bluuebunny/crossref_metadata_2025 huggingface dataset:
2.3 metre multi-colour photometry of a new AM Herculis variable
Authors: Tuohy I. R. , Ferrario L. , Wickramasinghe D. T. , Hawkins M. R. S.
Published: July 2016

We present UBVRI photometry of the faint and highly erratic cataclysmic variable discovered by Hawkins (1983) from a sequence of U.K. Schmidt plates. Observations using the ANU 2.3 m telescope over two nights in September 1986 show pronounced and repeatable modulation at a binary period of 108.6 min. Dramatic colour differences are evident in the folded UBVRI light curves: in the U band, a single sinusoidal peak is present, while at longer wavelengths, a second red peak dominates at a phase separation of Δϕ = 0.5. This behaviour is strongly suggestive of cyclotron emission from two magnetic accretion funnels in an AM Herculis binary system. Furthermore, the binary period lies in the narrow range of 100-115 minutes that characterizes most of the AM Herculis variables lying on the short side of the 2-3 hour period gap. We conclude therefore that the object is almost certainly a new AM Herculis system, and develop a model in which the blue and red components originate from two non-diametrically opposed cyclotron regions that are characterized by differing electron temperatures and opacities. Predictions are made regarding the linear and circular polarization properties of this important new magnetic variable.
Modelling Large Body Impacts
Authors: Pongracic Helen
Published: July 2016

Hypervelocity impacts are considered to be the main mechanism for the production of craters on the surfaces of planets and moons. Two- and three-dimensional numerical simulations for the first few seconds of large-body impacts will be discussed. Both normal and oblique impacts will be considered, with particular emphasis being placed on the distribution of impact products.
The Lyman Far Ultraviolet Spectroscopic Mission (Invited Paper)
Authors: Tuohy Ian R. , Dopita Michael A.
Published: July 2016

The Lyman mission will undertake the first sensitive high resolution spectroscopic observations in the largely unexplored 912-1216Å region. This astrophysically critical wavelength interval is exceedingly rich in diagnostic spectral lines such as the Lyman series of atomic hydrogen and deuterium, the Lyman and Werner bands of molecular hydrogen and deuterium, and the resonance lines of numerous important species including CIII, NI-III and OVI. Lyman will have a major impact in all areas of modern astrophysics, with the most fundamental contribution being the determination of light element abundances in the local interstellar medium and in the intergalactic medium at low redshift. The mapping of hot gas (T ∼ 3 × 105K) and molecular hydrogen and HD in the disk and halo of our galaxy represent additional major objectives for which Lyman is uniquely qualified.

The Lyman payload will comprise a grazing incidence telescope and three spectroscopic instruments: the prime spectrograph operating between 912-1250Å with a resolution of λ/ Δλ ∼ 30,000, a far ultraviolet spectrograph (1200-2000Å;λ/ Δλ ∼ 10,000), and an extreme ultraviolet spectrograph (100-900Å; λ /Δλ ∼ 300). Observations will be conducted from a highly efficient 48 hour elliptical orbit which will allow long un-interrupted exposures and real time operations. It is anticipated that Lyman will be launched by Ariane in 1996, and will have an operational lifetime of at least 5 years. Data reception and spacecraft control will be undertaken from ground stations in Spain and in Australia.

Lyman is currently being studied at Phase-A level by Australia in close coordination with the European Space Agency. The scientific involvement is the responsibility of the Lyman Science Working Group, composed of members representing the various astronomical institutions in Australia. Funding to support the technical and scientific aspects of the mission is provided via the Australian Space Board and the Department of Industry, Technology and Commerce in recognition of the major opportunity that Lyman presents to the Australian aerospace industry.
The Progenitor Star and its Evolution
Authors: Wood P.R.
Published: July 2016

Observational and theoretical constraints which apply to models of the precursor star before and at the time of explosion are presented. Stellar evolution sequences for the precursor star produced by various authors are described, and an attempt is made to define what these sequences tell us about the evolution of star of mass ∼ 20 M⊙.
Ultraviolet Observations of SN 1987A
Authors: Panagia N.
Published: July 2016

The IUE observations of SN 1987A are presented and the most important results are briefly summarised. The photometric observations of SN 1987A are discussed in some detail in the context of the supernova energetics. Adding the information from spectroscopy and neutrino observations, it is concluded that SN 1987A is a ‘normal’ Type II explosion (i.e. core collapse of a massive star) with an unusually compact initial configuration, just as expected for the progenitor Sk −69°202.
SN 1987A in the UV: the Progenitor Star, the Reddening and the Possible Detection of a UV Light Echo
Authors: Gilmozzi Roberto
Published: July 2016

Some special issues to which IUE observations have provided crucial insight are presented. The arguments leading to the definitive identification of Sk−69°202 as the progenitor of the LMC supernova are reviewed, and a preliminary determination of the reddening toward SN 1987A, based on the IUE spectra of stars 2 and 3, is discussed. Recent observations at the predicted position of the SN ultraviolet light echo are reported, and evidence, albeit circumstantial, is provided that a UV echo has been detected. Some consequences of this result are explored. The relevance of this observation lies in the fact that a UV echo, if really detected, would give direct information of the spectrum of the SN at the time of the shock breakout.
Absolute Spectrophotometry of SN 1987A and the Hα Bochum Event
Authors: Hanuschik Reinhard W.
Published: July 2016

