Fabricating Economic Development

Much of the literature, regardless of academic discipline, presents the publication of Economic Development in 1958 as analogous to a"big bang" event in the creation of modern Ireland. However, such a "big bang" perspective misrepresents the sophistication of economic debates prior to Whitaker's report as well as distorting the interpretation of subsequent developments. This paper reappraises Irish economic thinking before and after the publication of Economic Development. It is argued that an economically "liberal" approach to Keynesianism, such as that favoured by T. K. Whitaker and George O'Brien, lost out in the 1960s to a more interventionist approach: only later did a more liberal approach to macroeconomic policy triumph. The rival approaches to academic economics were in turn linked to wider debates on the influence of religious authorities on Irish higher education. Academic economists were particularly concerned with preserving their intellectual independence and how a shift to planning would keep decisions on resource allocation out of the reach of conservative political and religious leaders.

Fabricating Economic Development

This paper is concerned with the institutions of Irish economics; it is structured around two arguments each of which links to the thesis presented in Garvin’s Preventing the future (2004). Overall it will be demonstrated that Irish economics was shaped by intellectual trends experienced within economic thought globally as well as the social considerations that were peculiar to Ireland. The evidence presented indicates that firstly while Economic Development mattered to the Irish economy it did not matter for the reasons that most writers have suggested it did. It is argued for instance that much of the literature, regardless of academic discipline, presents the publication of Economic Development in 1958 as analogous to a “big bang” event in the creation of modern Ireland. However, such a “big bang” perspective misrepresents the sophistication of economic debates prior to Whitaker’s report as well as distorting the interpretation of subsequent developments. The paper secondly, by drawing on the contents of contemporary academic journals, reappraises Irish economic thinking before and after the publication of Economic Development. It is argued that an economically “liberal” approach to Keynesianism, such as that favoured by TK Whitaker and George O’Brien, lost out in the 1960s to a more interventionist approach: only later did a more liberal approach to macroeconomic policy triumph. The rival approaches to academic economics were in turn linked to wider debates on the influence of religious authorities on Irish higher education. Academic economists were particularly concerned with preserving their intellectual independence and how a shift to planning would keep decisions on resource allocation out of the reach of conservative political and religious leaders.

Slowly fading super-luminous supernovae that are not pair-instability explosions

Super-luminous supernovae that radiate more than 10 44 ergs per second at their peak luminosity have recently been discovered in faint galaxies at redshifts of 0.1-4. Some evolve slowly, resembling models of 'pair-instability' supernovae. Such models involve stars with original masses 140-260 times that of the Sun that now have carbon-oxygen cores of 65-130 solar masses. In these stars, the photons that prevent gravitational collapse are converted to electron-positron pairs, causing rapid contraction and thermonuclear explosions. Many solar masses of 56 Ni are synthesized; this isotope decays to 56 Fe via 56 Co, powering bright light curves. Such massive progenitors are expected to have formed from metal-poor gas in the early Universe. Recently, supernova 2007bi in a galaxy at redshift 0.127 (about 12 billion years after the Big Bang) with a metallicity one-third that of the Sun was observed to look like a fading pair-instability supernova. Here we report observations of two slow-to-fade super-luminous supernovae that show relatively fast rise times and blue colours, which are incompatible with pair-instability models. Their late-time light-curve and spectral similarities to supernova 2007bi call the nature of that event into question. Our early spectra closely resemble typical fast-declining super-luminous supernovae, which are not powered by radioactivity. Modelling our observations with 10-16 solar masses of magnetar-energized ejecta demonstrates the possibility of a common explosion mechanism. The lack of unambiguous nearby pair-instability events suggests that their local rate of occurrence is less than 6 × 10 -6 times that of the core-collapse rate. © 2013 Macmillan Publishers Limited. All rights reserved.

Astrophysics: Cosmic explosions in the young Universe

The discovery of two superluminous supernovae at large distances from Earth pushes the frontier of supernova studies to just 1.5 billion years after the Big Bang, and suggests that they may be common in the young Universe. See Letter p.228

Astronomy.

