bluuebunny/crossref_metadata_2025 huggingface dataset:
Twin Registers A progress report
Authors: Gedda L. , Milani-Comparetti M.
Published: July 2016

The Mendel Institute in Rome houses a Twin Register that was initiated by the senior author even before the opening of the Institute (September 1953).

The purpose of the Twin Register, originally limited to research on twin concordances as to blood glutathione levels (a subject that is still under investigation, as shown by the report presented at this Symposium by Gedda and Tatarelli), was gradually widened to cover the full horizon of twin studies.

The realization that the twin method, in its various formulations, is irreplaceable in most areas of biomedical research, led to the decision to include in the Register each and every contactable twin pair; wide use of mass media was made for recruitment purposes.

Recruitment generally occurred at very early ages, and all pairs are constantly followed. Formerly, definite zygosity determinations were obtained only for those pairs that were selected for specific research purposes. Zygosity determinations are currently being extended to all those pairs who come to the Institute's clinics, within the limits of the available budget (it should be noted that the Institute is a private foundation which provides free medical care to any twin. Lack of capital funds forces the Institute to limit its research activities to those for which grants are obtained).
The Swedish Twin Registry Past and future use
Authors: Cederlöf R. , Floderus B. , Friberg L.
Published: July 2016

The Swedish Twin Registry of the Karolinska Institute comprises about 10 000 sets of twins, and was built up in 1961-1962. It covers about 95% of all Swedish same-sexed twins that were born in the country in 1886-192 5 and were still living as unbroken pairs at the time of compilation.

The compilation procedure has been presented in detail by Cederlöf (1966a), and will be summarized as follows. Since the middle of the last century, a rather unique system for population registration has existed in Sweden. It is based not only on birth records, but also on migration records. As soon as an individual moves away from the place he lives, he has to notify the authorities as to where he moves. This system made it possible for us to follow-up any individual from his place of birth to his next place of living, and so on, until we found his current address or had to discard him as deceased. We started, in that way, with about 41 000 multiple birth records, handscreened from about 3½ million birth records from all Sweden during the period in question, and ended with a series of about 12 000 located sets of twins. Of the remainder, about 26 000 had to be discarded, due to death of one or both partners; 1 000, due to emigration to foreign countries; and 100, due to hospitalization in mental asylums, or home for aged people, etc. In the compilation procedure we lost track of about 1 100 individuals, or 1.5%.

The zygosity of the twins has been determined with the aid of some similarity questions contained in a questionnaire, mailed to all the twins in the registry. Out of several questions, one proved to be of high reliability, namely the very simple question whether the twins as children were as alike as two peas in a pod, or of family likeness only. We assumed that if both twins in a set agreed in saying that they had been as alike as two peas in a pod, the pair was MZ. If they, on the other hand, agreed in saying that they had been of family likeness only, we regarded the pair as DZ. We validated this questionnaire diagnosis by analyzing the outcome from a subsample of 200 pairs who had also been examined serologically in regard to five markers, A1A2BO, MN, Rh, Hp, and Gm. The results were reported here in Rome in 1961 and showed an agreement in diagnoses of 95% for MZ and 90% for DZ (Cederlöf et al, 1061).
Experimental Inhibition of the Virus-Induced Rauscher Leukemia of the Mouse
Authors: Seidel H. J.
Published: July 2016

Chemotherapy of murine Rauscher virus-induced leukemia using Trenimon, 6-Mercaptopurine, 5-Fluorouracil and Melphalan is described. Therapy is based on nucleated cell counts in peripheral blood and body weight of the animals. Remarkable remissions of the number of nucleated cells — not occurring in untreated animals — are induced by Trenimon and 6-Mercaptopurine. Prolongation of survival times exceeds 100% in the groups treated with Trenimon, 6-Mercaptopurine, and 5-Fluorouracil.
Introduction to the General Discussion on the Cytological and Haematological Effects of Antimitotics
Authors: Astaldi G.
Published: July 2016

I will just make a few remarks before opening this General Discussion on the Cytological and Haematological effects of Antimitotics. I believe that numerous and interesting will be your comments. Let me first go back very briefly to the pioneer of these compounds, colchicine, already mentioned in the Egyptian, Greek, and Roman Pharmacology, but whose stathmokinetic effect was illustrated by P. Dustin Sr. just in 1934. We are lucky enough to have in our program the Dustin name perpetrated through his son, A. P. Dustin Jr.

Several years ago, since 1947 on, my group adopted colchicine to perform a test for evaluating in tissue culture the proliferative activity of the blood-forming cells from different physio-pathologic conditions. Using that method, among other it was possible to ascertain that — contrary to expectations — the proliferative activity of the bone marrow cells in human leukaemias is rather low, and this finding has been later confirmed by many investigators using different approachments and methods. Quite recently, in collaboration with Gociu M. and Airò R., I have started investigating the effect of colchicine on the blastic transformation of human peripheral blood lymphocytes stimulated with Phytohaemagglutinin (Phyto) in cell culture. The main purposes of this research project are:

1. To test the effect of colchicine on the blastic development process, which occurs as a consequence of such an intense RNA- and DNA- synthesis presented by human lymphocytes in the Phyto-culture system;

2. To evaluate the extent of proliferation of the Phyto-stimulated lymphocytes, because the divisions which occur in these cells could definitely contribute in making higher their number. (In fact, the number of the blast-like cells obtained after 3-4 days of cell culture with Phyto is a function not only of the number of the lymphocytes which undergo blastic transformation, but also of the number of the same blastlike cells which undergo mitotic division).
A case of uniovular Twins of which one child was normal and the other had the syndrome of mongolism
Authors: van Beukering J. A. , Vervoorn J. D.
Published: July 2016

An African woman of about 40 years old reported to the out-patients' department on 31st January 1955 because of nausea and vomiting, with amenorrhoea of three months duration. Examination revealed a 2-months' pregnancy. She had six normal deliveries of which three children were still living.