Spectrophotometric optical fluxes of SN 1987A have been measured at high accuracy with the 61cm telescope equipped with a rapid spectrum scanner. This highly homogeneous data set covers the wavelength range 3200-8700Å at 10Å resolution. Selected wavelength regions, e.g. around Hα, have also been measured at 3Å resolution. The Hα line shows an undisturbed P Cygni-type profile until March 15, superimposed by variable fine-structure thereafter, developing within a few days into a blue-shifted, peak-like flux excess and a red-shifted flux deficiency. This fine-structure is intrinsic to Hα. Similar fine-structure is also observed in Na I-D, in Paschen-α and possibly in Hβ. We discuss our observations in terms of the ‘mystery spot’, and of models involving a jet and interactions with surrounding pre-existing material, and we propose density inhomogeneities, or occupation number deficits due to NLTE effects, within the inner regions of the envelope as origin.
Review of Speckle Observations of Supernova 1987A
Authors: Meikle W.P.S.
Published: July 2016

SN 1987A is sufficiently close to allow a unique examination of the morphology of a supernova, using speckle interferometry. Several groups [Center for Astrophysics (CfA); Imperial College (IC); Mount Stromlo and Siding Spring Observatories/Anglo-Australian Observatory (M/A)] have reported optical speckle observations. At Hα, both CfA and M/A have determined the angular extent of the emission, and reasonable agreement is obtained. The speckle-derived values are consistent with those obtained from line profiles. IC has also succeeded in resolving the supernova at Hα. At wavelengths other than Hα, at early epochs, angular diameters obtained by CfA are larger than those derived from photometric and spectroscopic measurements, possibly due to scattering effects. At later epochs, the diameters exhibit little variation between the wavelengths examined. CfA reports significant asymmetry in the late epoch data.

Several attempts have been made to re-observe (at optical wavelengths) the companion object, but none have succeeded. The nature of this phenomenon is still controversial, but the evidence indicates that the companion was real, with emission from dust apparently being the least problematic explanation. Support for this may lie in IR speckle observations (Haute Provence/Lyon) which, on about day 115, indicated the presence of one or more resolved components at an angular displacement comparable to that of the optical companion.
High Energy γ-ray Observations of SN 1987A
Authors: Sood R.K. , Thomas J.A. , Waldron L. , Manchanda R.K. , Rochester G.K. , Sumner T.J. , Frye G. , Jenkins T. , Koga R. , Ubertini P. , Bazzano A. , La Padula C. , Staubert R. , Kendziorra E.
Published: July 2016

SN 1987A has been observed with a combined high energy γ-ray (50-500 MeV) and hard X-ray (15-150 keV) payload during a balloon flight on 5 April 1988 from Alice Springs, Australia. The γ-ray observations, along with our earlier ones on 19 April 1987 are the only such observations of the supernova to date. The γ-ray detector characteristics are described. The preliminary results of the recent flight and their implications in terms of the known supernova parameters are discussed.
Simple Perspectives on SN 1987A
Authors: Fu Albert
Published: July 2016

This conference has shown that the accumulated wealth of data on SN 1987A has enabled us to learn an unprecedented amount of physical information about a single supernova event and supernovae in general, as well as to confirm much of the heretofore established theory. While some difficult problems remain, I discuss some particularly simple and useful theoretical notions concerning the bolometric and γ-ray light curves which can be gleaned from our current body of knowledge, drawing primarily upon results of analytic work performed by W.D. Arnett and myself. Also, the work of Lamb, Melia and Loredo (1987) on neutrinos from the supernova is discussed briefly.
On the Measurement of Slightly Extended Sources
Authors: Crawford David F.
Published: July 2016

A general method is described for estimating the position, integrated flux density and the second moments of the flux density distribution for sources in a two dimensional map. The method requires accurate knowledge of the beam shape of the telescope. Uncertainty estimates and significance levels of the source parameters are easily obtained.
Chromospheres of M Dwarf Stars with Incipient Hα Emission
Authors: Robinson R. D. , Cram L. E.
Published: July 2016

We present observations of Hα and CaII resonance lines in 4 stars having Hα features which place them intermediately between the non-(e) and (e) classifications of dK/dM stars. There is considerable variety in the shape of the Hα line, presumably due in part to differences in rotation rates. As expected, the energy fluxes in the CaII emission lines lie between those typical of non-(e) and (e) stars. There is some evidence (especially from the binary Gl 876A) that the energy fluxes in the CaII and Hα emission lines do not vary from star to star according to a simple proportionality. An intriguing result is the apparent detection of spatially displaced chromospheric emission in Gl 907.1 and Gl 890.
A Search for Non-Radial Oscillations on Late-Type Stars
Authors: Edmonds P. D. , Cram L. E.
Published: July 2016

