El bienestar en España: una perspectiva de largo plazo, 1850-1991

Los historiadores económicos han estimado tradicionalmente el bienestar en términos de renta por persona. Durante la última década se han publicado, sin embargo, diversos trabajos que utilizan otros indicadores. Siguiendo esta línea de investigación, el artículo contrasta cuatro indicadores del bienestar en España (renta per capita, índice de Desarrollo Humano, Índice Físico de Calidad de Vida y estatura), dos de los cuales son inéditos (IDH e IFCV). Los resultados complican el objeto de estudio, pero sirven para proponer algunas hipótesis que deben ser ratificadas o desmentidas por futuras investigaciones.

Características de la tematización del esquema de límite de una función

Esta investigación estudia las diferentes estructuras subyacentes en el esquema de límite de una función observadas en 23 estudiantes de Bachillerato situados en el nivel Trans del desarrollo del esquema de límite de una función. El esquema de límite de una función se caracterizó en términos de la habilidad que los estudiantes manifestaron en la construcción de la concepción dinámica del límite mediante la coordinación de los procesos de aproximación en el dominio y en el rango, diferenciando aquellas en las que las aproximaciones laterales coinciden de las que no coinciden. Nuestros resultados sugieren que los estudiantes construyen diferentes estructuras subyacentes al esquema debido a las relaciones que establecen entre el límite de una función en un punto y su representación gráfica que permiten identificar características del esquema tematizado del límite de una función.

Una defensa del convencionalismo jurídico

Este trabajo muestra que la existencia de un sistema jurídico requiere la presencia de una práctica unitaria de identificación de normas. El autor sostiene que esa práctica consiste en una convención constitutiva, que permite identificar de manera autónoma el Derecho de una determinada comunidad. Se pone de relieve de este modo una forma específica en que el Derecho es una creación social: del mismo modo que la existencia del dinero requiere la creencia de que éste existe, también la existencia de un sistema jurídico depende, en última instancia, de un conjunto de creencias compartido por las personas relevantes. El planteamiento de esta posición y de sus ventajas se lleva a cabo a lo largo de los apartados 2, 3, 4 y 5. El último apartado se dedica a examinar y a descartar cinco posibles objeciones a una tesis convencionalista como la que aquí se defiende.

Principios éticos y código de conducta para personas y entidades mediadoras

En este artículo se propone un código ético a modo de principios inspiradores de la intervención en procesos de gestión de conflictos y, en especial, en mediación. Esta propuesta combina la trayectoria del movimiento internacional en el desarrollo de procesos de calidad en la resolución de conflictos, con cuestionamientos prácticos que genera la intervención directa en la realidad española. Se ofrecen pautas de actuación para desarrollar el buen hacer de la persona mediadora, identificando una serie de situaciones excepcionales en las que, según el contexto y el rol profesional, se cuestionan tales principios y se anima a la adaptación a las necesidades de cada conflicto y a la evolución social.

Constitucionalismo principialista y constitucionalismo garantista

En este artículo, el autor presenta las diferencias más relevantes entre el neoconstitucionalismo y el constitucionalismo garantista. En primer lugar, afirma que el constitucionalismo puede ser concebido de dos formas opuestas: como una superación del positivismo jurídico en sentido tendencialmente iusnaturalista o como su expansión o perfeccionamiento, realizando para llevar a cabo esta labor una revisión terminológica. En segundo lugar, el autor considera que si las constituciones incorporan principios de justicia de carácter ético-político desaparece el principal rasgo distintivo del positivismo jurídico: la separación entre Derecho y moral o entre validez y justicia. A continuación, considera al constitucionalismo garantista como un iuspositivismo reforzado, completando al Estado de Derecho porque comporta el sometimiento al Derecho y al control de constitucionalidad. En cuarto lugar, el autor afirma que la tesis de que todo ordenamiento jurídico satisface objetivamente algún «mínimo ético» no es más que la vieja tesis iusnaturalista, que termina por convertirse en la actual versión del legalismo ético que es el constitucionalismo ético, en virtud del cual los principios constitucionales se pretenden objetivamente justos. En quinto lugar, el autor realiza una crítica a la contraposición entre principios y reglas, en los que se basa una concepción de la constitución y del constitucionalismo opuesta a la concepción positivista y garantista. En sexto lugar, el autor afirma que la idea de que los principios constitucionales son siempre objeto de ponderación y no de aplicación genera un peligro para la independencia de la jurisdicción y para su legitimación política. Finalmente, el autor considera que el constitucionalismo conlleva un debilitamiento y virtualmente un colapso de la normatividad de los principios constitucionales, así como una degradación de los derechos fundamentales establecidos en ellas a meras recomendaciones genéricas de carácter ético-político.

