Detection of acoustic class boundaries in soft sediment systems using the seafloor acoustic discrimination system QTC VIEW

Transition zones (or ‘ecotones’) are ecologically important spatial elements of subtidal landscapes that represent a mixture of different habitat elements. We provide a method for identifying such areas in broad-scale surveys of the seafloor using the acoustic discrimination system QTC VIEW. QTC VIEW is an acoustic processing system that assigns sonar ping stacks to clusters of like points, to identify different habitats on the seafloor. Paired QTC VIEW transects (20 m spacing) were run at intervals of 200 m, at two separate sampling locations, to assess the consistency of clustering of individual ping stacks into acoustic classes. Very consistent spatial patterns of class change were found between transect pairs, suggesting high stability in the classification process. QTC VIEW assigns confidence values to each individual record; running averages calculated using a moving window along transects showed drops in confidence values associated with areas of transition in habitat class assignment, but this was not always consistent. The Berger–Parker index, a class dominance statistic, provided a more consistent transition indicator. Class transition ranged from abrupt to gradual, along with areas where a mixture of acoustic classes occurred. However, acoustically detected transition zones did not consistently respond to visual observations of the sea floor.     

Comparative advantage and distant water fishing fleets: The Australian east coast tuna longline fishery

A coastal state benefits from importing the services of a distant water fishing nation (DWFN) fleet if the DWFN has a comparative advantage in exploiting the fishery, based on factors such as market access, costs or technology. The paper compares the activities of the Australian and Japanese vessels in the east coast tuna longline fishery and finds the Australian vessels receive higher prices, have higher costs and use a different technology from the Japanese fleet. These differences suggest a pattern of comparative advantage which can lead to Australia benefitting from importing the services of the Japanese fleet.     

Characteristics of the optical volume scattering function of sea water

The volume scattering function, σ(?), was observed for unpolarized green light near 5300 Å in a variety of water bodies over a wide range of scattering angle, ?. These data, includingin situ values measured to an extreme foward angle of 0.2^o, permit a statistical study of parameters describing the shape of the σ(?) curve and provide detailed information on small angle contributions to forward scattering. The angular limit, θ_1/2, which determines one-half the total scattering coefficient upon integration of σ(?) over small angles, is determined from measured data and ranges between about 2^o for clear ocean water and about 5^o for turbid coastal water. Use of σ(?), measured at a single fixed angle, is investigated further as an indicator of the total scattering coefficient, and results of other studies showing a high correlation between the total scattering coefficient and σ(45^o) are further substantiated.     

Four-color photometry of the Galilean satellites

Photometry obtained in 1973 on the uvby system yields high-precision rotational light curves for Io, Europa, and Ganymede at a mean phase angle of ～6°. By combining our observations with photometry obtained by others over a broader range of phase angle, we alsi derive improved values for the phase coefficients and opposition surges of the four Galilean satellites. The values of V(1, 0) obtained by linear extrapolation to zero phase are accurate to ±0.03 magnitudes. We also derive the colors of the sun of the uvby system and use these to obtain albedos of the satellites in four colors.     

The two faces of Iapetus

Combined photometry and radiometry of Iapetus can be used to investigate the nature of its surface and, in particular, the distribution of albedo that is responsible for the large variations in its visible and infrared brightness as it rotates. We present new 20-μm radiometric observations made in 1971–1973 and discuss these together with the photometric studies by Widorn (in 1949), Mills (in 1971), Noland et al. (in 1972–1973), and Franklin and Cook (in 1972–1974). The linear phase coefficient varies as the satellite rotates from 0.028 to 0.068 mag deg^?1. When corrected for this effect, the photometric variations suggest an albedo distribution characterized by a dark area covering most of the leading hemisphere and a bright trailing hemisphere and bright south polar cap. A combined analysis of the photometry and radiometry yields a radius of 800 to 850 km and mean geometric albedos for the light and dark faces of about 0.35 and 0.07, respectively. The average phase integral of the bright hemisphere is between 1.0 and 1.5. We offer no explanation for the unique photometric properties of this satellite.     

Io: Observational constraints on internal energy and thermophysics of the surface

Infrared observations of the Io eclipse of 12 April 1980 in five broad bands from 3 to 30 μm define the thermal emission spectrum both during and after eclipse. A substantial fraction of the emitted radiation during eclipse arises from hot spots; the equivalent global average heat flow is 1.5 ± 0.3 W m^?2, corresponding to an internal source of (6 ± 1) × 10¹³ W. The hot spot spectra can be matched by components with color temperatures of 200–600°K covering 1–2% of the surface. Comparison with observations over the past 8 years suggests that, while the flux at the hottest temperatures may be highly variable, there is no evidence for major changes in the total heat flow, which is emitted primarily in the spectral region 10–20 μm. The heating curves of the surface were observed at 10 and 20 μm; when corrected for the hot spot contribution they indicate a typical global thermal inertia for Io of $\text{(0.2 ± 0.1) × 10}{}^{\mathrm{?3}}\text{cal cm}{}^{\mathrm{?2}}\text{sec}\text{?}{}^{\mathrm{<mtext>1</mtext><mtext>2</mtext>}}\text{K}{}^{\mathrm{?1}}$, similar to that of the other Galilean satellites.     

Deregulation of the New Zealand labour market

The neo-classical rationale for deregulation of the labour market argues that capital and labour should have greater choice in their relationship with each other, in particular employers should have greater flexibility to affect wages and conditions in accord with specific product markets and local conditions. Decentralised decision making, it is argued, will lead to greater market efficiency than a centrally controlled system of employment relations and wage setting. Such was the rationale for the Employment Contracts Act (ECA) in 1991. Although it did even out the relative power granted to capital and labour the Employment Relations Act (ERA) introduced a decade later preserved the general thrust of the 1991 legislation. The ECA completed the dismantling of centralised regulation of employment relationships in New Zealand. But over ten years later there is still no clear consensus on its labour market impact. The immediate effects of the legislation on unionisation and levels of work stoppages are relatively easy to document. However, outcomes related to the functioning of the labour market as a whole – unemployment rates, labour force participation rates, wage levels, labour productivity and on-the-job-training – have proved far more difficult to tie directly or even indirectly to the ECA. It is argued here that the impact of the ECA on efficiency and growth has been extremely modest and that any net improvement in conventional labour market measures has been negligible. Rather the Act has been more influential in redistributing available paid work, including the redistribution of a greater share of the surplus from labour to capital itself. Any categorical conclusions on the impacts of the ECA and the ERA require a far more carefully specified research design than has been applied to date. This revised version was published online in July 2006 with corrections to the Cover Date.     

The E asteroids and the origin of the enstatite achondrites

Color, polarization and albedo data are summarized for the three known minor planets of optical type E— 44 Nysa, 64 Angelina and 434 Hungaria. The inventory of E asteroids with dimensions > 50 km is shown to be essentially complete.The surfaces of the E objects evidently consist of colorless, translucent, iron-free silicates such as plagioclase, forstefite, or enstatite. Their possible identification as the source of enstatite achondrites is consistent with new laboratory polarimetry of the Norton County aubrite. Both Nysa and Hungaria seem to be rather favorably situated for the production of meteorites.Nysa has a highly non-spherical shape, and is dynamically associated with the metal-rich asteroid 135 Hertha and several small objects also apparently of the metal-depleted E type. The configuration is suggestive of the fragments of a differentiated parent body, in which Hertha originated as the iron core and Nysa as the largest surviving mantle fragment. The relative volumes, however, are not consistent with simple igneous differentiation from a chondritic composition.