Examina la historia de esta ciencia considerada la más antigua de todas por el interés que desde la antigüedad ha suscitado en los hombres el conocimiento de los complejos movimientos de los objetos celestiales.También, se repasan los orígenes del universo con la violenta explosión ocurrida hace billones de años, llamada Big Bang. Se estudia el sistema solar, formado de planetas, lunas e innumerables cuerpos más pequeños como asteroides y cometas. Se completa con una observación de las estrellas y galaxias en el cielo de la noche, con cartas estelares y perfiles de constelaciones y, por último, se añade una guía con la posición mes a mes de las constelaciones septentrionales y australes.

El derecho de la naturaleza: fundamentos

Sumario: I. Todos los caminos conducen a Roma. 1.1. La dignidad. 1.2. El derecho subjetivo. 1.3. La capacidad. 1.4. La igualdad. II. Estirar los pies hasta donde alcanza la sábana. 2.1. La dignidad. 2.2. El derecho subjetivo. 2.3. La capacidad. 2.4. La igualdad. III. Caminar alegremente hacia la fuente. 3.1. La relacionalidad. 3.2. La correspondencia. 3.3. La complementariedad. 3.4. El principio de reciprocidad. IV. Del agujero negro al Big Bang. V. Reflexiones finales. VI. Bibliografía.

Imprints of fast-rotating massive stars in the Galactic Bulge

The first stars that formed after the Big Bang were probably massive(1), and they provided the Universe with the first elements heavier than helium (`metals`), which were incorporated into low-mass stars that have survived to the present(2,3). Eight stars in the oldest globular cluster in the Galaxy, NGC 6522, were found to have surface abundances consistent with the gas from which they formed being enriched by massive stars(4) (that is, with higher alpha-element/Fe and Eu/Fe ratios than those of the Sun). However, the same stars have anomalously high abundances of Ba and La with respect to Fe(4), which usually arises through nucleosynthesis in low-mass stars(5) (via the slow-neutron-capture process, or s-process). Recent theory suggests that metal-poor fast-rotating massive stars are able to boost the s-process yields by up to four orders of magnitude(6), which might provide a solution to this contradiction. Here we report a reanalysis of the earlier spectra, which reveals that Y and Sr are also over-abundant with respect to Fe, showing a large scatter similar to that observed in extremely metal-poor stars(7), whereas C abundances are not enhanced. This pattern is best explained as originating in metal-poor fast-rotating massive stars, which might point to a common property of the first stellar generations and even of the `first stars`.

Radiative capture of nucleons at astrophysical energies with single-particle states

Radiative capture of nucleons at energies of astrophysical interest is one of the most important processes for nucleosynthesis. The nucleon capture can occur either by a compound nucleus reaction or by a direct process. The compound reaction cross sections are usually very small, especially for light nuclei. The direct capture proceeds either via the formation of a single-particle resonance or a non-resonant capture process. In this work we calculate radiative capture cross sections and astrophysical S-factors for nuclei in the mass region A < 20 using single-particle states. We carefully discuss the parameter fitting procedure adopted in the simplified two-body treatment of the capture process. Then we produce a detailed list of cases for which the model works well. Useful quantities, such as spectroscopic factors and asymptotic normalization coefficients, are obtained and compared to published data. (C) 2010 Elsevier Inc. All rights reserved.

Observation of an Antimatter Hypernucleus

Nuclear collisions recreate conditions in the universe microseconds after the Big Bang. Only a very small fraction of the emitted fragments are light nuclei, but these states are of fundamental interest. We report the observation of antihypertritons-comprising an antiproton, an antineutron, and an antilambda hyperon-produced by colliding gold nuclei at high energy. Our analysis yields 70 +/- 17 antihypertritons (3/Lambda(H) over bar) and 157 +/- 30 hypertritons ((3)(Lambda)H). The measured yields of (3)(Lambda)H (3/Lambda(H) over bar) and (3)He ((3)(He) over bar) are similar, suggesting an equilibrium in coordinate and momentum space populations of up, down, and strange quarks and antiquarks, unlike the pattern observed at lower collision energies. The production and properties of antinuclei, and of nuclei containing strange quarks, have implications spanning nuclear and particle physics, astrophysics, and cosmology.

