The New Zealand Chinese gooseberry export industry and its future development : a thesis presented in partial fulfilment of the requirements for the degree of Master of Agricultural Science in Agricultural Economics at Massey University

New Zealand's dependence on the traditional exports, meat, wool, butter and cheese for the major overseas earners is well documented, (see (1)). New Zealand is one of the world's most efficient producers of these commodities but market access and short term political and social expediency has tended to reduce the gains of economic rationalization. During the last year (1971) butter and cheese have been placed in long term jeopardy due to Britain's impending union1 1. This is not an unexpected development. Britain first applied for membership in 1961 and was rejected in 1963 - negotation restarted in 1966 and entry will date from the 1/1/73. However, the provisions of the Common Agricultural Policy will not come into force until 1/1/74. with the European Economic Community. Wool suffered a serious price reversal in 1967 and although a price revival has occurred in the past year it is doubtful if this will be a long term recovery. Lamb exports to the U.K. are experiencing greater competition than ever from other meats, especially cheaply produced poultry. The beef quota for the U.S.A. cannot be considered safe as it depends to a large extent on seasonal production variations in the U.S.A. and the strength of the U.S.A. farm lobby. The existence of tariff and non-tariff barriers to trade, together with low price and income elasticities of demand for primary exports has placed emphasis on manufactured exports and import substitution in New Zealand, but many attempts at such diversification are often misdirected.2 2.An obvious example of this in New Zealand - The Automobile Industry. (see The World Bank Report on the New Zealand Economy 1968) though the farming industry has some protected sectors also. New Zealand has no absolute or comparative advantage in citrus production, hop production, wheat production - consequently all are protected by trade barriers in common with many other countries. Condliffe (5) has a cautionary note about this: "It is necessary to aim at competitive production for the world market rather than protected production for a small local market.

Teacher responses to a planning framework for junior technology classes learning outside the classroom

This paper describes teacher responses to a framework designed to support teacher planning for technology. It includes a learning experience outside the classroom [LEOTC] and is designed specifically for five-year-old students. The planning framework draws together characteristics of technology education, junior primary classrooms and LEOTC to describe the role of the teacher, parent helpers and students as they work through three identified phases - preparing for a visit outside the classroom, participating in a learning experience outside the classroom, and post-visit activities in the classroom. This framework was trialled using a case study approach in two new-entrant classrooms in which students made chocolates for Mother's Day as part of a technology unit. Students partook in a LEOTC visit to a chocolate factory in order to examine the practice of experts before designing and making their own chocolate gift. Data sources for this paper included interviews with two participating teachers. The analysis of these suggest the use of the planning framework led to the thorough preparation of parent helpers and students, clearly defined roles for both the teachers and the parents, and the use of valuable strategies which enhanced students memories of their visit enabled them to apply aspects of the knowledge gained to their own technological practice

The First Ten Years of Swift Supernovae

The Swift Gamma Ray Burst Explorer has proven to be an incredible platform for studying the multiwavelength properties of supernova explosions. In its first ten years, Swift has observed over three hundred supernovae. The ultraviolet observations reveal a complex diversity of behavior across supernova types and classes. Even amongst the standard candle type Ia supernovae, ultraviolet observations reveal distinct groups. When the UVOT data is combined with higher redshift optical data, the relative populations of these groups appear to change with redshift. Among core-collapse supernovae, Swift discovered the shock breakout of two supernovae and the Swift data show a diversity in the cooling phase of the shock breakout of supernovae discovered from the ground and promptly followed up with Swift. Swift observations have resulted in an incredible dataset of UV and X-ray data for comparison with high-redshift supernova observations and theoretical models. Swift's supernova program has the potential to dramatically improve our understanding of stellar life and death as well as the history of our universe.Comment: Invited review paper accepted into the Journal of High Energy Astrophysics for the dedicated issue: "Swift: Ten Years of Discovery" 8 pages, 4 figure

