La eficiencia energética: análisis empírico y regulatorio

A pesar de las ventajas medioambientales y económicas de la eficiencia energética, la experiencia muestra que las actuaciones en eficiencia energética se sitúan por debajo de lo requerido para afrontar los retos del modelo energético mundial. Ante esta paradoja, en este documento de trabajo, se realiza un análisis de los principales elementos que intervienen en el concepto de eficiencia energética, elaborando un diagnóstico que muestra las dificultades para acometer mejoras en este ámbito e identifica los instrumentos regulatorios que han tenido un mayor éxito. El documento se estructura en torno a cuatro bloques. En el primero, se elabora una breve descripción del concepto de eficiencia energética y su contribución, desde la perspectiva de la Agencia Internacional de la Energía, a la reducción de emisiones de gases de efecto invernadero (GEI), a la mejora de la seguridad energética y al desarrollo económico. Se particulariza el análisis para elaborar un diagnóstico del caso español y se presentan las principales dificultades para acometer mejoras, a partir de la experiencia empírica y los análisis académicos. En el segundo, después de revisar la literatura económica disponible y los documentos emitidos en la materia, especialmente aquellos elaborados por la Comisión Europea o la Agencia Internacional de la Energía, se analizan de forma equilibrada los principales instrumentos para mejorar la eficiencia energética, presentando tanto sus ventajas como sus inconvenientes. En el tercero se estudian las principales experiencias internacionales, presentándose los resultados que se han alcanzado en los distintos contextos con la utilización de los instrumentos del bloque anterior. Por último, se presentan unas recomendaciones regulatorias que tienen especial importancia en un contexto como el actual, en el que la política energética española ha establecido entre sus prioridades el ahorro y la eficiencia energética. En general, la experiencia muestra que un marco regulatorio de éxito debe contar con tres elementos básicos: precios que internalicen todos los costes, incluidos los ambientales, estándares energéticos y medidas de educación y sensibilización

Trajectory Reconstruction Techniques for Evaluation of ATC Systems

This paper is focused on trajectory reconstruction techniques for evaluating ATC systems, using real data of recorded opportunity traffic. We analyze different alternatives for this problem, from traditional interpolation approaches based on curve fitting to our proposed schemes based on modeling regular motion patterns with optimal smoothers. The extraction of trajectory features such as motion type (or mode of flight), maneuvers profile, geometric parameters, etc., allows a more accurate computation of the curve and the detailed evaluation of the data processors used in the ATC centre. Different alternatives will be compared with some performance results obtained with simulated and real data sets

Terrestrial planets in high-mass disks without gas giants

Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, superEarths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M. Results. All our simulations form massive planets on wide orbits. For a 0.1 M disk, 2–3 super-Earths of 2.8 to 5.9 M⊕ are formed between 2 and 5 AU. For disks of 0.125 and 0.15 M, our simulations produce a 10–17.1 M⊕ planet between 1.6 and 2.7 AU, and other super-Earths are formed in outer regions. Moreover, six planets survive in the habitable zone (HZ). These planets have masses from 1.9 to 4.7 M⊕ and significant water contents ranging from 560 to 7482 Earth oceans, where one Earth ocean represents the amount of water on Earth’s surface, which equals 2.8 × 10−4 M⊕. Of the six planets formed in the HZ, three are water worlds with 39%–44% water by mass. These planets start the simulations beyond the snow line, which explains their high water abundances. In general terms, the smaller the mass of the planets observed on wide orbits, the higher the possibility to find water worlds in the HZ. In fact, massive planets can act as a dynamical barrier that prevents the inward diffusion of water-rich embryos located beyond the snow line. Conclusions. Systems without gas giants that harbor super-Earths or Neptune-mass planets on wide orbits around solar-type stars are of astrobiological interest. These systems are likely to harbor super-Earths in the HZ with significant water contents, which missions such as Kepler and Darwin should be able to find.Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: Guilera, Octavio Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: Brunini, Adrian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentin

The Non-Structural NS1 Protein Unique to Respiratory Syncytial Virus: A Two-State Folding Monomer in Quasi-Equilibrium with a Stable Spherical Oligome