On 3rd February she reported again, complaining of stomach-ache and diarrhoea. The stool examination showed some leucocytes and erythrocytes, but no amoebae, cysts or parasitic ova. On 23rd February the woman again reported, this time with a simple pharyngitis. She came again on 29th June for pre-natal examination and treatment. She had no complaints and was seen to be about 32 weeks pregnant, with a moderate degree of hydramnios. The foetal heart was inaudible.

On 1st August she was admitted to hospital in labour. The membranes were intact, the cervix fully dilatated and presentation was occipito-anterior of the vertex. Artificial rupture of the membranes released only a small amount of amniotic fluid, but labour proceeded normally with the usual quantity of fluid accompanying the birth. Immediately this child was born another bag of waters presented, which was ruptured to release about six pints of amniotic fluid. A second baby now presented by the breech and was delivered by Bracht's method. We noticed at once that this second baby was affected by mongolism.
Eineiige Zwillingsmädchen mit konkordantem Albinismus Universalis aus Ehe normalpigmentierter, aber entsprechend belasteter Vettern I. Grades in oberitalienischem Isolat
Authors: Hanhart Ernst
Published: July 2016

Two monozygous twin girls, now 7 years old, with complete concordance of an almost total universal albinism were found in an « isolate » near Aosta in the Western Italian Alps. Their parents show normal pigmentation, and are first cousins, their common grandmothers having a brother who was the grandfather of another albinotic girl, aged 22. The parents of the latter were examined by the Dutch ophthalmogeneticist P. J. Waardenburg: while her father did not show definitely diaphane irides, her mother did. As a similar discrepancy in otherwise normal parents of albinos was stated in 2 more families (Hanhart 1952), the presence of diaphane or not diaphane irides cannot be regarded as sufficient symptom to distinguish two different biotypes of simple-recessive universal albinism. Heterogeny, though rather probable, of this character has not yet been proved in white man.

In Switzerland, and Italy as well, there are considerable local accumulations of universal albinism, so that calculations on the basis of a medium frequency do not hold. The percentage of 7.9 for first cousin marriages of normal parents of albinotic children and 8% for second cousins can hardly be taken as a proof for heterogeny of the gene concerned.

The observation of monozygous twins with concordant universal albinism is the first made in Europe, and the third published all over the world. It is unique on account of the near consanguinity of the normal parents of these twins. Its incidence in Northern Italy speaks in favour of a relatively frequent occurrence of this character in this country, suggested already by the author's population studies.
Oxycéphalie chez trois paires de jumeaux univitellins, associée dans un des cas à une cutis frontis gyrata
Authors: Franceschetti A. , Klein D.
Published: July 2016

Description of 3 cases of identical twins affected by concordant oxycephaly. In the first case, one of the twins had a son who was likewise afflicted by a typical scaphocephaly. In the second case, both children showed also a convergent concomitant strabismus, which was latent in one and manifest in the other, and moreover a concordant ptosis. In the third case, the oxycephaly was associated with cutis frontis gyrata homologous in both twins.

A confrontation of the cases of oxycephaly in identical twins based on the literature and our personal cases, shows clearly a majority in favour of concordance : 25 concordant pairs as compared to 10 discordant ones; the fraternal twins (7-8 cases) are all discordant as regards oxycephaly. The cases of discordant oxycephaly in monozygotic twins must therefore be interpreted as the result of an unstable gene of feeble penetrance. The conclusion of the genotypic origin of oxycephaly is corroborated by some pedigrees showing a transmission through 2 or more generations. Two reported cases with consanguinity of the parents suggest likewise the possibility of recessive inheritance.

The association of oxycephaly with cutis frontis gyrata, as observed in our third case, having not yet been described, we cannot for the moment decide whether this combination is due to chance or whether there exists a pathogenic correlation between both anomalies.
A Genetic Study of Paget’s Disease (Osteitis Deformans) in Monozygotic Twin Brothers
Authors: Aschner Bertha M. , Hurst Lewis A. , Roizin Leon
Published: July 2016

Observation of the behaviour of a pair of one-egg twins, incompletely concordant with resspect to Paget’s disease, is consistent with the courrent theory (based on 57 families in which the disease has occurred in more than one member of the family, and one other pair of one-egg twins), that the condition is of genetic origin, the gene responsible being an incompletely dominant autosomal gene with variable degrees of penetrance and expressivity.
Ricerche Sulla Eredità Delle Malattie Allergiche
Authors: Carbonera P. , Cresseri A.
Published: July 2016