The detection of non-radial oscillations on late-type dwarf stars may require the measurement of Doppler shifts of order 10 cm s−1. We report observations using the coudé echelle spectrograph of the 3.9 m Anglo-Australian Telescope which reveal a noise level in a 1 minute integration about a factor of one hundred greater than this. We then discuss a method of imposing a set of stable reference features on stellar spectra to permit Doppler measurements of the required accuracy. The method exploits a voltage-tuned solid Fabry-Perot interferometer whose passbands are fixed by a servo-control system to the light from a HeNe laser whose frequency is polarization-stablized. The desired wavelength stability demands careful control of the voltage, temperature and tilt of the etalon.
Activity in a Complete Sample of Red Giants
Authors: Slee O. B. , Stewart R. T. , Buntont John D. , Beasley A. J. , Carter B. D. , Nelson G. J.
Published: July 2016

The Parkes 64 m telescope has been used to survey a complete sample of nearby red giants (i.e. not members of close binaries or showing strong emission lines of CaII). The sample consisted of all 82 stars in the Bright Star Catalogue within 30 pc having spectral types G, K, M and luminosity classes I, II, III south of the celestial equator.
From the Sun to the Universe—The Woolley and Bok Directorships at Mount Stromlo
Authors: Hyland A. R. , Faulkner D. J.
Published: July 2016

The twenty years following the Second World War saw great changes in the research interests of the Observatory at Mount Stromlo, with the early emphasis on solar and geophysical phenomena giving way to stellar and galactic astrophysics. This paper traces the development of the astrophysical research work during the directorships of Woolley, who initiated the change of direction, and of Bok, who continued it. Apart from the shift in the Observatory’s research interests, these years were distinguished by (i) an outstanding period of telescope acquisition, which saw the commissioning of the 74 inch reflector, the 50 inch (formerly the Great Melbourne Telescope), the Yale/Columbia refractor (relocated from South Africa), and the Uppsala Schmidt; (ii) an Australia-wide site-testing programme and the consequent establishment of Siding Spring Observatory with the 40 inch, 24 inch and 16 inch reflectors (the site has subsequently, of course, also become the home of the Anglo-Australian Telescope, the U.K. Schmidt, and the ANU 2.3 m Advanced Technology Telescope); (iii) the incorporation of several major technological developments into the instrument complement of the Observatory, including photo-electric photometry, coudé spectroscopy, spectrum scanners, polarization instruments, and digital computers; (iv) the establishment of the link with the Australian National University and the consequent transformation of the Commonwealth Observatory into the Mount Stromlo Observatory; and (v) the setting up of a large and vigorous graduate school, comprising, at Bok’s departure, about fifteen PhD students on course.
Elliptical Galaxies—Getting to the Heart
Authors: Sadler Elaine M.
Published: July 2016

Elliptical galaxies are at first sight a remarkably homogenous class of objects, yet some of them produce large and enormously powerful radio sources while others remain more or less quiescent. Why should this be so? What prompts the nucleus of an elliptical galaxy to become ‘active’? What, if anything, do elliptical galaxies have in common with the bulges of spirals? Here, I review some of the radio and optical properties of nearby elliptical galaxies, with special emphasis on events which take place within the central kiloparsec.
VLBI in the 1990s
Authors: Kellermann K. I.
Published: July 2016

Radio telescopes in more than 20 different countries on five continents are being used for VLBI observations of galactic and extragalactic radio sources, as well for applications to geodesy and geophysics. New radio telescopes and networks of radio telescopes dedicated to VLBI which are being built in the United States, the U.S.S.R., Italy, China, Poland, the U.K. as well as in Australia will greatly improve the sensitivity, resolution, image quality, and frequency coverage of the existing networks. The Mk II VLBI recording system, which is based on consumer type Video Tape Recorders, is widely used but the sensitivity is limited. Broad band recording systems are expensive, but are becoming more popular due to their much greater sensitivity. They are expected to dominate VLBI systems in the 1990s.

The first tests of an earth-to-space VLBI system took place in 1986, and by the mid 1990s dedicated VLBI antennas will be launched into earth orbit by the U.S.S.R. and by Japan in collaboration with Australia and other countries throughout the world. Space VLBI missions will give an order of magnitude improvement in resolution over the ground based VLBI networks operating at the same wavelengths.
Universal Gravity: was Newton Right?
Authors: Wright Alan E. , Disney M. J. , Thomson R. C.
Published: July 2016

We question Newton’s inverse square law of universal gravitation in the light of recent, alternative formulations. In addition, we present numerical simulations of galaxy interactions which were used in an attempt to distinguish between an inverse square law and an inverse linear law. We conclude that an inverse linear relation is as compatible with the observational data on interacting galaxy systems as the inverse square law.
Investigating the Halo of the LMC
Authors: Hughes Shaun M. G. , Wood Peter R. , Reid Neill
Published: July 2016

Recent results have shown that Long-Period Variables (LPVs) with periods in the range 100 to 250 days have ages ~ 10 Gyr. We have studied the kinematics of a sample of such variables in the Large Magellanic Cloud (LMC). A comparison with the kinematics of other populations (H I gas, CO molecular clouds, planetary nebulae, CH stars and old clusters) indicates that all populations younger than the old LPVs are dominated by a single common rotating disk, with the kinematics of the old LPVs being the first to indicate the presence in the LMC of a spheroidal population, with little or no rotation and a velocity dispersion ~ 6 times larger than that of the H I gas.
The ATNF Logo Revisited
Authors: White Graeme L.
Published: July 2016