Observation of the antimatter helium-4 nucleus

High-energy nuclear collisions create an energy density similar to that of the Universe microseconds after the Big Bang(1); in both cases, matter and antimatter are formed with comparable abundance. However, the relatively short-lived expansion in nuclear collisions allows antimatter to decouple quickly from matter, and avoid annihilation. Thus, a high-energy accelerator of heavy nuclei provides an efficient means of producing and studying antimatter. The antimatter helium-4 nucleus ((4)(He) over bar), also known as the anti-alpha ((alpha) over bar), consists of two antiprotons and two antineutrons (baryon number B = -4). It has not been observed previously, although the alpha-particle was identified a century ago by Rutherford and is present in cosmic radiation at the ten per cent level(2). Antimatter nuclei with B -1 have been observed only as rare products of interactions at particle accelerators, where the rate of antinucleus production in high-energy collisions decreases by a factor of about 1,000 with each additional antinucleon(3-5). Here we report the observation of (4)<(He) over bar, the heaviest observed antinucleus to date. In total, 18 (4)(He) over bar counts were detected at the STAR experiment at the Relativistic Heavy Ion Collider (RHIC; ref. 6) in 10(9) recorded gold-on-gold (Au+Au) collisions at centre-of-mass energies of 200 GeV and 62 GeV per nucleon-nucleon pair. The yield is consistent with expectations from thermodynamic(7) and coalescent nucleosynthesis(8) models, providing an indication of the production rate of even heavier antimatter nuclei and a benchmark for possible future observations of (4)(He) over bar in cosmic radiation.

Low-energy d plus d fusion reactions via the Trojan Horse Method

The bare nucleus S(E) factors for the (2)H(d, p)(3)H and (2)H(d.n)(3)He reactions have been measured for the first time via the Trojan Horse Method off the proton in (3)He from 1.5 MeV down to 2 key. This range overlaps with the relevant region for Standard Big Bang Nucleosynthesis as well as with the thermal energies of future fusion reactors and deuterium burning in the Pre-Main-Sequence phase of stellar evolution. This is the first pioneering experiment in quasi free regime where the charged spectator is detected. Both the energy dependence and the absolute value of the S(E) factors deviate by more than 15% from available direct data with new S(0) values of 57.4 +/- 1.8 MeVb for (3)H + p and 60.1 +/- 1.9 MeV b for (3)He + n. None of the existing fitting curves is able to provide the correct slope of the new data in the full range, thus calling for a revision of the theoretical description. This has consequences in the calculation of the reaction rates with more than a 25% increase at the temperatures of future fusion reactors. (C) 2011 Elsevier By. All rights reserved.

O processo de humanização: as bases constitutivas da subjetividade

Iniciando-se por uma descrição longitudinal, seguida de interpretação "a posteriori", obteve-se categorias relativas a cada dimensão do psiquismo. Estas, em seu caráter de transversalidade, foram tomadas como esteios para as explicações acerca da passagem do sujeito da condição biológica à condição de sujeito falante. O norteamento dessa análise teve como ponto de partida a postulação acerca dessas dimensões, dos aspectos relativos as mesmas, e dos efetores referentes por essa passagem, cujo início tem a esses aspectos que respondem lugar quando a mãe se dispõe a apontar para o sujeito o limite entre o núcleo filogenético e as transformações sócio-histórica. A partir dessa delimitação, ocorre a assimilação de características, tipicamente humanas para, enfim, serem fixados pela lei paterna, os limites do “tornar-se humano”. Nesse ínterim, são observadas ocorrências relativas as dimensões mencionadas. Tratando-se de permanência de conteúdos mantidos fora do campo da simbolização, e excluídos da matriz imaginária, tem-se então a caracterização do real ~elo seu mecanismo específico: a foraclusão. Ainda se situa a pulsão no seu caráter impensável e inominável. Já as ações resultantes do recalcamento originário concorrem para a formação de marcas não-simbolizáveis que, como faceta do imaginário, se vinculam às informações do núcleo filogenético referentes aos protofantasmas, aqui considerado corno outra faceta desta dimensão. No que concerne ao simbólico, registra-se a significação como fundante da condição humana, resultante do recalcamento propriamente dito. Sendo assim, a humanização enquanto explicada pelo conceito de recalcamento, conforme evidencia a metapsicologia freudiana, não açambarça todas as nuances relativas ao humano; visto englobar apenas aquilo que é imaginado corno fantasma ou aquilo que e apresentado simbolicamente. Por isso, a utilização do conceito de foraclusão, da perspectiva lacaniana, justifica-se pelo fato de oferecer uma visão mais completa dessa dinâmica. Desse modo, se pode incluir no escopo do "tornar-se humano", aqueles elementos não passíveis de simbolização, bem como aqueles da realidade pulsional que não se apresentam no texto do fantasma; mas que, ao se constituírem como um "pano-de-fundo", possibilitam que a conteúdos simbólicos e imaginários viabilizem a socialização. De resto, a socialização é um processo que, originado do simbólico, se assenta no imaginário tomado como base. Para isto, o real, em seu efeito marginal, possibilita o retorno ao simbólico. A partir daí, se verifica a utilização dos elementos culturais, que são descobertos em função daquilo que a atividade fantasmática suscita.