The Authors from the examination of a group of pedigrees belonging to subjects with allergopathies conclude that in their observations allergopathies behave like monomeric dominant forms with little penetrance. Afterwards they propose an explanation of the relative excess of sick persons in the discordant marriages and of the remarkable incidence of pollinosis.
Schizoidness in Twins
Authors: Planansky Karel
Published: July 2016

Discordant schizophrenic monozygotic twin pairs were examined in order to clarify the view interpreting schizoid disorders as attenuated or incomplete expressions of schizophrenic heredity. The aggregate observations indicate that typical schizophrenia can be paired with all types and degrees of schizophrenic or schizoid illness, including clinical normality. These intra-pair combinations seem to occur more or less at random. The reviewed schizoid states showing evidence of schizophrenic psychopathology represent one of the developmental phases of schizophrenic process. Yet the psychopathologic connection with schizophrenia is not evident in all deviations and non-deviant personality patterns. Thus the seeming continuum of schizophnic psychosis — schizoid disorder — neurotic character — normal personality may consist of two discrete series: one with underlying schizophrenic psychopathology, and the other independent of the psychotic process. This division might reflect a threshold effect, dependent upon a switch mechanism.
X-Ray Emissions from Solar Flares and from Celestial Sources
Authors: Chubb T. A.
Published: July 2016

One of the interesting questions in solar X-ray astronomy is the question as to whether the hard X-ray emission which occurs during major solar flares is a thermal or nonthermal phenomenon. The evidence for non-thermal emission has been based in large measure on a balloon-borne experiment by Peterson and Winckler, which constituted the first detection of high energy flare X-rays. In the Peterson-Winckler experiment, the incident solar X-rays were measured by both an ion chamber and a Geiger counter photometer, and from the ratio of responses, the hardness character of the incident X-rays was reduced. It was concluded that the observed result could have been explained in terms of the sudden non-thermal production of a group of electrons with energy of the order of 500 kilovolts.
A Study of the Seyfert Galaxy NGC 4151
Authors: Oke J. B. , Sargent Wallace L. W.
Published: July 2016

The small group of known Seyfert galaxies (Seyfert 1943) is of interest because it is clear that some violent activity is occurring in the nucleus, and some of the properties suggest a relationship with quasi-stellar sources. The spectrum of a Seyfert galaxy consists of strong, often very broad, emission lines superposed on a continuous spectrum which in some cases shows no absorption-line features. Two of the galaxies, NGC 1068 and 1275, are radio galaxies and the latter is known to be variable at radio frequencies (Dent 1966).
The Nuclei of Planetary Nebulae
Authors: Faulkner D.J.
Published: July 2016

For some years now, there have been suggestions that the nuclei of planetary nebulae are stars undergoing a final gravitational contraction to the white dwarf state. These have culminated in two important studies by O’Dell, and by Seaton and his collaborators, the results of which are indicated on the Hertzsprung-Russell diagram of Figure 1. The temperatures and the distances—and hence luminosities—of the central stars are obtained from flux observations of the stars themselves and the surrounding nebular shells, the former by the Zanstra method, and the latter by that of Shklovsky.
The Formation of Simultaneous Radio Astronomical Images and Spectra by Electro-Optic Methods
Authors: McLean D. J.
Published: July 2016

This communication describes techniques, new to radio astronomy, which permit the analysis of electrical signals at radio-frequencies by optical methods.

Two applications will be described: the first is to a spectrograph which gives the instantaneous power spectrum of a single broad-band electrical signal; the second is to the analysis of the signals from a number of aerials of an array in order to form a simultaneous image of the brightness distribution of the region of the sky under observation.
Optical “Seeing” over Level Terrain
Authors: Coulman C. E.
Published: July 2016

This work is aimed at understanding the phenomena which affect the sharpness and stability of optical images transmitted through the atmosphere. A brief description is given of the results obtained to date from an experimental field-study directed at establishing a connection between optics and meteorology. Most of the work has, so far, been conducted in daytime because our main application is to solar astronomy; other fields such as surveying, aerial reconnaissance and so on can also benefit from basic research in atmospheric optics.

A horizontal line of sight over uniform, level terrain presents the simplest case for study. The optical transfer function (OTF) of the system comprising an air-path and telescope objective has been measured with an image analyser which is a modified form of stellar seeing-monitor. The outputs of this analyser are proportional to the modulus and argument of the OTF. The modulus, or modulation transfer function (MTF), is a measure of image contrast; the fluctuations of the argument measure image movement, or “dancing”. The OTF is a function of spatial frequency f (cycles per unit distance) which may be altered by radial movement of the scanning graticule of the image-analvser.
The Radioheliograph and the Radio Astronomy Programme of the Culgoora Observatory
Authors: Wild J.P.
Published: July 2016