The Logo of the Australia Telescope National Facility (ATNF) depicts a linear array of six antennas in the Southern Hemisphere. Precision measurement of this image implies that the Compact Array is located at latitude 37° south and azimuth 176°; this corresponds (surprisingly) to an approximately north-south array. Furthermore, the ATNF Logo was apparently prepared at LST 04h 00m.
Temporal and Spatial Characteristics of Solar Flares from Observations
Authors: Wang Jia-Long
Published: July 2016

Temporal and spatial characteristics of solar flares are briefly reviewed in this paper. The global, temporal and spatial behaviours of flares are given first. Besides the 154-day periodicity, an 80-day periodicity of occurrence rate of large hard X-ray bursts for the period 1980 February – 1985 December, and the delay of the peak occurrence rate of large flares are pointed out, then the gregariousness of major flares is shown. In the third section, the time process and spatial structure of individual flares are shown and described according to space and ground-based observations. In the last section two problems on flare properties are discussed. (i) Previous classifications of solar flares are based generally on observations in a single spectral region. A new classification of flares based on observations in multi-spectral regions is given. (ii) Energy released in part of a loop seems to be not enough for a whole flare, and a qualitative model in which the energy is supplied by the untwisting of magnetic fields is proposed.
The Presence of the Wielen Dip in the Disk Stellar Luminosity Function
Authors: Lee Sang-Gak
Published: July 2016

The disk stellar luminosity function has been redetermined by the mean absolute magnitude method, utilising the proper motion data of the LHS Catalog. The derived luminosity function shows a slightly deeper dip than that found by Wielen (1983) in the same magnitude range.
Sources of Enrichment
Authors: Dopita M. A.
Published: July 2016

The relative importance of the stellar sources contributing to the production matrix of the heavy elements up to iron is reviewed. Three main element groups may be distinguished: (a) oxygen and the alpha-process elements; (b) the iron-peak group; (c) helium, carbon and nitrogen. Each of these is produced in stars of a different mass range and in different ways, and it is shown that an examination of metallicity-metallicity relationships can be used to constrain models of the history of star formation, stellar evolution, and the initial mass function in galaxies.

We can conclude that in the case of our local solar neighbourhood the initial Fe/O ratio was set by Type II supernovae, but that Type I½ supernovae were never important. Iron is produced by the Type I deflagration supernovae on a time-scale comparable to the infall time-scale of the gas. Carbon is produced by dredge-up in low-mass stars, but nitrogen is shown to be produced both in the stellar winds of massive stars, and in higher mass stars which give rise to the Type I planetary nebulae.
Speckle Observations of Spectroscopic Binaries
Authors: Isobe Syuzo
Published: July 2016

This paper presents results from speckle observations of binary stars carried out between 1987 and 1990 using a 212-cm telescope at the San Pedro Martir Observatory, Mexico.
Period Changes of Ten Eclipsing Variable Stars
Authors: Oh Kyu-Dong
Published: July 2016

We examine the period variations of ten eclipsing binary stars and from the combined result, attempt to construct a physical explanation for their behaviour.
G54.4–0.3: Interaction of a Supernova Remnant with the Interstellar Medium
Authors: Junkes Norbert
Published: July 2016

In our study of the extended supernova remnant G54.4–0.3, we find a CO emission shell at about 40km s−1 radial velocity, in striking alignment with the radio continuum shell. The correspondence in position and size argues strongly for a physical connection, and allows derivation of the kinematic distance as well as the mass and density of the CO shell. The correlation with an OB association supports the value derived for the kinematic distance. Model calculations suggest that the formation of the CO shell results from a stellar wind and that the supernova remnant has expanded into the wind bubble located inside the shell.
An Explanation for the Solar Neutrino Problem—a New Mechanism of Thermonuclear Reaction
Authors: Wang Hongzhang
Published: July 2016

A new mechanism of thermonuclear reaction is briefly introduced. It shows that a certain amount of thermonuclear reaction can take place in dense, low temperature (T < 1 × 105 K) plasmas. As most regions in the Sun are at moderate and low temperature, a sufficient amount of fusion energy is generated there. Therefore, the current standard solar models, in which the solar central temperature must be slightly lower than 15 × 106 K, must be modified, and this would make the flux of high-energy neutrinos conform with the observational results.
Japanese Lunar Mission in the mid-1990s
Authors: Mizutani Hitoshi
Published: July 2016

This paper outlines the plans for a Japanese lunar exploration mission in the mid-1990s.
The Magnetic Pole Model for Pulsar Emission
Authors: Manchester R. N.
Published: July 2016

Pulsars are unique astronomical objects in that their emission is in the form of a periodic pulse train. For most pulsars the pulse duty cycle is small, only a few per cent of the period. The shapes and intensities of individual pulses are in general quite variable. This is illustrated in Figure 1 which shows a series of individual pulses from PSR 1133 + 16. Despite this variation in shape of individual pulses, it is found that the mean or integrated pulse profile obtained by adding many pulses synchronously with the period is in most cases stable in shape.
A Gyro-Synchrotron Maser in the Solar Corona?
Authors: Melrose D. B. , White S. M.
Published: July 2016

