Transformations of European Financial Instruments in the Context of European Enlargement Process

The necessity of a regional development policy at the nowadays’ European Union level has become vital since the beginning of the enlargement process in 1973 when to those six founding states (Belgium, France, Germany, Italy, Luxembourg and Netherlands) subjoined Great Britain, Ireland and Denmark. In 1957 when European Economic Community was founded, the EU-6 recorded a similar development level, the regional problems being isolated only in Southern part of Italy. Although on Italy request, the Treaty ascertained the existence of some inequities between prosperity levels of different regions, article 130 was one of the fundamental motives of creating the European Investment Bank, which may be considered one of the regional policy instruments. The enlargement process increased regional problems, major disparities regarding the economic development level being recorded between EU-6 regions and regions of the new member states (North part of England and North part of Ireland). Rural areas from Denmark and Ireland recorded a precarious development compared with similar areas from member states, and mining regions of Great Britain were confronted with industrial re-conversion problems. These kinds of problems existed even inside member states so that carboniferous regions Lorena (France), Ruhr (Germany), South part of Belgium were strongly affected by the deindustrialisation process. These situations led to the creation of the European Regional Development Fund in 1975 and its main objective at that moment was promoting innovation and infrastructure development in order to adjust the existing discrepancies at the Community level.European Financial instruments, European Regional Development Fund, economic development

Constraining multiple systems with GAIA

GAIA will provide observations of some multiple asteroid and dwarf systems. These observations are a way to determine and improve the quantification of dynamical parameters, such as the masses and the gravity fields, in these multiple systems. Here we investigate this problem in the cases of Pluto's and Eugenia's system. We simulate observations reproducing an approximate planning of the GAIA observations for both systems, as well as the New Horizons observations of Pluto. We have developed a numerical model reproducing the specific behavior of multiple asteroid system around the Sun and fit it to the simulated observations using least-square method, giving the uncertainties on the fitted parameters. We found that GAIA will improve significantly the precision of Pluto's and Charon's mass, as well as Petit Prince's orbital elements and Eugenia's polar oblateness.Comment: 5 pages, accepted by Planetary and Space Science, Gaia GREAT-SSO-Pis

On the distribution of adjectives in Romanian : the cel construction

This paper deals with the variable position of adjectives in the Romanian DP. As all other Romance languages, Romanian allows for adjectives to appear in both prenominal and post-nominal position. In addition, however, Romanian has a third pattern: the so-called cel construction, in which the adjective in the post-nominal position is preceded by a determiner-like element, cel. This pattern is superficially similar to Determiner Spreading in Greek. In this paper we contrast the cel construction to Greek DS and discuss the similarities and differences between the two. We then present an analysis of cel as involving an appositive specification clause, building on de Vries (2002). We argue that the same structure is also involved in the context of nominal ellipsis, the second environment in which cel is found

Component-resolved Near-infrared Spectra of the (22) Kalliope System

We observed (22) Kalliope and its companion Linus with the integral-field spectrograph OSIRIS, which is coupled to the adaptive optics system at the W.M. Keck II telescope on March 25 2008. We present, for the first time, component-resolved spectra acquired simultaneously in each of the Zbb (1-1.18 um), Jbb (1.18-1.42 um), Hbb (1.47-1.80 um), and Kbb (1.97-2.38 um) bands. The spectra of the two bodies are remarkably similar and imply that both bodies were formed at the same time from the same material; such as via incomplete re-accretion after a major impact on the precursor body.Comment: 20 pages, 5 figures, 1 table. Accepted for publication in Icaru

Supercritical Mean Field Equations on convex domains and the Onsager's statistical description of two-dimensional turbulence

We are motivated by the study of the Microcanonical Variational Principle within the Onsager's description of two-dimensional turbulence in the range of energies where the equivalence of statistical ensembles fails. We obtain sufficient conditions for the existence and multiplicity of solutions for the corresponding Mean Field Equation on convex and "thin" enough domains in the supercritical (with respect to the Moser-Trudinger inequality) regime. This is a brand new achievement since existence results in the supercritical region were previously known \un{only} on multiply connected domains. Then we study the structure of these solutions by the analysis of their linearized problems and also obtain a new uniqueness result for solutions of the Mean Field Equation on thin domains whose energy is uniformly bounded from above. Finally we evaluate the asymptotic expansion of those solutions with respect to the thinning parameter and use it together with all the results obtained so far to solve the Microcanonical Variational Principle in a small range of supercritical energies where the entropy is eventually shown to be concave.Comment: 35 pages. In this version we have added an interesting remark (please see Remark 1.17 p. 9). We have also slightly modified the statement of Proposition 1.14 at p.8 so to include a part of it in a separate 4-line Remark just after it (please see Remark 1.15 p.9

Orbits, masses, and evolution of main belt triple (87) Sylvia

Sylvia is a triple asteroid system located in the main belt. We report new adaptive optics observations of this system that extend the baseline of existing astrometric observations to a decade. We present the first fully dynamical 3-body model for this system by fitting to all available astrometric measurements. This model simultaneously fits for individual masses, orbits, and primary oblateness. We find that Sylvia is composed of a dominant central mass surrounded by two satellites orbiting at 706.5 +/- 2.5 km and 1357 +/- 4.0 km, i.e., about 5 and nearly 10 primary radii. We derive individual masses of 1.484 -0.014/+0.016 x 10^19 kg for the primary (corresponding to a density of 1.29 +/- 0.39 g cm^-3), 7.33 -2.3/+4.7 x 10^14 kg for the inner satellite, and 9.32 -8.3/+20.7 x 10^14 kg for the outer satellite. The oblateness of the primary induces substantial precession and the J_2 value can be constrained to the range of 0.0985-0.1. The orbits of the satellites are relatively circular with eccentricities less than 0.04. The spin axis of the primary body and the orbital poles of both satellites are all aligned within about two degrees of each other, indicating a nearly coplanar configuration and suggestive of satellite formation in or near the equatorial plane of the primary. We also investigate the past orbital evolution of the system by simulating the effects of a recent passage through 3:1 mean-motion eccentricity-type resonances. In some scenarios this allow us to place constraints on interior structure and past eccentricities.Comment: 14 pages, 8 figures, accepted to A