The radio installations at Culgoora Observatory evolved from the work carried out at Dapto field station between 1952 and 1965—which in turn was based on earlier observations. The basic instrument at Dapto was a radiospectrograph which produced two solar spectra per second over a frequency range originally of 40-210 MHz and finally of 5-2000 MHz. Until 1957 the Dapto radio spectrograph was the only one operating in the world and it fell upon this instrument to reveal many of the spectral phenomena which are now well known. The spectrograph observations referred to the total flux from the Sun observations with high directivity began at Dapto in 1958 with the introduction of a swept-frequency interferometer which measured the one-dimensional (east-west) positions of bursts and their approximate angular size over a continuous range of frequencies between 40 and 70 MHz. The results obtained from this combination of spectrograph and interferometer indicated that great advances would be made in our knowledge and understanding of the phenomena if two-dimensional metre-wavelength pictures of the Sun could somehow be recorded at short time intervals of about Is—again in combination with spectrographic observations. This requirement led to the start of the radioheliograph project. One requirement for this instrument was a site with linear dimensions of the order of 3x3 km. This was far too large for the Dapto site and a new site was selected at Culgoora in the north-west plains of New South Wales. The virtues of this site are its size, flatness, freedom from flooding, low radio noise level and accessibility from Sydney by air transport. Its sunshine and optical-seeing properties also made it a highly desirable site for optical observations, and developments assumed a new significance when Dr. Giovanelli and his optical colleagues decided to join us at the same observatory.
A New Compound Interferometer Operating at 160 MHz at Nobeyama
Authors: Takakura T. , Tsuchiya A. , Morimoto M. , Kai K.
Published: July 2016

During the last solar cycle a number of observations of solar radio emissions were made in a wide frequency range from which an enormous amount of information has been obtained. However the results obtained so far are limited by rather poor angular resolution. Observations with much higher resolution (of the order of 1′ arc) have been required for further studies of solar radio emissions. At the present stage such observations have proceeded in the microwave range; also the radioheliograph at 80 MHz has just started at the Culgoora Observatory. At the Tokyo Astronomical Observatory a high-resolution study of radio bursts in the metre-wave range has been planned since 1960, and the construction of a new compound interferometer operating at 160.3 MHz was started in April 1967 at a new site, Nobeyama. This site, located about 150 km north-west of Tokyo, is surrounded by mountains and quite free from man-made interference. We shall give a brief description of this equipment; details will be published later.
The Effect of lo on Jupiter’s Decametric Emissions
Authors: McCulloch P.M.
Published: July 2016

The innermost Galilean satellite of Jupiter, Io, has been observed to strongly modulate the probability and intensity of Jupiter’s decametric emissions. The effect is most pronounced at frequencies greater than 30 MHz. Radiation occurs from two configurations of Jupiter and Io, the first when Io is 90° from superior geocentric conjunction (s.g.c.) and Jupiter’s longitude is near 120°, and the second when Io is 240° from s.g.c. and Jupiter’s longitude is near 230°.
A Summary of Recent Observations with the Parkes Interferometer
Authors: Wall J.V. , Cole D.J. , Milne D.K.
Published: July 2016

The Parkes interferometer consists of the 210-ft para-boloidal reflector of the ANRAO, and a 60-ft paraboloidal reflector mounted on rail tracks. These extend from 400 ft to 1400 ft from the 210-ft paraboloid and run both north-south and east-west. The baseline may be continuously varied during observation; receivers operating simultaneously at 468 and 1402 MHz enable the determination of complete visibility functions over the range 200λ to 2000λ.
11 cm Radio Sources Associated with Clusters of Galaxies
Authors: Komesaroff M. M. , Slee O.B. , Higgins C.S.
Published: July 2016

A survey of clusters of galaxies from Abell’s catalogue has been carried out using the Mk II 11 cm receiver recently installed at Parkes. For the present preliminary report only sources with flux densities down to about 0.3 f.u. will be considered, although the sensitivity limit of the receiver is about one-sixth of that value.
Astrophysical Aspects of Cosmic-Ray Research at Hobart
Authors: Fenton A.G. , Fenton K.B.
Published: July 2016

Using a network of ground-based stations stretching from Lae, New Guinea, to the Antarctic, and high altitude balloons and rockets, the Hobart cosmic ray group is studying several aspects of naturally-occurring high energy radiation.
The Chemical Composition of the Sun and the Solar System
Authors: Aller L. H.
Published: July 2016

A knowledge of the quantitative chemical composition of the primordial solar system must underlie all comprehensive studies of its origin and evolution. Usually we take the composition of the surface layers (photosphere) of the Sun as representative of this composition (except perhaps for deuterium, Li, B, and Be).
An Anomalous Forbush Decrease
Authors: Humble J. E.
Published: July 2016

Ground level detectors observed several major changes in the primary cosmic-ray flux during November 4960. Large increases, of solar origin, occurred on November 12 and 15, and a smaller one on November 20. The galactic flux in the region of the Earth was severely reduced by a Forbush decrease on November 12, and remained notably depressed until November 25. Considerable magnetic activity was observed throughout the period. Several models have been proposed to account for these observations.
High-Energy Cosmic-Ray Muons from a Weak Interaction
Authors: Campbell J. A.
Published: July 2016

A recent measurement of muon flux at energies greater than 1012 eV provides evidence for muon production by a process other than pion decay in cosmic-ray showers. Near this characteristic energy, the existing theory of weak interactions requires modification if it is not to violate a limitation (2) imposed by unitarity, which represents the conservation of probability. This work is an examination of modifications that are needed if the framework (4) of the theory is to be retained.
The X-Ray Spectrum of Sco XR-1 to 100 keV
Authors: Davison P. J. N.
Published: July 2016