Stewart (1978) has reported four moving type IV bursts observed with the Culgoora radio heliograph at 43, 80 and 160 MHz. After an early phase, the brightness temperatures of the observed bursts decreased with increasing frequency and with time. The highest brightness temperature observed at 43 MHz was 1010K, and it seems that the brightness temperature would have been still higher at even lower frequencies. Existing theoretical ideas on moving type IV bursts are based on data (at 80 MHz primarily) which included no brightness temperatures in excess of 109K. the accepted interpretation involved gyro-synchrotron radiation from mildly relativistic electrons (energies ≈ 100 keV); reabsorption by the electrons themselves restricts the brightness temperature to less than about 100 keV ≈ 109K (Wild and Smerd 1972, Dulk 1973). Stewart’s (1978) new data at 43 MHz require that this accepted interpretation be modified; he has suggested that higher energy electrons are involved. An alternative suggestion is explored here, namely that the absorption might be negative. In other words, the high brightness temperatures observed could be due to a gyro-synchrotron maser involving electrons with energies of about 100 keV.
Supernova Rates, Starbursts and Galaxy Inclinations
Authors: van den Bergh S.
Published: July 2016

The supernova rate in spirals of types Sc and Sd shows a sharp peak in face-on galaxies with inclination i ≤ 25°. This suggests that most supernovae in late-type galaxies occur in rich clusters or associations that are located at the base of chimney-like structures formed by a previous generation of supernovae. These chimneys are transparent because most of the dust contained in the rising column of gas within them had previously been destroyed in the hot bubble surrounding supernovae.
Inhomogeneities in Globular Clusters
Authors: Chun Mun-Suk
Published: July 2016

Inhomogeneities in globular clusters are reviewed with the observational evidence for chemical abundance variations from star to star in individual clusters and the large-scale structural variation of clusters. The reality of the radial colour gradient is tested in 47 Tuc (NGC 104). The result shows that the observed radial colour gradient comes from the integration of the calculated colours of individual stars. The cause of this radial colour variation is the result of the concentration of evolved stars and the reddening of the main sequence in the central region. We propose that the CNO abundance gradient in the early stage of a cluster’s formation is the interpretation of the observed radial colour gradient.
New Zealand Astronomy in the 1990s
Authors: Cottrell P. L.
Published: July 2016

There has been a dramatic increase in astronomical research output in New Zealand over the last decade. This is set to increase with the advent of a number of new pieces of astronomical hardware over the last five years. These include the 1m telescope and associated instrumentation at Mount John and the JANZOS collaboration, with its instrumentation on Black Birch. Black Birch is also the site of the US Naval Observatory’s southern hemisphere astrometric station, where, using a transit circle instrument, they are collecting data which will form part of the International Reference Star Catalogue. As well as these ‘professional’ programs there is also a large network of amateur astronomers, who can provide extremely useful input into certain astronomical programs at the various observatories around the country and the world.

A brief overview of the existing New Zealand astronomical scene will be followed by discussion of a number of new initiatives being proposed, which includes an automatic patrol telescope being developed by Carter Observatory, an expansion of the JANZOS collaboration and initial discussion about the possibility of an eastern arm for the Australia Telescope some where in New Zealand. In addition, for programs which require a long timebase of observations, extreme southerly latitudes or longitudinal coverage, New Zealand could provide a unique opportunity.
The Dust Opacity of Spiral Galaxies
Authors: Byun Y. I. , Freeman K. C.
Published: July 2016

In order to find the best observable diagnostics for the amount of internal extinction within spiral galaxies, we have constructed models for disk galaxies with immersed dust layers. The radiative transfer problem, including both scattering and pure absorption, has been computed for a range of model galaxies. This reveals a set of superior diagnostics for the opacity. These include the behaviour of the radial colour and luminosity distributions, the amplitude of the asymmetry between the near and far sides of the major axis, and their dependence on the orientation of the galaxy with respect to the observer.
High-resolution Na I Observations of the Local Interstellar Medium
Authors: Welsh Barry Y. , Vedder Peter W. , Vallerga John V.
Published: July 2016

We present high-resolution absorption measurements (R ~ 150 000) of the interstellar Na I D-lines at 5890 Å observed towards 46 early-type stars. The distance to these stars ranges from 20–200 pc, allowing a probe of the local interstellar medium (LISM). The velocity structure, velocity dispersions and column densities of the various cloud components have been derived using an absorption line-fitting analysis. Sodium column densities have been determined for 23 of the 46 target stars. No sodium absorption was detected towards any of the stars with distances < 43 pc. Such null results imply a corresponding hydrogen column density limit, N(H), of ~ 2.5 × 1018cm−2 in many directions in the LISM. For three exceptionally vacant lines of sight (to β CMa, 36 Lyn and η Hya) this limit of low hydrogen column density can be placed out to a much further distance of > 150 pc.