Force-free twisted magnetospheres of neutron stars

Context. The X-ray spectra observed in the persistent emission of magnetars are evidence for the existence of a magnetosphere. The high-energy part of the spectra is explained by resonant cyclotron upscattering of soft thermal photons in a twisted magnetosphere, which has motivated an increasing number of efforts to improve and generalize existing magnetosphere models. Aims. We want to build more general configurations of twisted, force-free magnetospheres as a first step to understanding the role played by the magnetic field geometry in the observed spectra. Methods. First we reviewed and extended previous analytical works to assess the viability and limitations of semi-analytical approaches. Second, we built a numerical code able to relax an initial configuration of a nonrotating magnetosphere to a force-free geometry, provided any arbitrary form of the magnetic field at the star surface. The numerical code is based on a finite-difference time-domain, divergence-free, and conservative scheme, based of the magneto-frictional method used in other scenarios. Results. We obtain new numerical configurations of twisted magnetospheres, with distributions of twist and currents that differ from previous analytical solutions. The range of global twist of the new family of solutions is similar to the existing semi-analytical models (up to some radians), but the achieved geometry may be quite different. Conclusions. The geometry of twisted, force-free magnetospheres shows a wider variety of possibilities than previously considered. This has implications for the observed spectra and opens the possibility of implementing alternative models in simulations of radiative transfer aiming at providing spectra to be compared with observations.

Pulsar timing irregularities and the imprint of magnetic field evolution

Context. The rotational evolution of isolated neutron stars is dominated by the magnetic field anchored to the solid crust of the star. Assuming that the core field evolves on much longer timescales, the crustal field evolves mainly though Ohmic dissipation and the Hall drift, and it may be subject to relatively rapid changes with remarkable effects on the observed timing properties. Aims. We investigate whether changes of the magnetic field structure and strength during the star evolution may have observable consequences in the braking index n. This is the most sensitive quantity to reflect small variations of the timing properties that are caused by magnetic field rearrangements. Methods. We performed axisymmetric, long-term simulations of the magneto-thermal evolution of neutron stars with state-of-the-art microphysical inputs to calculate the evolution of the braking index. Relatively rapid magnetic field modifications can be expected only in the crust of neutron stars, where we focus our study. Results. We find that the effect of the magnetic field evolution on the braking index can be divided into three qualitatively different stages depending on the age and the internal temperature: a first stage that may be different for standard pulsars (with n ~ 3) or low field neutron stars that accreted fallback matter during the supernova explosion (systematically n < 3); in a second stage, the evolution is governed by almost pure Ohmic field decay, and a braking index n > 3 is expected; in the third stage, at late times, when the interior temperature has dropped to very low values, Hall oscillatory modes in the neutron star crust result in braking indices of a high absolute value and both positive and negative signs. Conclusions. Current magneto-thermal evolution models predict a large contribution to the timing noise and, in particular, to the braking index, from temporal variations of the magnetic field. Models with strong (≳ 1014 G) multipolar or toroidal components, even with a weak (~1012 G) dipolar field are consistent with the observed trend of the timing properties.

