Sustainable shellfish aquaculture in Saldanha Bay,South Africa

The carrying capacity for bivalve shellfish culture in Saldanha Bay, South Africa, was analysed through the application of the well-tested EcoWin ecological model, in order to simulate key ecosystem variables. The model was set up using: (i) oceanographic and water-quality data collected from Saldanha Bay, and (ii) culture-practice information provided by local shellfish farmers. EcoWin successfully reproduced key ecological processes, simulating an annual mean phytoplankton biomass of 7.5 µg Chl a l^–1 and an annual harvested shellfish biomass of about 3 000 tonnes (t) y^–1, in good agreement with reported yield. The maximum annual carrying capacity of Small Bay was estimated as 20 000 t live weight (LW) of oysters Crassostrea gigas, or alternatively 5 100 t LW of mussels Mytilus galloprovincialis, and for Big Bay as 100 000 t LW of oysters. Two production scenarios were investigated for Small Bay: a production of 4 000 t LW y^–1 of mussels, and the most profitable scenario for oysters of 19 700 t LW y^–1. The main conclusions of this work are: (i) in 2015–2016, both Small Bay and Big Bay were below their maximum production capacity; (ii) the current production of shellfish potentially removes 85% of the human nitrogen inputs; (iii) a maximum-production scenario in both Big Bay and Small Bay would result in phytoplankton depletion in the farmed area; (iv) increasing the production intensity in Big Bay would probably impact the existing cultures in Small Bay; and (v) the production in Small Bay could be increased, resulting in higher income for farmers.     

Landscape-scale analysis of ecosystem risk and returns: A new tool for ICZM

Management of the coastal zone often focuses on “islands” of high value ecosystems, in terms of economic value or conservation. However, integrated management requires landscape-level analysis of all ecosystem values. The biodiversity portfolio analysis (BPA) method is derived from the logic used in share (equity) portfolio management in terms of balancing within a portfolio the returns with the risks. Optimising the returns from a share portfolio, or a suite of ecosystems in a landscape, is dependent on the relationship between the units in terms of risk and return. Three case studies are then presented to test the applicability of the BPA method at the international (North West Europe), regional (Durham Heritage Coast, UK) and local (part of South Uist, Outer Hebrides, UK) spatial scale. The Biodiversity Portfolio Analysis for NW Europe showed that risk and return were highly correlated in the studied Member States. The ranking of risk and return, with the highest first, was Ireland > UK > France=Netherlands > Belgium. For these Member States the risks to ecosystem service provision were positively correlated with GNI (r=0.97, P<0.01); suggesting that the higher the economic importance of coastal and marine resources in a Member State the more at risk the resources are. The regional and local case studies were more focussed on providing information on which to base Integrated Coastal Zone Management (ICZM) decision making; both case studies used stakeholder participation to determine risks and returns. The conclusions from these two case studies show how the BPA method can be useful in terms of setting ICZM priorities and in addressing local coastal issues. The BPA involves making a number of assumptions, however, it does provide coastal managers with a potential tool to strategically plan due to increased awareness of the interaction between the ecosystems in the portfolio.There is a need for such techniques, which involve stakeholder participation and which create objective outcomes, to support the implementation of ICZM.     

Geochronology of Precambrian rocks in the Laramie Range and implications for the tectonic framework of Precambrian southern Wyoming

From Casper Mountain; at its northern end, to the northwestern margin of the Laramie anorthosite—syenite complex, in its central parts, the Laramie Range is underlain by granite and granitic gneiss that has a minimum age of 2.54 ± 0.04 Ga (Rb/Sr whole-rock isochron) and by metasedimentary rocks, including marble and quartzite, that appear to overlie the granitic gneiss nonconformably (minimum age: 1.7 Ga based on several horn-blende K/Ar dates). Southward from the anorthosite—syenite complex into Colorado, the Range is underlain chiefly by the Sherman Granite (1.41 Ga; Peterman and Hedge, 1968) and scattered patches of gneiss that are not dated, but are tentatively correlated wit similar gneiss in the southern Medicine Bow Mountains and in the Colorado Front Range, where they are dated as ? 1.7 Ga (Peterman and Hedge, 1968).The Laramie anorthosite—syenite complex (minimum age: ? 1.42 Ga or ? 1.51 Ga if a hornblende K/Ar date is accepted) apparently intruded the suture separating the old (? 2.5 Ga) continental edge from younger (? 1.7 Ga) geosynclinal rocks. The suture, which manifests itself as the Mullen Creek—Nash Fork shear zone in the Medicine Bow Mountains, also is the boundary between ensialic and ensimatic geosynclinal deposition that occurred during the interval 1.7–2.5 Ga ago.K/Ar dates on biotite and muscovite from rocks north of the anorthosite—syenite complex grade from 2.5 Ga on Casper Mountain down to 1.38 Ga near the complex. Near its northern tip, the Laramie Range is crossed by a geochronologic front, separating 2.5 Ga old gneiss whose K/Ar dates were not lowered by subsequent metamorphism from 2.5 Ga old gneiss whose mica dates were reset between 1.4 and 1.6 Ga ago.     