We have plotted the distribution of sodium column density in the LISM for a total of 118 stars in the form of three galactic maps. These maps qualitatively show that the present picture of the LISM, in which the first 50 pc is essentially free of dense clumps of neutral gas, is correct. Our map of sodium columns for stars with distances > 100 pc shows that the region within the galactic quadrant defined by 200° < l < 270° shows a conspicuous absence of any significant concentration of neutral gas. This region will be a prime direction of study for forthcoming soft X-ray and extreme ultraviolet satellite experiments.
IUE Spectral Analysis of the Be Star HD 184279
Authors: Dawanas D. N. , Hirata R.
Published: July 2016

The authors analyse four high-dispersion IUE spectra of HD 184279 observed in 1979 and 1982.
Photometric Monitoring of the Long-period Eclipsing Binaries at Yonsei University Observatory
Authors: Nha Seong , Lee Yong-Sam , Kim Ho
Published: July 2016

This paper is the second report since 1984 on the photometric monitoring of long-period eclipsing binary stars at Yonsei University Observatory using a 61-cm reflector.
China’s Postgraduate Education in Astronomy
Authors: Liu Lin
Published: July 2016

This paper summarises the opportunities available for postgraduate education in astronomy and related disciplines in China.
Education in Astronomy: Some Suggestions
Authors: Kalra G. L.
Published: July 2016

Astronomy is one of the most ancient disciplines of knowledge which has inspired a great deal of human thought. Its study has triggered developments in many fields. Bohr’s atomic model and our idea about the thermonuclear fusion are two of the many examples which have significantly influenced (and will continue to influence) the course of human civilisation.
The Bulletin ‘Teaching of Astronomy’
Authors: Isobe Syuzo
Published: July 2016

The paper briefly describes a new publication in Japan, the bulletin ‘Teaching of Astronomy in the Asian-Pacific Region’. The author is the Chairman of the Working Committee of Teaching of Astronomy in the Asian-Pacific region of the IAU.
Ground-based Gamma-ray Astronomy
Authors: Clay R.W. , DawSOn B.R.
Published: July 2016

Ground-based gamma-ray astronomy has slowly developed over the past quarter of a century to a position now where a number of sources are known to produce gamma-rays in the energy range 1011eV to 1018eV. The observations are difficult, with exceptional signal to noise problems, but improved techniques are now allowing observers to proceed with confidence. In this paper the physical bases of the observations are emphasised to show the important issues in the field and the present state of the observations is indicated.
Coherent Curvature Emission in Pulsar Magnetospheres: Non-dipolar Geometric Effects
Authors: Luo Qinghuan
Published: July 2016

The effects of the specific geometry of the magnetic field (such as field lines with torsion) on curvature emission and absorption in pulsar magnetospheres are discussed. Curvature maser emission can arise from two effects: the curvature drift, as has already been discussed in the literature, and field line torsion as discussed here in detail for the first time. Maser emission due to field line torsion can operate only when the Lorentz factor is larger than a certain value. However, when the Lorentz factor of electrons or positrons is sufficiently high, curvature masering is due to both curvature drift and magnetic field line torsion. The optical depth in the case of field line torsion is estimated. It is shown that if torsion is due to rotation, the resultant luminosity should be dependent on the rotation period in such a way that shorter periods correspond to larger luminosities.
Are Gamma-Ray Bursts At Cosmological Distances?
Authors: Webster Rachel , Blaes Omer
Published: July 2016

We review the discovery of gamma-ray bursts, and summarise the new data from the Compton Gamma-Ray Observatory. We evaluate the evidence that gamma-ray bursts are at cosmological distances, and discuss applications of such gamma-ray bursts to cosmological problems.
Synchrotron Bubbles and Radio Transients
Authors: Ball Lewis , Vlassis Michael
Published: July 2016

We discuss a generalisation of the synchrotron bubble model which has been applied to short-lived radio transients which can peak and decay over just a few days. The assumptions of the simple model imply that when the flux is increasing with time, it must also be an increasing function of frequency. Observations of two recent radio transients, Nova Muscae 1991 and the Galactic Centre Transient, include the first data showing such a rising phase, and in both cases the radio flux was a decreasing function of frequency during the observed rising phases. Thus the simple synchrotron bubble model is inadequate, at least for these events. A fundamental feature of the simple model is the assumption that the process accelerating the radiating electrons ceases before the radio emission can escape. We relax this assumption by including an injection of electrons, with a constant energy spectrum, into the synchrotron bubble.
Interpretation of a Correlation between the Flux Densities of Extended Hard X-ray and Microwave Solar Bursts
Authors: Nelson G. J. , Stewart R. T.
Published: July 2016

In a previous paper of this issue (Stewart and Nelson 1979 — Paper A) we showed that for extended bursts a good correlation exists between the observed 100 keV X-ray slux density and the 3.75 or 9.4 GHz microwave flux density. We also showed that the microwave spectrum of these bursts was much flatter (S ∝ f1.0 on the average) than the optically thick (self-absorbed) spectrum observed for impulsive microwave bursts (Crannell et al. 1978; Dulk et al. 1978). Furthermore, the microwave turnover frequency was > 10 GHz in eight of the nine events studied and <20 GHz in four of these cases. The remaining event, which was severely occulted by the solar limb, had a turnover frequency of ∽ 1 GHz.
Accurate Radio Positions with the Tidbinbilla Interferometer
Authors: Batty M. J. , Jauncey David L. , Rayner P. T. , Gulkis S.
Published: July 2016

Radio position measurements with an error of <2” arc rms allow reliable optical identifications of compact radio sources to be made solely on the basis of radio-optical position coincidence. In this way neutral or red stellar objects, faint compact galaxies and faint QSOs can be reliably identified. Such identifications are of particular interest because they are rich in BL Lac objects, high-redshift QSOs, QSOs with unusual optical emission or absorption spectra and galaxies with active nuclei (see Jaunceyet al. 1978).
John Tebbutt and the Astronomy at Windsor Observatory
Authors: White G. L
Published: July 2016