This paper presents the results of a measurement of the high-energy (E ≥ 17 keV) X-ray flux from Sco XR-1 extending to higher energies than has previously been reported. The measurement was made during a balloon flight launched from Mildura, Australia, on 29 February 1968. The X-ray observatory contained two independent X-ray detectors, one being similar in principle to the active collimator detector pioneered by Peterson et al., the other being basically similar to the graded shield detector developed by Boldt et al. Our two detecting systems are described in more detail by Buselli et al. and also in previous papers of this conference.
Interactions Between Distant Centres Around the Sun
Authors: Wild J. P.
Published: July 2016

Until comparatively recently solar activity was discussed in terms of independent centres around the Sun’s surface. These centres, which form a constantly but slowly changing pattern, were thought to be linked only beneath the photosphere by tangled magnetic fields, themselves dominated by the mechanical energy of mass motions at photospheric and lower levels. Recent discoveries now indicate that active centres interact with one another above photospheric level and especially through linkages within the corona. The linkages appear to be of at least two distinctive kinds: magneto-hydrodynamic shock waves capable of travelling vast distances through the corona at ∼103 km/s and triggering eruptions at distant centres; and magnetic field lines which loop high and wide in the corona and convey energy in the form of fast particles. These two kinds of interaction will be considered in turn.
Observations of Motions in a Solar Storm Centre
Authors: McLean D. J.
Published: July 2016

With a number of important exceptions associated with transitory flare activity, most persistent sources of solar radio emission observed to date with the 80 MHz Culgoora radioheliograph have been stable in position over periods of tens of minutes or hours even though they fluctuated greatly in intensity. During several hours on 1968 November 11, however, we observed some interesting activity which showed frequent changes in the position of a source.
The Heights of Solar Radio Sources at 1424 MHz and 696 MHz
Authors: Cole D. G. , Mullaly R. F.
Published: July 2016

The heights of solar radio sources at 1424 MHz and 696 MHz have been measured during the years 1965 and 1966. Solar activity at this time was near minimum. The number of radio sources appearing on the solar disk rarely exceeded three at any time and it thus was possible to resolve the majority of these with a high resolution grating interferometer. Many of the previous height measurements at these frequencies have been made near times of maximum solar activity and the confusion of sources within the beam has limited their accuracy. The number of sources studied here is quite considerably higher than in any previous investigation at these frequencies, and the period of observation has been continuous.
Observations of Emission from Saturn at 408 MHz
Authors: McAdam W. B.
Published: July 2016

Following the detection of a high flux density from Saturn at 21.2 cm by Davies and Williams and the confirmation by Kellermann, it has been known that the radio emission from Saturn is enhanced at long wavelengths. The Molonglo cross telescope has searched for this emission at 73.5 cm on two occasions, the first in 1967 November when the planet was stationary, and the second during the opposition of 1968 October. Between these dates, installation of preamplifiers on the EW arm doubled the sensitivity of the cross so that although the same procedures were used on both occasions, this paper is based almost entirely on the recent results.
The Occultation of BD -17° 4388 by Neptune: II. Photo-electric observations
Authors: LyngÅ G. , Freeman K. C. , Miller M. J. , Serkowski K. , Stokes N.
Published: July 2016

Photo-electric observations of the occultation of BD —17°4388 by Neptune on 1968 April 7 were made with instruments and techniques as listed in Table I. A preliminary report of these observations has been given in IAU Circular No. 2067.
A Comparison of Pulse Shapes of Pulsars at Different Frequencies
Authors: McCulloch P. M. , Hamilton P. A. , Komesaroff M. M. , Cooke D. J.
Published: July 2016

Observations at a number of frequencies indicate that for at least two pulsars the average pulse shape has a slow but quite definite frequency dependence. Figure 1 shows average pulse shapes for CP 1919, CP 0950 and CP 1133. With the exception of those at 408 MHz these results were obtained at Parkes. The 408 MHz pulse shapes were obtained at Jodrell Bank by Lyne and Rickett. Circumstances of the observations are listed in Table I. Linearly polarized feeds were used at all frequencies.
X-Ray Astronomy: The Extension of Celestial X-ray Spectra to Higher Proton Energies
Authors: McCracken K. G.
Published: July 2016

The three objects Tau X−1, Cyg X−l and GX3+1 are the most prominent discrete X-ray objects in the sky at photon energies of ≃ 100 keV.
Proposed Observations of Astronomical Spectra at Hobart
Authors: Waterworth M. D.
Published: July 2016

The overall aim of the planned astronomical programme at Hobart (University of Tasmania) is to obtain stellar and planetary spectra in the ultra-violet, visible, and infrared regions of the spectrum. The major instruments to be used are a 16-inch telescope, a 40-inch telescope, and a solar spectrograph. Included in the project is a programme of laboratory studies, aimed at making quantitative comparisons of several of the most efficient methods for detecting and recording spectra from astronomical objects with low levels of flux. In addition, several new methods will be investigated. These will be referred to later in this paper.
Cosmic Rays and the Interstellar Medium
Authors: Fenton K. B.
Published: July 2016

