Correlated adaptation of agents in a simple market: a statistical physics perspective

We discuss recent work in the study of a simple model for the collective behaviour of diverse speculative agents in an idealized stockmarket, considered from the perspective of the statistical physics of many-body systems. The only information about other agents available to any one is the total trade at time steps. Evidence is presented for correlated adaptation and phase transitions/crossovers in the global volatility of the system as a function of appropriate information scaling dimension. Stochastically controlled irrationally of individual agents is shown to be globally advantageous. We describe the derivation of the underlying effective stochastic differential equations which govern the dynamics, and make an interpretation of the results from the point of view of the statistical physics of disordered systems.Comment: 15 Pages. 5 figure

Les biomarqueurs dans la maladie de Fabry: relation entre Sphingosine-1 phosphate et Lyso-Gb3

Problématique : La maladie de Fabry est une maladie métabolique à stockage lysosomal. C'est une maladie héreditaire à transmission récessive qui concerne l'enzyme alpha-Galactosidase A. Le gène de l'alpha-Galactosidase A (GLA) se trouve au niveau du bras long du chromosome X «carté en Xq21.33-Xq22 ». L'enzyme muté ne recouvre plus son rôle catabolisateur et il ne métabolise pas le substrat globotriaosylceramide (Gb3). Par conséquence le Gb3 s'accumule dans tous les tissus. Dans les parois des vaisseaux sanguins le Gb3 s'accumule dans l'endothelium, la tunique interne des vaisseaux sanguins. Ce déficit métabolique se traduit par l'épaississement de la paroi vasculaire, des processus d'infarctus et ischémies du tissu cardiaque, rénal et cérébral. L'implication cardiaque de la maladie de Fabry est décrite chez plus de 78% des patients affectés par la maladie et se manifeste par une hypertrophie cardiaque du ventricule gauche. Toutefois, il n'existe pas de relation étroite entre hypertrophie cardiaque et le Gb3. La sphingosine 1-phosphate à été identifiée dans notre laboratoire et proposée comme facteur de croissance à l'origine du remodelage cardiovasculaire. De plus, la Globotriaosylsphingosine (Lyso-Gb3) à été aussi proposée comme facteur vasoactif chez les patients Fabry. Objectif : L'identification d'un biomarqueur pour le diagnostic et le suivi thérapeutique de la maladie de Fabry représente une domaine d'investigation active en recherche scientifique. Le Gb3 plasmatique ou dans les urines, la biopsie rénale ou cardiaque qui est mis en évidence grâce à la microscopie électronique sous forme de corps concentrique lamellaires, constituent les biomarqueurs classiques de la maladie de Fabry. Dernièrement, le Lyso-Gb3 et le Sphingosine-1 phosphate (S1P) ont été proposés comme marqueurs du remodelage cardiovasculaire. Le but de ce travail est de rassembler et de discuter la littérature concernant ces nouveaux marqueurs et, d'étudier une possible interaction entre Lyso-Gb3 et le S1P. Méthodologie : Rassembler la littérature scientifique et analyser l'implication de ces marqueurs dans la maladie de Fabry et leur effets cardiovasculaires. De plus, un travail expérimental est effectué. Ce travail consiste en l'identification d'une relation possible entre le Lyso-Gb3 et le S1P. Résultats : Avec ce travail on a cherché à actualiser et mettre à jour les notions concernant les biomarqueurs qui prennent place dans cette pathologie et les connaissances qu'on possède à ce jour sur les manifestations cardiovasculaires et neurologiques.La recherche d'un biomarqueur prime par le fait qu'un nombre considerable de patients est sous-diagnostiqués pour la maladie de Fabry et que entre les taux de substrat enzymatique accumulé dans les tissus et l'hypertrophie cardiaque, on peut constater une discordance. Grâce à ce travail expérimental, on a exclue la possibilité d'un effet précurseur du lyso-Gb3 pour le S1P. Nous avons montré que le Lyso-Gb3 est reconnu par les récepteurs du S1P avec des effets commun pour les S1P1-3 et différents pour le S1P2. Les taux du Lyso-Gb3 et du S1P doivent être mesuré chez les patients Fabry et une stratégie thérapeutique doit prendre en compte le rapport S1P/Lyso-Gb3

Atmosphere above a large solar pore

A large solar pore with a granular light bridge was observed on October 15, 2008 with the IBIS spectrometer at the Dunn Solar Telescope and a 69-min long time series of spectral scans in the lines Ca II 854.2 nm and Fe I 617.3 nm was obtained. The intensity and Doppler signals in the Ca II line were separated. This line samples the middle chromosphere in the core and the middle photosphere in the wings. Although no indication of a penumbra is seen in the photosphere, an extended filamentary structure, both in intensity and Doppler signals, is observed in the Ca II line core. An analysis of morphological and dynamical properties of the structure shows a close similarity to a superpenumbra of a sunspot with developed penumbra. A special attention is paid to the light bridge, which is the brightest feature in the pore seen in the Ca II line centre and shows an enhanced power of chromospheric oscillations at 3-5 mHz. Although the acoustic power flux in the light bridge is five times higher than in the "quiet" chromosphere, it cannot explain the observed brightness.Comment: 6 pages, 3 figures, accepted in Journal of Physics: Conference Serie

Imaging Spectropolarimetry with IBIS: Evolution of Bright Points in the Quiet Sun