A new code for the Hall-driven magnetic evolution of neutron stars

Over the past decade, the numerical modeling of the magnetic field evolution in astrophysical scenarios has become an increasingly important field. In the crystallized crust of neutron stars the evolution of the magnetic field is governed by the Hall induction equation. In this equation the relative contribution of the two terms (Hall term and Ohmic dissipation) varies depending on the local conditions of temperature and magnetic field strength. This results in the transition from the purely parabolic character of the equations to the hyperbolic regime as the magnetic Reynolds number increases, which presents severe numerical problems. Up to now, most attempts to study this problem were based on spectral methods, but they failed in representing the transition to large magnetic Reynolds numbers. We present a new code based on upwind finite differences techniques that can handle situations with arbitrary low magnetic diffusivity and it is suitable for studying the formation of sharp current sheets during the evolution. The code is thoroughly tested in different limits and used to illustrate the evolution of the crustal magnetic field in a neutron star in some representative cases. Our code, coupled to cooling codes, can be used to perform long-term simulations of the magneto-thermal evolution of neutron stars.

Unifying the observational diversity of isolated neutron stars via magneto-thermal evolution models

Observations of magnetars and some of the high magnetic field pulsars have shown that their thermal luminosity is systematically higher than that of classical radio-pulsars, thus confirming the idea that magnetic fields are involved in their X-ray emission. Here we present the results of 2D simulations of the fully coupled evolution of temperature and magnetic field in neutron stars, including the state-of-the-art kinetic coefficients and, for the first time, the important effect of the Hall term. After gathering and thoroughly re-analysing in a consistent way all the best available data on isolated, thermally emitting neutron stars, we compare our theoretical models to a data sample of 40 sources. We find that our evolutionary models can explain the phenomenological diversity of magnetars, high-B radio-pulsars, and isolated nearby neutron stars by only varying their initial magnetic field, mass and envelope composition. Nearly all sources appear to follow the expectations of the standard theoretical models. Finally, we discuss the expected outburst rates and the evolutionary links between different classes. Our results constitute a major step towards the grand unification of the isolated neutron star zoo.

The outburst decay of the low magnetic field magnetar SGR 0418+5729

We report on the long-term X-ray monitoring of the outburst decay of the low magnetic field magnetar SGR 0418+5729 using all the available X-ray data obtained with RXTE, Swift, Chandra, and XMM-Newton observations from the discovery of the source in 2009 June up to 2012 August. The timing analysis allowed us to obtain the first measurement of the period derivative of SGR 0418+5729: ˙ P = 4(1) × 10−15 s s−1, significant at a ∼3.5σ confidence level. This leads to a surface dipolar magnetic field of Bdip 6 × 1012 G. This measurement confirms SGR 0418+5729 as the lowest magnetic field magnetar. Following the flux and spectral evolution from the beginning of the outburst up to ∼1200 days, we observe a gradual cooling of the tiny hot spot responsible for the X-ray emission, from a temperature of ∼0.9 to 0.3 keV. Simultaneously, the X-ray flux decreased by about three orders of magnitude: from about 1.4 × 10−11 to 1.2 × 10−14 erg s−1 cm−2. Deep radio, millimeter, optical, and gamma-ray observations did not detect the source counterpart, implying stringent limits on its multi-band emission, as well as constraints on the presence of a fossil disk. By modeling the magneto-thermal secular evolution of SGR 0418+5729, we infer a realistic age of ∼550 kyr, and a dipolar magnetic field at birth of ∼1014 G. The outburst characteristics suggest the presence of a thin twisted bundle with a small heated spot at its base. The bundle untwisted in the first few months following the outburst, while the hot spot decreases in temperature and size. We estimate the outburst rate of low magnetic field magnetars to be about one per year per galaxy, and we briefly discuss the consequences of such a result in several other astrophysical contexts.

