 70 mJy, using the COSMOS database, is under way. To facilitate this programme we are improving the positional accuracy of PMN sources with observations made at the Australia Telescope National Facility compact array. We have developed a new “snapshot” mode of observing to process the large number of sources (~ 8000) in our sample. It is possible to obtain accurate positions from three snapshots efficiently with a total integration of < 3 minutes.
Charles Todd and the Adelaide Observatory
Authors: Edwards P.G.
Published: July 2016

Charles Todd was the first Government Astronomer and Superintendent of Telegraphs in South Australia. Most widely known for his instrumental role in the construction of the Overland Telegraph, linking Australia and England, Todd also established the Adelaide Observatory and made valuable contributions to both astronomy and meteorology.
An Observed Correlation between the Flux Densities of Extended Hard X-ray and Microwave Solar Bursts
Authors: Stewart R. T. , Nelson G. J.
Published: July 2016

Crannell et al. (1978) have reported an observed correlation between the time profiles and flux densities of impulsive hard X-ray and microwave solar bursts. We report here on a significant correlation between the flux density of extended bursts of hard X-rays and micowaves. These extended events follow after impulsive bursts and last much longer (see e.g. Fig. 1, Frost and Dennis 1971). However, as extended bursts only occur during very large flares the number of cases available for study is small. The significance of our observations follows from the suggestion of Wild et al. (1963) that the extended bursts are evidence for a second-phase acceleration process in the corona. We show that the observed characteristics of these extended microwave bursts (viz. a rather flat spectrum below a turnover frequency which is independent of intensity) can be explained by gyro-synchrotron radiation from the same population of energetic (E ≈ 100 keV) electrons as those emitting (thin-target) X-ray bremsstrahlung. A detailed source model is discussed in a companion paper (Nelson and Stewart 1979 — Paper B).
Does the Radio Spectrum have Room for Radio Astronomy?
Authors: Robinson B. J. , Whiteoak J. B.
Published: July 2016

In a technical sense radio astronomers do not use the radio spectrum; they are listeners only, and when the science began they had to listen in the quiet spaces between transmitting services. Radio astronomy was first recognized as a service by the International Telecommunications Union (ITU) in 1959, and the first frequency allocations were then made for it as a ‘passive’ service. In 1963 and 1971 further allocations and frequency protection were obtained at specialized World Administrative Radio Conferences (WARC). The allocations were required for two purposes: (i) to protect the frequencies of the most important spectral lines of atoms and molecules, and (ii) to provide a series of bands for continuum observations. The general protection so far provided has been vital to the growth of the science, and its continuation is of the highest priority to the future life and development of radio astronomy.
Molecular Line Observations at Parkes with a 3 GHz Maser
Authors: Höglund B. , Whiteoak J. B. , Gardner F. F.
Published: July 2016

A 3 GHz maser from the Onsala Space Observatory, Sweden, is currently at Parkes on a long-term loan basis. So far, it has been used on the 64-m radio telescope for a two-week period of spectral-line observations in February 1979, providing a system sensitivity far superior to that previously available at the same frequency. The observed lines were the ground-state transitions of CH at 3264, 3335 and 3349 MHz, the 211 – 212 transition of H2CS at 3139 MHz, and the 211-212 transition of CH3CHO at 3195 MHz.
On the Measurement of Atmospheric Extinction by Rufener’s Method
Authors: KviZ Z.
Published: July 2016

The coefficient of atmospheric extinction may change during the night and in fact it often does. This has an adverse effect on the determination of atmospheric extinction by simple Bouguer plot of magnitude against air mass. This effect was studied by Rufener (1964), who introduced for the purpose of accurate photoelectric photometry in the Geneva photometric system the method of two ‘extinction stars’. His method consists of the measurement of two stars of the same colour — one starting at high air mass 2 - 3, the M-star (for French montante = rising) and the second starting simultaneously in the meridian at low air mass, the D—star (for descending).
Fleurs Synthesis Telescope Observations of Galactic SNRs
Authors: Milne D. K.
Published: July 2016

It is now generally accepted that the remnants of supernovae (SNRs) are of two types, recognizable by their radio structure and spectral index. To date most of the radio sources identified as SNRs are of the easily identified shell type. These have spectral indices a of -0.5 ±0.2 and exhibit some degree of annular brightness distribution — the projection of the radio shell. The second type, e.g. the Crab Nebula, have filled structures and relatively flat (a = -0.1 ±0.1) spectral indices. The relatively strong radio polarization exhibited by some members of this class has led to their identification but generally they tend to be hidden amongst the HII regions in our galaxy.
Preliminary Results from a New Survey of Ringed Galaxies
Authors: Buta R.
Published: July 2016

The SRC-J and ESO-B Sky Survey copy films are being used to compile a major new catalogue of apparent diameters, axis ratios, and relative bar/ring position angles of inner and outer rings in more than one thousand southern galaxies. This paper presents a preliminary analysis of the data for about two hundred SB rings of both types. It is concluded that the rings have a wide range of intrinsic eccentricities, and more importantly that they have preferred alignments, one mode for inner rings and two for outer rings, with respect to bars.
Upper Mass Limits for Hydrogen-Rich Planetary Nebula Nuclei
Authors: Faulkner D. J . , Wood P. R.
Published: July 2016

We have discovered a radiation levitation mechanism which, under certain circumstances, can remove the last vestiges of hydrogen-rich material from an incipient planetary nebula nucleus if its mass exceeds a critical value of about 0.85M⊙. This process may be responsible for the production of helium-rich planetary nuclei, and their progeny the DB white dwarfs.
Pulsar Astronomy at Molonglo
Authors: Manchester R. N.
Published: July 2016

Molonglo Observatory has played an important role in pulsar astronomy from shortly after the initial discovery announcement in 1968 to the present. Its major contribution has been in the area of searches for new pulsars – for most of the 17-year period more than half of the known pulsars were Molonglo discoveries. The history of pulsar astronomy at Molonglo is reviewed and a brief account of current observation programs is given.