We present the results from first spectropolarimetric observations of the solar photosphere acquired at the Dunn Solar Telescope with the Interferometric Bidimensional Spectrometer. Full Stokes profiles were measured in the Fe I 630.15 nm and Fe I 630.25 nm lines with high spatial and spectral resolutions for 53 minutes, with a Stokes V noise of 0.003 the continuum intensity level. The dataset allows us to study the evolution of several magnetic features associated with G-band bright points in the quiet Sun. Here we focus on the analysis of three distinct processes, namely the coalescence, fragmentation and cancellation of G-band bright points. Our analysis is based on a SIR inversion of the Stokes I and V profiles of both Fe I lines. The high spatial resolution of the G-band images combined with the inversion results helps to interpret the undergoing physical processes. The appearance (dissolution) of high-contrast G-band bright points is found to be related to the local increase (decrease) of the magnetic filling factor, without appreciable changes in the field strength. The cancellation of opposite-polarity bright points can be the signature of either magnetic reconnection or the emergence/submergence of magnetic loops.Comment: 4 pages, 5 figures, accepted for publication in ApJ Letter

Super-diffusion versus competitive advection: a simulation

Magnetic element tracking is often used to study the transport and diffusion of the magnetic field on the solar photosphere. From the analysis of the displacement spectrum of these tracers, it has been recently agreed that a regime of super-diffusivity dominates the solar surface. Quite habitually this result is discussed in the framework of fully developed turbulence. But the debate whether the super-diffusivity is generated by a turbulent dispersion process, by the advection due to the convective pattern, or by even another process, is still open, as is the question about the amount of diffusivity at the scales relevant to the local dynamo process. To understand how such peculiar diffusion in the solar atmosphere takes places, we compared the results from two different data-sets (ground-based and space-borne) and developed a simulation of passive tracers advection by the deformation of a Voronoi network. The displacement spectra of the magnetic elements obtained by the data-sets are consistent in retrieving a super-diffusive regime for the solar photosphere, but the simulation also shows a super-diffusive displacement spectrum: its competitive advection process can reproduce the signature of super-diffusion. Therefore, it is not necessary to hypothesize a totally developed turbulence regime to explain the motion of the magnetic elements on the solar surface

Chromospheric heating by acoustic waves compared to radiative cooling

Acoustic and magnetoacoustic waves are among the possible candidate mechanisms that heat the upper layers of solar atmosphere. A weak chromospheric plage near a large solar pore NOAA 11005 was observed on October 15, 2008 in the lines Fe I 617.3 nm and Ca II 853.2 nm with the Interferometric Bidimemsional Spectrometer (IBIS) attached to the Dunn Solar Telescope. Analyzing the Ca II observations with spatial and temporal resolutions of 0.4" and 52 s, the energy deposited by acoustic waves is compared with that released by radiative losses. The deposited acoustic flux is estimated from power spectra of Doppler oscillations measured in the Ca II line core. The radiative losses are calculated using a grid of seven 1D hydrostatic semi-empirical model atmospheres. The comparison shows that the spatial correlation of maps of radiative losses and acoustic flux is 72 %. In quiet chromosphere, the contribution of acoustic energy flux to radiative losses is small, only of about 15 %. In active areas with photospheric magnetic field strength between 300 G and 1300 G and inclination of 20-60 degrees, the contribution increases from 23 % (chromospheric network) to 54 % (a plage). However, these values have to be considered as lower limits and it might be possible that the acoustic energy flux is the main contributor to the heating of bright chromospheric network and plages.Comment: 9 pages, 10 figures. Accepted for publication in The Astrophysical Journa

Risk management in solitary agricultural work: new technologies for handling emergency and falls from great heights (SHADE)

Solitary work and agricultural activities are the scenarios of a large number of severe injuries and deaths, also because first aid may be difficult to achieve in isolated locations. This work proposes a technology available on smartphones that allows triggering an emergency call when a fall from height or an unconsciousness state is detected. The results of several tests, which include different detection algorithms and scenarios, are reported in this work. Tests performed with the aid of a dummy have allowed developing a reliable algorithm for the detection of dangerous situations. This system is available as an Android application

Dynamics of the solar atmosphere above a pore with a light bridge

Context: Solar pores are small sunspots lacking a penumbra that have a prevailing vertical magnetic field component. They can include light bridges at places with locally reduced magnetic field. Like sunspots, they exhibit a wide range of oscillatory phenomena. Aims: A large isolated pore with a light bridge (NOAA 11005) is studied to obtain characteristics of a chromospheric filamentary structure around the pore, to analyse oscillations and waves in and around the pore, and to understand the structure and brightness of the light bridge. Methods: Spectral imaging observations in the line Ca II 854.2 nm and complementary spectropolarimetry in Fe I lines, obtained with the DST/IBIS spectrometer and HINODE/SOT spectropolarimeter, were used to measure photospheric and chromospheric velocity fields, oscillations, waves, the magnetic field in the photosphere, and acoustic energy flux and radiative losses in the chromosphere. Results: The chromospheric filamentary structure around the pore has all important characteristics of a superpenumbra: it shows an inverse Evershed effect and running waves, and has a similar morphology and oscillation character. The granular structure of the light bridge in the upper photosphere can be explained by radiative heating. Acoustic waves leaking up from the photosphere along the inclined magnetic field in the light bridge transfer enough energy flux to balance the total radiative losses of the light-bridge chromosphere. Conclusions: The presence of a penumbra is not a necessary condition for the formation of a superpenumbra. The light bridge is heated by radiation in the photosphere and by acoustic waves in the chromosphere.Comment: 14 pages, 14 figures, 3 tables, accepted for publication in Astrononomy & Astrophysic