The effect of UV stars on the intergalactic medium

We have investigated the effect of ionizing radiation from the UV stars (hot prewhite dwarfs) on the intergalactic medium (IGM). If the UV stars are powered only by gravitational contraction they radiate most of their energy at a typical surface temperature of 1.5×10⁵ K which produces a very highly ionized IGM in which the elements carbon, nitrogen and oxygen are left with only one or two electrons. This results in these elements being very inefficient coolants. The gas is cooled principally by free-free emission and the collisional ionization of hydrogen and helium. For a typical UV star temperature ofT=1.5×10⁵ K, the temperature of the ionized gas in the IGM isT _g =1.2×10⁵ K for a Hubble constantH _o=75 km s^–1 Mpc^–1 and a hydrogen densityn _H =10^–6 cm^–3. Heating by cosmic rays and X-rays is insignificant in the IGM except perhaps inHi clouds because when a hydrogen atom recombines in the IGM it is far more likely to be re-ionized by a UV-star photon than by of the other two types of particles due to the greater space density of UV-star photons and their appreciably larger ionization cross-sections. If the UV stars radiate a substantial fraction of their energy in a helium-burning stage in which they have surface temperatures of about 5×10⁴ K, the temperature of the IGM could be lowered to about 5×10⁴ K.     

Submillimetre continuum observations of pre-protostellar cores

Results are outlined of a JCMT submillimetre continuum survey of Myers cores that have no known infrared associations - the so-called starless cores. Detailed parameters are calculated, such as temperature, mass, luminosity and radial density dependence. On the basis of lifetime and luminosity arguments, the cores are found to be pre-protostellar in nature, undergoing the ambipolar diffusion phase prior to protostellar collapse. The cores do not follow the r^–2 density dependence predicted by the standard model, but are consistent with a recent model of magnetic support of cloud cores.     

Practitioner training for building capacity in ICZM

Capacity building has been a much promoted principle of Integrated Coastal Zone Management (ICZM) since its advent beginning in the 1970’s. Although the concept of capacity building includes human resource development, organizational development and institutional and legal framework development, in practice it has often become focussed on the transfer of technical knowledge and procedures to managers and decision makers. The effect of this is often to emphasise and promote sectoral approaches rather than a holistic one as advocated by ICZM. Experiences gained during the EU Intereg IIIB COREPOINT project led to the development of a training programme that progressively reduced its formal lecture-style content and increased opportunity for discussion and delegate participation. It also produced a more uniform and systematic style and structure to presentations, in particular the case studies illustrating the eight EU ICZM principles of best practice, and embedded the ICZM principles and European perspectives of coastal management within the context of the work environment.This paper reviews methods for practitioner-oriented capacity building, and details the evolution of a training course to sensitise and familiarise coastal practitioners with the principles and practices of ICZM, working from local to national to trans-national scales. The lessons learnt from the ICZM capacity development in COREPOINT are identified and it is suggested that these are relevant and applicable to many other ICZM initiatives.     

Pitchblende and galena ages in the Alligator Rivers region,Northern Territory,Australia

U-Pb and Pb isotopic studies have been made of pitchblendes and associated galenas from four major deposits in the Alligator Rivers region of the Northern Territory, Australia. These are compared with previously-published data on deposits in the South Alligator Valley and in the Westmoreland area on the Queensland border. In all, four different times of possible mineral formation have been detected (1880 ± m. y., 1700 ± m. y., 800–900 m. y., 400–500 m. y.) Some deposits reveal only one time, others two; no deposit shows evidence for all four. The associated galenas are in general highly radiogenic (206/204 ratios range from 2000 to 29, 000); some can be interpreted as reflecting development in two completely different generations of pitchblende. The clearest evidence for solid-state formation of galena from presently-existing pitchblende is to be found at Nabarlek, where the major time of pitchblende formation (920 m. y.) bears no relationship to any known Rb-Sr or K-Ar age.     