Spectroscopic Investigation of Some Metal VI Carbonyl Phosphine Complexes

Preparation of metal carbonyl phosphine complexes of type LM(C0)5 and trans L2(CO)4 M = Cr, Mo and W; L = P(OMe)3, P(OEt)3, P(OPri)3, PPri3 and PEun3 has been studied in a systematic way. Direct solventless reaction has been found applicable for preparation of the trans disubstituted derivatives, especially those of tungsten which are difficult to obtain in other ways. Chromatography was used for separation and purification of the complexes. The ultraviolet spectra of the phosphine complexes have been recorded both at room temperature and. low temperature. The low temperature spectra were obtained using a sample cooled by liquid nitrogen in a dewar. The observed change in the spectral outline on sample cooling has been successfully related to the forbidden/allowed character of the electronic transition involved. Using this experimental evidence, the spectra of the metal complexes have been partially assigned for the energies approximately 35,000 - 25,000 cm-1 where transition energies may represent either d-d or charge transfer type transitions and the extinction coefficients at room temperature have values intermediate between accepted d-d and charge transfer values. Thus the lowest energy charge transfer transition has been assigned for thirty complexes, in only three of which it has been previously reported and these on the basis of spectra recorded at room temperature only. Some representative examples of the ultraviolet spectra having several overlapped, partially resolved bands were analysed using a combination of Gaussian curves, This technique has become more popular recently and has been applied to complex spectra of derivatives of the type studied here. The spectral outlines were not all suitable for curve analysis since in cases where the degree of overlap is very high, it is not possible to make a plausible assessment of the number of peaks involved, this information being essential for the analysis. Comparative critical studies have been carried out on the Gaussian analyses obtained, taking account of the subjective factors of the operator's decisions concerning the number of peaks and their relative intensities. This has been used in assessing both the validity and usefulness of the peak information revealed by such analyses. Nuclear magnetic resonance spectra of the complexes have been recorded for proton and carbon-13 resonance. The proton spectra of the trans disubstituted phosphite derivatives have been related to the phenomenon of virtual coupling which is seen for protons on the alpha-carbon of the ligand substituent only. Analogous phosphine derivatives are seen to have second order splitting patterns which would require further analysis, probably by computer simulation, to be discussed in relation to the phosphite spectra. The carbon-13 spectral parameters are reported for these complexes for the first time. Chemical shifts of the carbon in the carbonyl groups and in the ligands along with coupling constants for phosphorus-carbon and tungsten-carbon coupling are given. Their discussion is limited by the undeveloped nature of chemical shift and coupling theory as they apply to carbon-13 magnetic resonance. The Mass spectra of a limited number of the complexes are reported and a short discussion of the possible fragmentation patterns is given. These patterns are derived by analogy with previously reported patterns of similar complexes. The spectra of two monosubstituted complexes are compared with those of the corresponding trans disubstituted derivatives and the differences in relative intensities and m/e fragments observed are discussed. Infrared spectra of the complexes have been recorded in the stretching carbonyl region on solutions of very high concentration and formally forbidden peaks have been observed and assigned for mono-and trans disubstituted phosphite derivatives while only for the monosubstituted phosphine derivatives have such peaks been assigned. The deltaMCO and nuMC absorptions have been recorded although, as in previous studies, fewer peaks are observed than are required by group theory. Metal phosphorus bonding is discussed taking account of the U.V., I.R. and N.M.R. studies reported here along with recent developments in relevant molecular orbital theory and other reported results concerning bonding in similar complexes. An assessment has been made of the value of relating spectroscopic results directly to variations in the metal-ligand bonds, especially the metal-phosphorus bond. A short appendix deals with preparation of trifluorophosphine derivatives of M2(CO)10M =Mn, Re

Radio Emission from the Composite Supernova Remnant G326.3-1.8 (MSH15-56)

High resolution radio observations of the composite supernova remnant (SNR) G326.3-1.8 or MSH 15-56 with the Australia Telescope Compact Array show details of both the shell and the bright plerion which is offset about 1/3 of the distance from the center of the SNR to the shell. The shell appears to be composed of thin filaments, typical of older shell SNRs. The central part of the elongated plerion is composed of a bundle of parallel ridges which bulge out at the ends and form a distinct ring structure on the northwestern end. The magnetic field with a strength of order 45 microGauss, is directed along the axis of the ridges but circles around the northwestern ring. This plerion is large and bright in the radio but is not detected in x-ray or optical wavelengths. There is, however, a faint hard x-ray feature closer to the shell outside the plerion. Perhaps if the supernova explosion left a rapidly moving magnetar with large energy input but initially rapid decay of both relativistic particles and magnetic field, the observed differences with wavelength could be explained.Comment: 15 pages, 10 figures, accepted by Ap