Absorption limits the distances at which X-ray sources may be observed at low photon energies (≲3 keV). Several authors have estimated the X-ray absorption coefficients of the interstellar medium by assuming a chemical composition such as that given by Aller for the general abundances of the elements.
Circularly Polarized Synchrotron Radiation in Dipolar Magnetic Fields with Application to the Planet Jupiter
Authors: Gleeson L. J. , Legg M. P. C. , Westfold K. C.
Published: July 2016

This paper is a preliminary account of the calculation of the circularly polarized synchrotron radiation received from a distribution of electricallycharged particles confined to a thin shell in the magnetic field of a dipole. Calculations of the total radiation and the degree of linear polarization have previously been carried out, and these calculations are duplicated in part.
Recent Evidence Concerning the Sidereal Anisotropy in the Charged Primary Cosmic Radiation
Authors: Jacklyn K. G. , Vrana A.
Published: July 2016

Significant evidence for a bi-directional sidereal anisotropy has been obtained from observations with meson telescopes at depths in the vicinity of 40 metres water equivalent (m.w.e.) underground. The anisotropy is of the type which should occur when charged particles which were formerly isotropic stream equally in both directions along a magnetic field, if there is a tendency for pitch angles to become reduced (the pitch angle being the angle between the particle trajectory and the direction of the field). If the magnetic moments of the particles are adiabatically invariant, changes in the magnetic field, both with position and time, could be responsible for the anisotropy.
Pulsars and Cosmic Rays
Authors: Fenton A. G.
Published: July 2016

At present there are two general theories of the origin of cosmic rays. One is that most, if not all, galactic cosmic rays originate within the Galaxy, probably during supernova explosions. The other is that cosmic rays pervade the universe, originating mainly in the powerful radio galaxies and possibly in quasars, where vast stores of energy are available. The former theory has been discussed in detail by Ginzburg and Syrovatskii, while proponents of the latter theory include Burbidge and Hoyle, and Burbidge.
Techniques for Pulsar Observation
Authors: Ellis G. R. A.
Published: July 2016

Pulsar observations will be made with two new general-purpose transit radiotelescopes at present being built near Hobart.
80 MHz Observations of the Coronal Broadening of the Crab Nebula
Authors: Harries J. R. , Blesing R. G. , Dennison P. A.
Published: July 2016

Regions of the interplanetary medium currently inaccessible to space vehicles may conveniently be studied using the radio scattering properties of the interplanetary plasma. These effects may give rise to angular broadening of radio sources sufficiently close to the Sun, or to amplitude scintillation of sources of small angular size.
Radial Oscillations of Stellar Models: Density Distributions which Lead to Three-term Recurrence Relations
Authors: Murphy J. O. , Smith A. C.
Published: July 2016

In an early paper Sterne investigated the pulsational properties of three stellar models with specified density distributions. He assumed a solution for the relative amplitude of the displacement to be of the form

and on substitution into Eddington’s equation for small radial adiabatic oscillations of a star

obtained a two-term recurrence relation to solve for the an in the case of each model.
Theory of the Solar 22-Year Cycle
Authors: Piddington J. H.
Published: July 2016

If there were no solar magnetic fields, then the most active feature observable on the Sun would be the hydrodynamic convection. There would be no sunspots, flares, prominences, plage, spicules, and no copious emissions of X-rays, energetic particles or radio bursts. These effects are all due to the presence of a changing pattern of magnetic fields which repeats every 22 years. While observations of electromagnetic phenomena are limited to the solar surface and atmosphere, a full understanding of these effects must include a satisfactory theory of the solar cycle and of the fields which evolve beneath the surface as a result of plasma velocity fields.
Depth Dependence on the Various Scale Lengths in a Quasi-Vitense Model of the Solar Convection Zone
Authors: Waters B. E.
Published: July 2016

As has been previously stated (van der Borght) the lengths l1, l2, l3 and l4 are functions of and so a discussion of these lengths is in fact a discussion of the f’s. For a first approach to a determination of these f’s, a standard Vitense2 model of the convection zone—with mixing length l, is used. We assume that l = H. The variables we need are kz, which are the vertical wave number associated with the characteristic eddy, the average vertical velocity, and the average (non-dimensional) temperature fluctuation. These quantities are approximated, using the following relations
Interplanetary Scintillation Studies at the Molonglo Radio Observatory
Authors: Milne R. G.
Published: July 2016

The structure of small diameter radio sources can be investigated by studying the scintillation of the source due to the interplanetary medium when the line of sight approaches the Sun. Observations of radio source scintillation are currently being undertaken with the separate arms of the 1 mile radio telescope at the Molonglo Observatory. The EW arm allows successive transit observations with three fan beams, 1′.4 EW by 4°.2 NS at 408 MHz, bandwidth 2.5 MHz. Sources transit the half-power points of each beam in 6 sec δ seconds of time (δ is the source declination). The NS arm gives eleven fan beams at neighbouring declination, 1′.5 sec Z NS by 4° EW (Z is the zenith angle). Complete transit of a NS beam takes 15 sec δ minutes.
A Southern Hemisphere Radio Meteor Orbit Survey
Authors: Gartrell G.
Published: July 2016