About 1 km to the east of the township of Windsor, NSW and only 50 ft above mean tide level, stands the remains of one of the first observatories in Australia. Here John Tebbutt established his private observatory and for over 60 years continued a remarkable career as a gentleman astronomer in the best tradition of 19th century Europe.
A Monte Carlo Model for Light Scattering by Dark Nebulae
Authors: Darby M. I. , King D. J. , Taylor K. N. R.
Published: July 2016

The Thumbprint Nebula (TPN) in Chamaeleon (first described by Fitzgerald (1974), and shown in Figure 1) is a good example of the class of dense, dark nebulae that exhibit dark cores and bright rims, and have been referred to (Lynds 1967) as ‘bright dark nebulae’. Early observations of these nebulae established that the dust grains within them were strongly forward-scattering (Struve and Elvey 1936, Struve 1937). However, the treatment of the radiative transfer problem was too inadequate to permit more than tentative conclusions regarding the nebulae. In more recent years, with the advent of modern computers, the transfer of radiation through a dust cloud has been treated more rigorously, using Monte Carlo techniques (Mattila 1970, Witt and Stephens 1974). Witt and Stephens (1974) have demonstrated that for a dense nebula the surface brightness profile is sensitive to the dust grain density distribution within the cloud and to the scattering properties of the grains. The scattering model approach can be valuable in the investigation of very opaque dark nebulae that cannot be studied by conventional star counting techniques. This has been demonstrated in the case of the TPN by Fitzgerald et al (1976), who used the Witt and Stephens model.
Optical Line Studies of the Nuclei of NGC 4945 and 5128
Authors: Whiteoak J. B. , Gardner F. F.
Published: July 2016

Microwave line investigations have shown that several bright southern galaxies contain dense molecular clouds overlying bright radio nuclei (see e.g. Whiteoak 1978). In terms of general kinematic models of galaxies the clouds have velocities that are anomalous, being consistent with radial motions both towards and away from the nucleus. To extend our knowledge of these motions we are investigating the distribution of optical spectral lines near the nuclei of the galaxies. We present here preliminary results for NGC 4945 and 5128.
A ‘Narrabri’ Binary Star Resolved by Speckle Interferometry
Authors: Tango W. J. , Davis J. , Thompson R. J. , Brown R. Hanbury
Published: July 2016

The Chatterton Astronomy Department of Sydney University, in collaboration with the Astronomy Group of Imperial College (London), has carried out a program of speckle interferometry on the 3.9 m Anglo-Australian Telescope (AAT). Over 2 km of film were exposed during the two observing sessions in November and December, 1978, and the analysis of this very large amount of data is being carried out at the present time.
80 MHz Survey of Extra-Galactic X-ray Sources
Authors: Slee O. B. , Quinn P. J.
Published: July 2016

The completion of the Uhuru (Forman et al. 1978) and Ariel V (Cooke et al. 1978) surveys of the sky for X-ray emission has resulted in many proposed identifications with individual galaxies and clusters of galaxies. The X-ray positions are not usually accurate enough to enable a positive identification to be made of the X-ray sources with optical or radio objects, and hence the identification is often based on statistical arguments — viz., the unexpected occurrence of unusual galaxies, radio sources or clusters of galaxies within or near the X-ray error boxes. There is usually no significant information available on the angular size of the X-ray emitter but in two or three cases (e.g. Perseus cluster, Coma cluster and Virgo cluster) the angular resolution is good enough to identify a broad component with dimensions approaching those of the whole cluster. This extended X-ray emission has been ascribed to either inverse Compton scattering of the 3° microwave background by relativistic electrons in the intra-cluster medium or to thermal-bremsstrahlung emission by an optically thin plasma at - 10s K.
3.3 GHz Ground-State Transitions of CH towards Southern HII Regions–1. An Atlas of CH Profiles
Authors: Whiteoak J. B. , Gardner F. F. , Manefield Gwenyth A. , Höglund B. , Johansson L. E. B.
Published: July 2016

The Parkes 64-m radio telescope equipped with a 3 GHz maser on loan from the Onsala Space Observatory has been used to observe the three ground-state transitions of CH (at 3264, 3335 and 3349 MHz) towards a total of 74 HII regions, mostly at southern declinations. In this paper the regions and related characteristics are listed, and the CH spectra displayed.
A New Very High Angular Resolution Stellar Interferometer
Authors: Davis J . , Tango W . J .
Published: July 2016

The Chatterton Astronomy Department of the University of Sydney is proposing the construction of a very high angular resolution stellar interferometer of major astronomical and international significance. Based on the prototype modern Michelson stellar interferometer which the Department has developed, the new instrument will be used in a wide range of astrophysical programmes. The siting, specification, design and costing of the instrument are outlined.
Radio Continuum Emission from Sculptor Galaxies
Authors: Harnet J . I.
Published: July 2016

The five major members of the Sculptor Group of galaxies and NGC 45 have been observed with the Molonglo observatory synthesis telescope. NGC 247 and NGC 300 were not detected and upper limits to their 843 MHz flux densities are given. Radio emission from NGC 7793 is discussed with particular attention to its morphology, radial dependence compared with that of the blue light and possible coincidences between HII regions and 843 MHz peak flux densities.
Astronomy with the Fleurs Six-Dish Array
Authors: Batty Michael J . , Bunton John D. , Brown David R. , Corben Julian B. , White Graeme L.
Published: July 2016

Operation of the six 13.7 m antennas of the Fleurs synthesis telescope as a sub-array has provided a new and surprisingly versatile astronomical tool. With enhanced reliability and fully automated operation, unattended observing over several days is possible. Interleaved ‘multiple-snapshot’ observations of many fields per day can be made.

