Trade dispute settlement mechanisms: the WTO dispute settlement understanding in the wake of the GATT

A critical feature of the GATT Uruguay Round negotiations was the establishment of a new and more effective system of dealing with international trade disputes, known as the WTO Dispute Settlement Understanding (DSU). The original GATT dispute settlement system comprised rudimentary remnants of a more thorough framework contained in the defunct Havana Charter of the International Trade Organization (ITO). By the time of the start of the Uruguay Round negotiations in Punta del Este in 1986, the effectiveness and credibility of the GATT dispute settlement system was being very seriously questioned. The primary reason for the increasing lack of confidence in the system was the propensity of GATT contracting countries to ignore the findings of Panels, resulting in a stalemate in a number of high profile trade disputes. Several trade disputes between the EU and the United States discussed were initiated under the GATT dispute settlement system but remained unresolved. These disputes became increasingly acrimonious as a direct consequence of the failure of the GATT system to enforce a satisfactory resolution. This paper provides an outline of the workings of the GATT and WTO dispute settlement systems underlie several recent trade disputes. The first two sections deal with the GATT system of settling trade disputes. The first details the key elements of the GATT dispute settlement system while the second considers its performance in resolving disputes. Section 3 outlines the origins of the WTO DSU and summarises its principal Articles. The WTO DSU is appraised on the basis of its first nine years of operation in Section 4 followed by a brief discussion of the key issues that have arisen from its operation. The final Section makes some concluding comments on the relative efficacy of the GATT and WTO dispute settlement systems.

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The XMM-Newton EPIC Background and the production of Background Blank Sky Event Files

We describe in detail the nature of XMM-Newton EPIC background and its various complex components, summarising the new findings of the XMM-Newton EPIC background working group, and provide XMM-Newton background blank sky event files for use in the data analysis of diffuse and extended sources. Blank sky event file data sets are produced from the stacking of data, taken from 189 observations resulting from the Second XMM-Newton Serendipitous Source Catalogue (2XMMp) reprocessing. The data underwent several filtering steps, using a revised and improved method over previous work, which we describe in detail. We investigate several properties of the final blank sky data sets. The user is directed to the location of the final data sets. There is a final data set for each EPIC instrument-filter-mode combination.Comment: Paper accepted by A&A 22 December 2006. 14 pages, 8 figures. Paper can also be found at http://www.star.le.ac.uk/~jac48/publications

A Semi-Analytic dynamical friction model that reproduces core stalling

We present a new semi-analytic model for dynamical friction based on Chandrasekhar's formalism. The key novelty is the introduction of physically motivated, radially varying, maximum and minimum impact parameters. With these, our model gives an excellent match to full N-body simulations for isotropic background density distributions, both cuspy and shallow, without any fine-tuning of the model parameters. In particular, we are able to reproduce the dramatic core-stalling effect that occurs in shallow/constant density cores, for the first time. This gives us new physical insight into the core-stalling phenomenon. We show that core stalling occurs in the limit in which the product of the Coulomb logarithm and the local fraction of stars with velocity lower than the infalling body tends to zero. For cuspy backgrounds, this occurs when the infalling mass approaches the enclosed background mass. For cored backgrounds, it occurs at larger distances from the centre, due to a combination of a rapidly increasing minimum impact parameter and a lack of slow moving stars in the core. This demonstrates that the physics of core-stalling is likely the same for both massive infalling objects and low-mass objects moving in shallow density backgrounds. We implement our prescription for dynamical friction in the direct summation code NBODY6 as an analytic correction for stars that remain within the Roche volume of the infalling object. This approach is computationally efficient, since only stars in the inspiralling system need to be evolved with direct summation. Our method can be applied to study a variety of astrophysical systems, including young star clusters orbiting near the Galactic Centre; globular clusters moving within the Galaxy; and dwarf galaxies orbiting within dark matter halos.Comment: 16 pages, 21 figures, Accepted for publication in MNRA