O enigmático problema das gigantes ricas em Lítio e as perspectivas com o satélite Kepler

Lithium (Li) is a chemical element with atomic number 3 and it is among the lightest known elements in the universe. In general, the Lithium is found in the nature under the form of two stable isotopes, the 6Li and 7Li. This last one is the most dominant and responds for about 93% of the Li found in the Universe. Due to its fragileness this element is largely used in the astrophysics, especially in what refers to the understanding of the physical process that has occurred since the Big Bang going through the evolution of the galaxies and stars. In the primordial nucleosynthesis in the Big Bang moment (BBN), the theoretical calculation forecasts a Li production along with all the light elements such as Deuterium and Beryllium. To the Li the BNB theory reviews a primordial abundance of Log log ǫ(Li) =2.72 dex in a logarithmic scale related to the H. The abundance of Li found on the poor metal stars, or pop II stars type, is called as being the abundance of Li primordial and is the measure as being log ǫ(Li) =2.27 dex. In the ISM (Interstellar medium), that reflects the current value, the abundance of Lithium is log ǫ(Li) = 3.2 dex. This value has great importance for our comprehension on the chemical evolution of the galaxy. The process responsible for the increasing of the primordial value present in the Li is not clearly understood until nowadays. In fact there is a real contribution of Li from the giant stars of little mass and this contribution needs to be well streamed if we want to understand our galaxy. The main objection in this logical sequence is the appearing of some giant stars with little mass of G and K spectral types which atmosphere is highly enriched with Li. Such elevated values are exactly the opposite of what could happen with the typical abundance of giant low mass stars, where convective envelops pass through a mass deepening in which all the Li should be diluted and present abundances around log ǫ(Li) ∼1.4 dex following the model of stellar evolution. In the Literature three suggestions are found that try to reconcile the values of the abundance of Li theoretical and observed in these rich in Li giants, but any of them bring conclusive answers. In the present work, we propose a qualitative study of the evolutionary state of the rich in Li stars in the literature along with the recent discovery of the first star rich in Li observed by the Kepler Satellite. The main objective of this work is to promote a solid discussion about the evolutionary state based on the characteristic obtained from the seismic analysis of the object observed by Kepler. We used evolutionary traces and simulation done with the population synthesis code TRILEGAL intending to evaluate as precisely as possible the evolutionary state of the internal structure of these groups of stars. The results indicate a very short characteristic time when compared to the evolutionary scale related to the enrichment of these stars

Anisotropias da radiação cósmica de fundo e vínculos em modelos com decaimento do vácuo

Many astronomical observations in the last few years are strongly suggesting that the current Universe is spatially flat and dominated by an exotic form of energy. This unknown energy density accelerates the universe expansion and corresponds to around 70% of its total density being usually called Dark Energy or Quintessence. One of the candidates to dark energy is the so-called cosmological constant (Λ) which is usually interpreted as the vacuum energy density. However, in order to remove the discrepancy between the expected and observed values for the vacuum energy density some current models assume that the vacuum energy is continuously decaying due to its possible coupling with the others matter fields existing in the Cosmos. In this dissertation, starting from concepts and basis of General Relativity Theory, we study the Cosmic Microwave Background Radiation with emphasis on the anisotropies or temperature fluctuations which are one of the oldest relic of the observed Universe. The anisotropies are deduced by integrating the Boltzmann equation in order to explain qualitatively the generation and c1assification of the fluctuations. In the following we construct explicitly the angular power spectrum of anisotropies for cosmologies with cosmological constant (ΛCDM) and a decaying vacuum energy density (Λ(t)CDM). Finally, with basis on the quadrupole moment measured by the WMAP experiment, we estimate the decaying rates of the vacuum energy density in matter and in radiation for a smoothly and non-smoothly decaying vacuum