A combined multi-station radar equipment of c.w. and pulse at 27 MHz was used at Adelaide (lat. 35°S) during the period December 1968 to June 1969 and again in October 1969 to measure radiants and velocities of individual meteors down to limiting radio magnitude MR = + 8. Reflections from 3 to 5 points typically separated by 2 to 6 km along each trail were used and corrections for the effects of meteor region winds and wind shears were included. To date 1667 orbits have been determined from 6 months of data.
The Temperature of the Solar Photosphere-Chromosphere Transition Region
Authors: Carver J. H. , Horton B. H. , Lockey G. W. A.
Published: July 2016

The region of the solar atmosphere where the brightness temperature is less than 9 x 103 K. defines the photosphere and low chromosphere. In physical scale this covers the range from 300 km. below to 2 x 103 km. above the visible surface.
Relative Positions of Fundamental and Second Harmonic Type III Bursts
Authors: Stewart R. T.
Published: July 2016

Observations of the relative positions of fundamental and second harmonic bursts can be used to study refraction and scattering effects in the corona. Smerd, Wild and Sheridan have pointed out that the observed positions of type II bursts can be interpreted as favouring the backward emission of the second harmonic in a smooth corona. In this case the harmonic is seen after reflection from near the fundamental plasma level. Several other examples of type II and type III bursts have been reported which show this effect. We wish to present further evidence from a recent study of a large number of type III bursts observed with the 80 MHz heliograph and 158 MHz interferometer.
Thermal Pulses in Helium Shell-Burning Stars
Authors: Faulkner D. J. , Wood P. R.
Published: July 2016

In recent years there have been numerous investigations of the helium shell-burning evolution of low-mass stars, and it was in such studies that Schwarzschild and Härm and Weigert independently discovered the thermal instability phenomenon. In the case of stars with hydrogen-rich envelopes, its reality has been amply confirmed. On the other hand, studies have also been made of the shell-burning in pure helium stars (many for comparison with the nuclei of planetary nebulae), and here the situation is far less clear. Some investigators have found the instability, while others have not. Paczyński has drawn attention to the fact that in all cases where thermal pulses have been reported for pure helium stars, the helium shell-source was treated as an abundance discontinuity, while in all cases where a detailed abundance profile was used, there was no evidence of pulses. He suggests therefore that the shells in pure helium stars are stable. We wish to report a calculation for a 0.8 ɱ⊙ pure helium star, with a detailed shell abundance profile, in which a single thermal pulse was encountered at the end of the shell-burning evolution.
The Variable Polarization of T Cen
Authors: Victoria Peterson A.
Published: July 2016

T Centauri (HD119090) is a semi-regular variable with a period of 90d.61. The period is apparently stable but the photometry does not repeat very closely from cycle to cycle. The general Catalogue of Variable Stars gives a range of magnitudes from 5.5 to 9.0 and spectral types from KOe to M4IIe.
The Design of an Infra-Red Interferometer
Authors: Harwood K.
Published: July 2016

Spectrometers give information on the chemical composition and physical properties of celestial objects. The Earth’s atmosphere restricts the observable spectra to windows in the absorption. Most of these windows are less than one octave wide. To increase the amount of information gained, it is necessary to increase the resolution of the spectrometers. With the advent of balloons, rockets and spacecraft, it is possible to make observations free from atmospheric absorption and it is possible to gain more information by increasing the bandwidth of spectrometers. This paper describes an infra-red Fourier transform spectrometer. The interferometer has a bandwidth of over one decade, from 500 to 5,000 cm-1, with a maximum resolution of 10 cm-1. The resolution can be electronically controlled. There are no absorbing or refracting parts in the interferometer and the resolution is limited by mechanical considerations.
Future Plans for the Molonglo Radio Telescope
Authors: Mills B. Y. , Little A. G.
Published: July 2016

The Molonglo cross-type radiotelescope has been in operation since 1967 and it is expected that its principal task, the fundamental sky survey, will be completed within the next few years. This by no means represents the end of the useful life of the instrument but we have been investigating modifications to extend further its usefulness. The most desirable modification appears to be a substantial increase in operating frequency to improve the resolution and positional accuracy.
Finite-Amplitude Convection under the Combined Effect of Rotation and a Magnetic Field
Authors: Murphy J. O. , Van der Borght R.
Published: July 2016

It is well known from linear theory that a magnetic field or rotation, acting separately, have an inhibiting effect on the onset of thermal convection. This has been confirmed by corresponding studies of finite amplitude convection. On the other hand, when both magnetic field and rotation act together, the linear theory predicts that they may have conflicting tendencies. It is the purpose of the present paper to report on the investigation of these effects in the case of non-linear thermal convection.
Dust Shell Models for Infrared Sources
Authors: Hyland A. R. , Gingold R. A.
Published: July 2016

Recent reviews have demonstrated that a wide ranging selection of objects emit a major proportion of their energy at wavelengths longer than 1 µm, including such intrinsically different objects as late type stars, Be stars, F supergiants and novae. In the majority of cases the infrared radiation has been interpreted in terms of thermal radiation from a circumstellar shell of solid ‘dust’ particles. Any attempt at a detailed comparison of theoretical energy distributions with observed infrared photometry encounters the problems of uncertainties in the absolute calibration, and limited accuracy of the observations.
Spiral Structure Viewed as a Density Wave
Authors: Kalnajs A. J.
Published: July 2016

