De lo eterno a lo infinito: un intento de reconstrucción del argumento de Meliso (B2-4 D-K)

El autor ofrece un intento de reconstrucción lógicamente consistente e históricamenteplausible del argumento con que probaba Meliso la infinitud de lo que es (Mel. B 2-4 D-K), argumento tradicionalmente considerado como un manualístico ejemplo de falacia. La auténtica demostración de la infinitud por Meliso es la que menciona Aristóteles en De gen. et corr. 1 8, 325 a 13 (= Mel. B 4 a Reale), mientras que B 2, donde se la ha solido querer ver, tan sólo contiene una previa enunciación (primera frase) de los dos argumentos que van a seguir y el desarrollo del primero de ellos; el segundo, sobre la infinitud espacial, se desarrollaría en la segunda parte del fragmento, parte que, excepto la primera frase (B 3), se ha perdido. La reinterpretación de la primera partecomo una prueba de la infinitud se debe a Aristóteles, quien logró sacar magisteril partido de los defectos formales del argumento para echar por tierra la más importante tesis de su adversario atribuyéndole una demostración lógicamente inconsistente, de la que, en realidad, Meliso nunca se sirvió.

Prevenda

Aquest projecte es base en una aplicació de prevenda per terminals amb Sistema Operatiu Windows CE 4.3 i plataforma Pocket PC 2003. L'aplicació permetrà al terminal conectar-se amb un ordenador central (PC) per tal de descarregar la informació dels clients, artícles, rutes, etc. Una vegada s'hagi rebut la informació, el comercial podrà anar visitant els diferents clients seguint una ruta i introduint les comandes. En qualsevol moment del dia el comercial podrà enviar les comandes a la central mitjançant una conecció remota o bé mitjançant una comunicació directa.

The 2010 May Flaring Episode of Cygnus X-3 in Radio, X-rays, and γ-rays

In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ~3 day softening and recovery of the X-ray emission, followed almost immediately by a ~1 Jy radio flare at 15 GHz, followed by a 4.3σ γ-ray flare (E > 100 MeV) ~1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ-ray emission from Cyg X-3.

Hybrid model of a double-fed induction machine and back-to-back converter

This report details the port interconnection of two subsystems: a power electronics subsystem (a back-to-back AC/AC converter (B2B), coupled to a phase of the power grid), and an electromechanical subsystem (a doubly-fed induction machine (DFIM), coupled mechanically to a flywheel and electrically to the power grid and to a local varying load). Both subsystems have been essentially described in previous reports (deliverables D 0.5 and D 4.3.1), although some previously unpublished details are presented here. The B2B is a variable structure system (VSS), due to the presence of control-actuated switches: however from a modelling and simulation, as well as a control-design, point of view, it is sensible to consider modulated transformers (MTF in the bond-graph language) instead of the pairs of complementary switches. The port-Hamiltonian models of both subsystems are presents and coupled through a power-preserving interconnection, and the Hamiltonian description of the whole system is obtained; detailed bond-graphs of all the subsystems and the complete system are provided.

The 2010 May Flaring Episode of Cygnus X-3 in Radio, X-rays, and γ-rays

In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ~3 day softening and recovery of the X-ray emission, followed almost immediately by a ~1 Jy radio flare at 15 GHz, followed by a 4.3σ γ-ray flare (E > 100 MeV) ~1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ-ray emission from Cyg X-3.