A strongly magnetized pulsar within the grasp of the milky way’s supermassive black hole

The center of our Galaxy hosts a supermassive black hole, Sagittarius (Sgr) A∗. Young, massive stars within 0.5 pc of Sgr A∗ are evidence of an episode of intense star formation near the black hole a few million years ago, which might have left behind a young neutron star traveling deep into Sgr A∗’s gravitational potential. On 2013 April 25, a short X-ray burst was observed from the direction of the Galactic center. With a series of observations with the Chandra and the Swift satellites, we pinpoint the associated magnetar at an angular distance of 2.4±0.3 arcsec from Sgr A∗, and refine the source spin period and its derivative (P = 3.7635537(2) s and ˙ P = 6.61(4) × 10−12 s s−1), confirmed by quasi simultaneous radio observations performed with the Green Bank Telescope and Parkes Radio Telescope, which also constrain a dispersion measure of DM = 1750 ± 50 pc cm−3, the highest ever observed for a radio pulsar. We have found that this X-ray source is a young magnetar at ≈0.07–2 pc from Sgr A∗. Simulations of its possible motion around Sgr A∗ show that it is likely (∼90% probability) in a bound orbit around the black hole. The radiation front produced by the past activity from the magnetar passing through the molecular clouds surrounding the Galactic center region might be responsible for a large fraction of the light echoes observed in the Fe fluorescence features.

The imprint of the crustal magnetic field on the thermal spectra and pulse profiles of isolated neutron stars

Isolated neutron stars (NSs) show a bewildering variety of astrophysical manifestations, presumably shaped by the magnetic field strength and topology at birth. Here, using state-of-the-art calculations of the coupled magnetic and thermal evolution of NSs, we compute the thermal spectra and pulse profiles expected for a variety of initial magnetic field configurations. In particular, we contrast models with purely poloidal magnetic fields to models dominated by a strong internal toroidal component. We find that, while the former displays double-peaked profiles and very low pulsed fractions, in the latter, the anisotropy in the surface temperature produced by the toroidal field often results in a single pulse profile, with pulsed fractions that can exceed the 50–60 per cent level even for perfectly isotropic local emission. We further use our theoretical results to generate simulated ‘observed’ spectra, and show that blackbody (BB) fits result in inferred radii that can be significantly smaller than the actual NS radius, even as low as ∼1–2 km for old NSs with strong internal toroidal fields and a high absorption column density along their line of sight. We compute the size of the inferred BB radius for a few representative magnetic field configurations, NS ages and magnitudes of the column density. Our theoretical results are of direct relevance to the interpretation of X-ray observations of isolated NSs, as well as to the constraints on the equation of state of dense matter through radius measurements.

The influence of magnetic field geometry on magnetars X-ray spectra

Nowadays, the analysis of the X-ray spectra of magnetically powered neutron stars or magnetars is one of the most valuable tools to gain insight into the physical processes occurring in their interiors and magnetospheres. In particular, the magnetospheric plasma leaves a strong imprint on the observed X-ray spectrum by means of Compton up-scattering of the thermal radiation coming from the star surface. Motivated by the increased quality of the observational data, much theoretical work has been devoted to develop Monte Carlo (MC) codes that incorporate the effects of resonant Compton scattering (RCS) in the modeling of radiative transfer of photons through the magnetosphere. The two key ingredients in this simulations are the kinetic plasma properties and the magnetic field (MF) configuration. The MF geometry is expected to be complex, but up to now only mathematically simple solutions (self-similar solutions) have been employed. In this work, we discuss the effects of new, more realistic, MF geometries on synthetic spectra. We use new force-free solutions [14] in a previously developed MC code [9] to assess the influence of MF geometry on the emerging spectra. Our main result is that the shape of the final spectrum is mostly sensitive to uncertain parameters of the magnetospheric plasma, but the MF geometry plays an important role on the angle-dependence of the spectra.