The Global Programme of Action for the Protection of the Marine Environment from Land-based Activities (GPA) represents an ambitious attempt to make the leap between the rhetoric of protecting and preserving the marine environment and action. With degradation of the marine environment from land based activities posing one of the most serious threats to the quality and productivity of the coastal and marine environment, the GPA can only be viewed as a milestone rather than a destination, as so much work remains to be done in this field.States supporting the GPA are entering the most challenging phase of the program, that of implementation. But the international community in taking on this challenge is not without a few signposts. The failure of the Montreal Guidelines to be implemented, provides States with many important lessons. This paper suggests that if the GPA is to have an impact on the complex problem of land-based activities then several tasks need to be grappled with. Substantial financial support needs to be generated, a proactive and cooperative secretariat established and the nexus between the GPA and United Nations Environment Programme Regional Seas Programme examined. The importance of people and training to the capacity building process needs to be recognised and a wider variety of stakeholders engaged in the follow up phase. Pivotal to the aforementioned is the need to generate political will to address the problem, without which the GPA will become yet another dusty volume on the bookshelf. 相似文献
Based on the analysis of newly collected data of plate tectonics, distribution of active faults and crustal deformation, the Taiwan area is divided into two seismic regions and six seismic belts. Then, correlation fractal dimensions of all the regions and belts are calculated, and the fractal characteristics of hypocenteral distribution can be quantitatively analyzed. Finally, multifractal dimensions Dq and f(α) are calculated by using the earthquake catalog of the past 11 years in the Taiwan area. This study indicates that (1) there exists a favorable corresponding relationship between spatial images of seismic activity described with correlation fractal dimension analysis and tectonic settings; (2) the temporal structure of earthquakes is not single but multifractal fractal, and the pattern of Dq variation with time is a good indicator for predicting strong earthquake events. 相似文献
Canteen Kopje, situated in the Northern Cape Province of South Africa, has two main archaeological deposits: alluvial gravels and a mantle of overlying fine sediments known locally as the “Hutton Sands.” This paper focuses on the fine sediments, the three industries contained within them, and the interface with the underlying gravels in an attempt to clarify their formation and transformation. A Fauresmith assemblage is found at this interface; it is thus crucial to understand the processes of deposition and modification at this poorly understood boundary. The methods used in this study involved the analysis of artifact depositional (dip and orientation) and spatial data, artifact condition, raw materials, and assemblage size profiles. Data presented document the mixing between the lowest levels of the fine sediments and the underlying alluvial gravels. This study thus provides important contextual information for the Fauresmith industry at Canteen Kopje. 相似文献
Historically, carbonate spots have been identified as an indicator of gold mineralization throughout central Victoria, Australia.
However, the exact timing relationships between the growth of carbonates, development of deformation fabrics, and the introduction
of gold has only been determined in more recent times through isolated studies on individual gold deposits. Detailed examination
of the evolution of hydrothermal alteration associated with the Magdala gold deposit at Stawell recognized the fact that there
were at least two generations of carbonate growth, an early rounded ankerite phase that predated gold mineralization and a
later euhedral siderite phase coincident with gold mineralization. This pattern of carbonate growth is repeated in the majority
of significant gold deposits, including Bendigo and Ballarat, throughout central Victoria. Timing relationships within the
carbonates suggest that a fluid was introduced along bedding planes and early deformation fabrics prior to the main upright
folding events that significantly modified the original sedimentary basin. It is suggested that the early rounded carbonates
may have formed as a result of anaerobic oxidation of methane, derived from the sediments and advected along normal growth
faults within the sedimentary basin, through interaction with downward diffusing seawater sulfate. Although the growth of
the early carbonates is not related to gold mineralization, the change in the speciation of the carbonate during the later
carbonate event is critical and can be tracked using a simple geochemical index that can be used not only in areas of outcrop
but also in conjunction with exploration undercover. 相似文献
The Visual and Infrared Mapping Spectrometer (VIMS) instrument on the Cassini Saturn Orbiter returned spectral imaging data as the spacecraft undertook six close encounters with Titan beginning 7 July, 2004. Three of these flybys each produced overlapping coverage of two distinct regions of Titan's surface. Twenty-four points were selected on approximately opposite hemispheres to serve as photometric controls. Six points were selected in each of four reflectance classes. On one hemisphere each control point was observed at three distinct phase angles. From the derived phase coefficients, preliminary normal reflectances were derived for each reflectance class. The normal reflectance of Titan's surface units at 2.0178 μm ranged from 0.079 to 0.185 for the most absorbing to the most reflective units assuming no contribution from absorbing haze. When a modest haze contribution of τ=0.1 is considered these numbers increase to 0.089–0.215. We find that the lowest three reflectance classes have comparable normal reflectance on either hemisphere. However, for the highest brightness class the normal reflectance is higher on the hemisphere encompassing longitude 14–65° compared to the same high brightness class for the hemisphere encompassing 122–156° longitude. We conclude that an albedo dichotomy observed in continental sized units on Titan is due not only to one unit having more areal coverage of reflective material than the other but the material on the brighter unit is intrinsically more reflective than the most reflective material on the other unit. This suggests that surface renewal processes are more widespread on Titan's more reflective units than on its less reflective units.
We note that one of our photometric control points has increased in reflectance by 12% relative to the surrounding terrain from July of 2004 to April and May of 2005. Possible causes of this effect include atmospheric processes such as ground fog or orographic clouds; the suggestion of active volcanism cannot be ruled out.
Several interesting circular features which resembled impact craters were identified on Titan's surface at the time of the initial Titan flyby in July of 2004. We traced photometric profiles through two of these candidate craters and attempted to fit these profiles to the photometric properties expected from model depressions. We find that the best-fit attempt to model these features as craters requires that they be unrealistically deep, approximately 70 km deep. We conclude that despite their appearance, these circular features are not craters, however, the possibility that they are palimpsests cannot be ruled out.
We used two methods to test for the presence of vast expanses of liquids on Titan's surface that had been suggested to resemble oceans. Specular reflection of sunlight would be indicative of widespread liquids on the surface; we found no evidence of this. A large liquid body should also show uniformity in photometric profile; we found the profiles to be highly variable. The lack of specular reflection and the high photometric variability in the profiles across candidate oceans is inconsistent with the presence of vast expanses of flat-lying liquids on Titan's surface. While liquid accumulation may be present as small, sub-pixel-sized bodies, or in areas of the surface which still remain to be observed by VIMS, the presence of large ocean-sized accumulations of liquids can be ruled out.
The Cassini orbital tour offers the opportunity for VIMS to image the same parts of Titan's surface repeatedly at many different illumination and observation geometries. This creates the possibility of understanding the properties of Titan's atmosphere and haze by iteratively adapting models to create a best fit to the surface reflectance properties. 相似文献