The array has shown itself to be particularly suitable for the measurement of precision (a few arcsecond) positions for the optical identification of a large number of radio sources, a survey of compact sources and the monitoring of the activity of several radio stars over periods of weeks. At present a program of recalibration is under way to improve the positional accuracy and dynamic range of the instrument.
SCIENCE, COMMODITIES, AND CORRUPTION IN THE GILDED AGE
Authors: Singerman David Roth
Published: July 2016

This essay argues that categories of corruption and reform, so often used by historians to assess the Gilded Age, are themselves the ideological products of the period's struggles for political, economic, and social power. It does so by exploring fierce disputes over how to value sugar, a crucial commodity in the political economy of the late nineteenth-century United States. Confronted with evidence of massive fraud, the Treasury hoped that chemical techniques would rationalize the collection of sugar tariffs. Instead their introduction enabled the rise of the notorious Sugar Trust, by making it more difficult to distinguish corrupt influence from the legitimate exercise of expert judgment.

Sugar exemplifies how Gilded Age battles over corruption should be seen in the broader and longer context of the history of capitalism, in which self-proclaimed reformers have used charges of fraud and adulteration to discredit the knowledge of artisans and workers while mantling themselves in claims to objectivity and reason. Scientific knowledge, far from being the inevitable ally of accountability and good governance, could just as easily be deployed to obfuscate and confuse, and thereby to wrest control of social and economic power.
Graft is good: the economic and environmental benefits of grafted naranjilla in the Andean region
Authors: Clements Corinna , Alwang Jeffrey , Barrera Victor , Dominguez Juan Manuel
Published: July 2016

Naranjilla cultivation is highly profitable in many parts of the Andean foothills in Colombia and Ecuador. Its susceptibility to soil-borne diseases, however, lowers its economic benefits, reduces sustainability of production and increases its contribution to environmental degradation. This paper presents an analysis of the potential market and non-market benefits of research that developed and tested the grafting of common naranjilla onto disease-resistant rootstock. Grafting reduces the need for pesticide application and increases the longevity and sustainability of the plant. An economic surplus approach, carefully calibrated to reflect the realities of naranjilla production, was employed to show the large benefits from such research. Environmental and health benefits are very close in magnitude to market-mediated surplus gains. The results show substantial potential benefits from an outreach program to diffuse the new technology.
The Unavoidable Necessity of Formalizing Condominium Ownership in China: A Pilot Study
Authors: Chen Lei , Mostert Hanri
Published: July 2016

This article identifies the problems and malfunctions of the Chinese apartment ownership regime that necessitates its formalization. The benefits of formalizing the apartment ownership, such as resolution of the social housing problem, and establishment of the mortgage-backed real estate market, are presented. Thereafter, we indicate that the success of formalizing apartment ownership in China depends on one hand on the extent to which the unique property market in China can be reconciled with acknowledged ways of dealing with apartment ownership in various other jurisdictions acting as comparative examples. On the other hand, simply grafting borrowed laws or legal institutions into a new context cannot achieve the desired effects. Legal culture matters and it cannot be downplayed in the formalizing process. Our conclusion is that the booming but immature Chinese apartment ownership market will benefit greatly if the casual link between the market economy and well-defined property rights are confirmed through legal formalization.
Secularism, the Islamic State and the Malaysian Legal Profession
Authors: Whiting Amanda J.
Published: July 2016

Eschewing theoretical discussion of both “secularism” and the “Islamic state,” this article instead examines situated understandings of these ideas as they emerge in contests about the place of religion in Malaysian law, politics and society, paying particular attention to the views of Malaysian legal professionals. It examines the official positions taken by the peak professional legal organisation (the Malaysian Bar Council) speaking on behalf of its professional constituents and to a wider constituency of Malaysia citizens in order to examine how the organised Bar has used its prestige and expertise to explain and clarify the legal aspects of these issues to the general public and how it has attempted to use its privileged status to foster informed discussion about law reform.
The Philippine President as Tortfeasor-in-Chief: Establishing Civil Liability for Constitutional Negligence
Authors: Hilbay Florin Ternal
Published: July 2016

This article analyzes the liability of the Philippine President for the tort of constitutional negligence in relation to the murders and forced disappearances of leftists, journalists, and other dissidents. It uses the international law doctrine of command responsibility as a form of attribution that may be used, by analogy, to hold the President accountable for a culture of impunity. The article describes the role of the President as the regulator of a human rights-conducive information ecology and argues that massive human rights violations meant to silence dissidents are a source of liability for which a class action suit is an available remedy. Finally, it looks at the concept of presidential immunity from suit from a comparative perspective and argues that the continued application of restrictive immunity rules established during the American colonial era is misplaced considering the universalist design of the present Philippine Constitution and developments in immunity jurisprudence in the United States.