Human respiratory syncytial virus (hRSV) is a major infectious agent that cause pediatric respiratory disease worldwide. Considered one of the main virulence factors of hRSV, NS1 is known to suppress type I interferon response and signaling, thus favoring immune evasion. This, together with the fact that NS1 is unique to hRSV among paramyxoviruses, and that has no homology within databases, prompted us to investigate its conformational stability, equilibria and folding. Temperature cooperatively induces conformational changes leading to soluble spherical oligomers (NS1SOs) with amyloid-like or repetitive ß-sheet structures. The onset of the thermal transition is 45°C, and the oligomerization rate is increased by 25-fold from 40 to 46°C. Conformational stability analyzed by chemical perturbation of the NS1 monomer shows a two-state, highly reversible and cooperative unfolding, with a denaturant midpoint of 3.8 M, and a free energy change of 9.6±0.9 kcal⋅mol(-1). However, two transitions were observed in the chemical perturbation of NS1SOs: the first, from 2.0 to 3.0 M of denaturant, corresponds to a conformational transition and dissociation of the oligomers to the native monomer, indicating a substantial energy barrier. The second transition (2.0 to 3.5 M denaturant) corresponds to full unfolding of the native NS1 monomer. In addition, different cosolvent perturbations converged on the formation of ß-sheet enriched soluble oligomeric species, with secondary structure resembling those obtained after mild temperature treatment. Thus, a unique protein without homologs, structure or mechanistic information may switch between monomers and oligomers in conditions compatible with the cellular environment and be potentially modulated by crowding or compartmentalization. NS1 may act as a reservoir for increased levels and impact on protein turnover.Fil: Pretel, Miguel Esteban. Consejo Nacional de Invest.cientif.y Tecnicas. Oficina de Coordinacion Administrativa Pque. Centenario. Instituto de Invest.bioquimicas de Bs.as(i);Fil: Camporeale, Gabriela. Consejo Nacional de Invest.cientif.y Tecnicas. Oficina de Coordinacion Administrativa Pque. Centenario. Instituto de Invest.bioquimicas de Bs.as(i);Fil: de Prat Gay, Gonzalo. Consejo Nacional de Invest.cientif.y Tecnicas. Oficina de Coordinacion Administrativa Pque. Centenario. Instituto de Invest.bioquimicas de Bs.as(i)

Terrestrial planets in high-mass disks without gas giants

Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, superEarths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M. Results. All our simulations form massive planets on wide orbits. For a 0.1 M disk, 2–3 super-Earths of 2.8 to 5.9 M⊕ are formed between 2 and 5 AU. For disks of 0.125 and 0.15 M, our simulations produce a 10–17.1 M⊕ planet between 1.6 and 2.7 AU, and other super-Earths are formed in outer regions. Moreover, six planets survive in the habitable zone (HZ). These planets have masses from 1.9 to 4.7 M⊕ and significant water contents ranging from 560 to 7482 Earth oceans, where one Earth ocean represents the amount of water on Earth’s surface, which equals 2.8 × 10−4 M⊕. Of the six planets formed in the HZ, three are water worlds with 39%–44% water by mass. These planets start the simulations beyond the snow line, which explains their high water abundances. In general terms, the smaller the mass of the planets observed on wide orbits, the higher the possibility to find water worlds in the HZ. In fact, massive planets can act as a dynamical barrier that prevents the inward diffusion of water-rich embryos located beyond the snow line. Conclusions. Systems without gas giants that harbor super-Earths or Neptune-mass planets on wide orbits around solar-type stars are of astrobiological interest. These systems are likely to harbor super-Earths in the HZ with significant water contents, which missions such as Kepler and Darwin should be able to find.Instituto de Astrofísica de La Plat

Terrestrial planets in high-mass disks without gas giants

Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, superEarths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M. Results. All our simulations form massive planets on wide orbits. For a 0.1 M disk, 2–3 super-Earths of 2.8 to 5.9 M⊕ are formed between 2 and 5 AU. For disks of 0.125 and 0.15 M, our simulations produce a 10–17.1 M⊕ planet between 1.6 and 2.7 AU, and other super-Earths are formed in outer regions. Moreover, six planets survive in the habitable zone (HZ). These planets have masses from 1.9 to 4.7 M⊕ and significant water contents ranging from 560 to 7482 Earth oceans, where one Earth ocean represents the amount of water on Earth’s surface, which equals 2.8 × 10−4 M⊕. Of the six planets formed in the HZ, three are water worlds with 39%–44% water by mass. These planets start the simulations beyond the snow line, which explains their high water abundances. In general terms, the smaller the mass of the planets observed on wide orbits, the higher the possibility to find water worlds in the HZ. In fact, massive planets can act as a dynamical barrier that prevents the inward diffusion of water-rich embryos located beyond the snow line. Conclusions. Systems without gas giants that harbor super-Earths or Neptune-mass planets on wide orbits around solar-type stars are of astrobiological interest. These systems are likely to harbor super-Earths in the HZ with significant water contents, which missions such as Kepler and Darwin should be able to find.Instituto de Astrofísica de La Plat

El giro científico (1870-1910): hacia un nuevo concepto de opinión pública

El autor sostiene que durante las últimas décadas del siglo XIX y a comienzos del siglo XX se difundió en Europa y en América un nuevo enfoque que miraba al concepto de opinión pública desde una perspectiva más profunda y pretendidamente "científica "