On the process of accretion in the formation of the planets and comets

The physically reasonable assumption that the seed bodies which initiated the accretion of the individual asteroids, planets, and comets (subsequently these objects are collectively called planetoids) formed by stochastic processes requires a radius distribution function which is unique except for two scaling parameters: the total number of planetoids and their most probable radius. The former depends on the ease of formation of the seed bodies while the second is uniquely determined by the average pre-encounter velocity, V, of the accretable material relative to an individual planetoid. This theoretical radius function can be fit to the initial asteroid radius distribution which Anders (1965) derived from the present-day distribution by allowing for fragmentation collisions among the asteroids since their formation. Normalizing the theoretical function to this empirical distribution reveals that there were about 10² precollision asteroids and that V = (2?4) × 10^?2 km/sec which was presumably the turbulent velocity in the Solar Nebula. Knowing V we can determine the scale height of the dust in the Solar Nebula and consequently its space density. The density of accretable material determines the rate of accretion of the planetoids. From this we find, for example, that the Earth formed in about 8 × 10⁶ yr and it attained a maximum temperature through accretion of about 3 × 10³°K. From the total mass of the terrestrial planets and the theoretical radius function we find that about 2 × 10³ planetoids formed in the vicinity of the terrestrial planets. Except for the asteroids the smaller planetoids have since been accreted by the terrestrial planets. About 15% of the present mass of the terrestrial planets was accumulated by the secondary accretion of these smaller primary planetoids. There are far fewer primary planetoids than craters on the Moon or Mars. The craters were likely produced by the collisional breakup of a few primary planetoids with masses between one-tenth and one lunar mass. This deduction comes from comparing the collision cross sections of the planetoids in this mass range to that of the terrestrial planets. This comparison shows that two to three collisions leading to the breakup of four to six objects likely occurred among these objects before their accretion by the terrestrial planets. The number of these fragments is quite adequate to explain the lunar and Martin craters. Furthermore the mass spectrum of such fragments is a power-law distribution which results in a power-law distribution of crater radii of just the type observed on the Moon and Mars. Applying the same analysis to the planetoids which formed in the vicinity of the giant planets reveals that it is unlikely that any fragmentation collisions took place among them before they were accreted by these planets due to the integrated collision cross section of the giant planets being about three orders of magnitude greater than that of the terrestrial planets. We can thus anticipate a marked scarcity of impact craters on the satellites of these outer planets. This prediction can be tested by future space probes. Our knowledge of the radius function of the comets is consistent with their being primary planetoids. The primary difference between the radius function of the planetoids which formed in the inner part of the solar system and that of the comets results from the fact that the seed bodies which grew into the comets formed far more easily than those which grew into the asteroids and the terrestrial planets. Thus in the outer part of the Solar Nebula the principal solid material (water and ammonia snow) accreted into a huge (～10¹²⁺) number of relatively small objects (comets) while in the inner part of the nebula the solid material (hard-to-stick refractory substances) accumulated into only a few (～10³) large objects (asteroids and terrestrial planets). Uranus and Neptune presumably formed by the secondary accretion of the comets.     

The role of biodegradation and photo-oxidation in the transformation of terrigenous organic matter

Microbial and photochemical decomposition are two major processes regulating organic matter (OM) transformation in the global carbon cycle. However, photo-oxidation is not as well understood as biodegradation in terms of its impact on OM alteration in terrigenous environments. We examined microbial and photochemical transformation of OM and lignin derived phenols in two plant litters (corn leaves and pine needles). Plant litter was incubated in the laboratory over 3 months and compositional changes to OM were measured using nuclear magnetic resonance (NMR) and gas chromatography-mass spectrometry. We also examined the susceptibility of soil organic matter (SOM) to ultraviolet (UV) radiation. Solid-state ¹³C NMR spectra showed that O-alkyl type structures (mainly from carbohydrates) decreased during biodegradation and the loss of small carbohydrates and aliphatic molecules was observed by solution-state ¹H NMR spectra of water extractable OM from biodegraded litters. Photochemical products were detected in the aliphatic regions of NaOH extracts from both litter samples by solution-state ¹H NMR. Photo-oxidation also increased the solubility of SOM, which was attributed to the enhanced oxidation of lignin derived phenols and photochemical degradation of macromolecular SOM species (as observed by diffusion edited ¹H NMR). Overall, our data collectively suggests that while biodegradation predominates in litter decomposition, photo-oxidation alters litter OM chemistry and plays a role in destabilizing SOM in soils exposed to UV radiation.