Evaluation of approaches to control of Maedi-Visna disease of sheep using a Markov chain simulation model for a range of typical British Flocks

An epidemiological model is described that closely mimicked results of a published serological study of natural transmission of Maedi-Visna virus in a low ground flock of sheep. We adjusted parameters in the model from this baseline to explore the possible implications for the control of Maedi-Visna virus in typical British flocks. On closed hill farms, low probability of effective contact was most critical for control. In open low ground flocks, purchasing accredited replacements eliminated disease spread, otherwise flock size was the most important factor governing flock prevalence. Results highlighted the need for more epidemiological information about Maedi-Visna, particularly whether hill farms act as a hidden reservoir of virus or reduce the impact of this disease on the industry by providing a source of clean replacementsLivestock Production/Industries, Maedi-Visna, Model, Markov Chain, Sheep, Control,

Theoretical Clues to the Ultraviolet Diversity of Type Ia Supernovae

The effect of metallicity on the observed light of Type Ia supernovae (SNe Ia) could lead to systematic errors as the absolute magnitudes of local and distant SNe Ia are compared to measure luminosity distances and determine cosmological parameters. The UV light may be especially sensitive to metallicity, though different modeling methods disagree as to the magnitude, wavelength dependence, and even the sign of the effect. The outer density structure, ^56 Ni, and to a lesser degree asphericity, also impact the UV. We compute synthetic photometry of various metallicity-dependent models and compare to UV/optical photometry from the Swift Ultra-Violet/Optical Telescope. We find that the scatter in the mid-UV to near-UV colors is larger than predicted by changes in metallicity alone and is not consistent with reddening. We demonstrate that a recently employed method to determine relative abundances using UV spectra can be done using UVOT photometry, but we warn that accurate results require an accurate model of the cause of the variations. The abundance of UV photometry now available should provide constraints on models that typically rely on UV spectroscopy for constraining metallicity, density, and other parameters. Nevertheless, UV spectroscopy for a variety of SN explosions is still needed to guide the creation of accurate models. A better understanding of the influences affecting the UV is important for using SNe Ia as cosmological probes, as the UV light may test whether SNe Ia are significantly affected by evolutionary effects.Comment: 10 pages. Submitted to Ap

Grouping Normal Type Ia Supernovae by UV to Optical Color Differences

Observations of many SNe Ia with the UVOT instrument on the Swift satellite has revealed that there exists order to the differences in the UV-OPT colors of normal SNe. We examine UV-OPT color curves for 25 SNe Ia, dividing them into 4 groups, finding that ~1/3 of these SNe Ia have bluer UV-OPT colors than the larger group, with these "NUV-blue" SNe Ia 0.4 mag bluer than the "NUV-red" SNe Ia in u-v. Another group of events feature colors similar to NUV-red SNe Ia in the u-v to uvw1-v colors, but similar to the NUV-blue SNe Ia in the uvm2-v color. We name these events "MUV-blue". The last group initially has colors similar to NUV-red SNe Ia, but with color curves that feature more modest changes than the larger NUV-red group. These "irregular" events are comprised of all the NUV-red events with the broadest optical peaks, which leads us to consider this minor group a subset of the NUV-red group. When so separated and the accounting is made for the rapid time evolution of the UV-OPT colors, we find that the scatter in two NUV-OPT colors, u-v & uvw1-v, is at the level of the scatter in b-v. This finding is promising for extending the cosmological utilization of SNe Ia into the NUV. We generate spectrophotometry of SNe Ia that have been observed with HST and argue that there is a fundamental spectral difference in the 2900-3500A wavelength range, a range suggested to be dominated by absorption from iron-peak elements. The NUV-blue SNe Ia feature less NUV absorption than the NUV-red SNe Ia. We show that all the NUV-blue SNe Ia in this sample have also featured evidence of unburned carbon in optical spectra, whereas only one NUV-red SN Ia features that absorption line. Every NUV-blue event also exhibits a low gradient of the SiII 6355A absorption feature, but many NUV-red events also exhibit a low gradient, perhaps suggestive that NUV-blue events are a subset of the larger LVG group.Comment: Accepted to the Astrophysical Journal Updated version: Sept 16, 201