One of the main reasons for pursuing a gravitational as opposed to a magnetic theory is that there exist galaxies which seem devoid of gas and yet show unmistakable structure. These galaxies are among those classified as SBO2/3 to SBa(r), and I shall, after Curtis, call them theta galaxies. Examples are: NGC 1512, 1291,4693, and 2859. The theta galaxies gradually merge into ringed bar galaxies, which in turn merge into ordinary spirals.
Reassessment of Suggested Frequency Dependent Positions for 4C Sources
Authors: Hoskins D. G. , Murdock H. S.
Published: July 2016

Frequency dependent structure is not uncommon in observations of extended radio sources. Where a source consists of two components with different spectra at an angular separation considerably less than the resolution of the telescope, the centroid position will vary systematically with frequency. A well-known example is 3C 273 though the effect in this case is quite small. With beams of a few minutes of arc, larger position differences could occur between measurements made at widely separated frequencies without the source being noticeably resolved. In a preliminary study of a sample of 120 4C radio sources, Munro and Hoskins found 17 cases of discrepancies in the range 45 to 100 seconds of arc between positions measured at 408 MHz with the Molonglo cross (beam width ~3′ arc) and at 2700 MHz with the Parkes 64 m telescope (beam width ~7′ arc) by Wills and Bolton. These separations were considered to be significant in terms of the quoted errors which were typically 10 to 15″ arc in each coordinate for both sets of measurements. It was pointed out that to explain the results on the basis of a double source model it would be necessary for the two components to differ in spectral index by ~1.
Computer Hardware and Software for On-line Pulsar Hunting
Authors: Rayner P. T. , Whitham P. S.
Published: July 2016

The optical astronomy group at the University of Tasmania is engaged in a search for optical pulsations from pulsars.

It was considered that the PDP-8/F mini-computer, purchased with A.R.G.C. funds to control the 40 inch telescope and on-line experiments, would be extremely useful for this purpose, until completion of the 40 inch telescope. Interfacing the computer to the output of the Cassegrain photo-electric photometer required work at both the hardware and software level.
Evolutionary Relation between Type I Storm Activity and the S-Component at Centimetre Wavelengths
Authors: Kai K. , Sekiguchi H.
Published: July 2016

Type I storms are the most frequently observed solar phenomena at metre and decimetre wavelengths. Since the first identification of the emission of this type with a large sunspot group a great many type I storms have been recorded with radio-spectrographs, polarimeters and interferometers (see, for example, Wild, Smerd and Weiss, Kundu, Wild). Nevertheless, we can offer no satisfactory answers to the most fundamental questions about type I storms: ‘What kind of disturbances supply energy to a localized coronal region to maintain the storm activity for up to several days?’; ‘What is the emission mechanism responsible for the peculiar features observed in type I storms?’.
A Moving Radio Burst on the Limb of the the Sun Observed at 80 and 160 MHz
Authors: McLean D. J.
Published: July 2016

On 1973 March 22 a radio event was observed above the east limb of the Sun with the Culgoora radioheliograph operating at both 80 and 160 MHz. The first stage of this event, a type I storm closely associated with a rising prominence, offers a new insight into the nature of this phenomenon. This storm was followed immediately by a moving type IV burst – the first burst of this kind for which two-dimensional observations are available at two frequencies. The relation between these two stages may help explain the ‘missing hour’ in observations of another moving type IV burst known as ‘Westward Ho’.
The Jupiter Radio Bursts
Authors: Ellis G. R. A.
Published: July 2016

Like the strong non-thermal radio bursts from the solar corona and from the earth’s magnetosphere, the Jupiter radio bursts are characterized by their duration which may be from milliseconds to seconds, and by their complex structure on the frequency-time plane. In addition, they exhibit a variety of periodicities in their rate of occurrence, the primary one of which is associated with the rotation of Jupiter. The smaller physical scale of Jupiter compared with the Sun naturally leads to a much shorter time scale in the various radio phenomena and it is only recently that suitable equipment has become available to permit the detailed investigation of the dynamic spectra of the bursts with the necessary high time resolution of the order of 10–3 sec (Ellis 1973a,b,c). As in the case of the solar radio bursts, a number of distinct types of dynamic spectra are observed and they provide a convenient basis for classification.
The Inverted Alt-Alt Configuration for Optical Telescopes
Authors: Simmonds E. W.
Published: July 2016

Introduction

My interest in the construction and costs of telescopes began with the design and construction of the building for the 48 inch Schmidt Telescope (on behalf of the Science Research Council of the United Kingdom) and was stimulated by a visit to Mt Palomar and Kitt Peak Observatories. With regard to costs I would like to quote Meinel (1969).
The 4830 MHz Formaldehyde Absorption in a Region of the Southern Coalsack
Authors: Brooks J. W. , Sinclair M. W. , Manefield Gwenyth A.
Published: July 2016

The detection of formaldehyde absorption of the microwave background radiation in a region of the Southern Coalsack (Sinclair and Brooks 1972) was made at about the same time as an optical study of this region (Tapia 1972) in which six globule-like clouds of interstellar dust were found. The size (0.3 pc) and position of the formaldehyde cloud were similar to the corresponding parameters of one of the globules (No. 2 on Tapia’s list).