La masa no se crea ni se destruye ¿Estáis seguros?

From the very outset of the study of chemistry, the concepts of mass, physical and chemical transformations of matter and the law of conservation are fundamental. However, in reality, the learning of these concepts that pupils believe they understand is not very secure. When they try to apply their ideas to simple questions they make mistakes and the reasoning they use does not correspond to the explanations or definitions that they are able to repeat

Dificultades en la enseñanza-aprendizaje de los problemas de física y química : I. Opiniones del alumno

Analysing the ideas with which teachers and pupils confront problems in physics and chemistry. The starting point for this analysis is the compilation of the difficulties and causes of failure involved in solving problems raised during a didactic investigation of these subjects. This part shows the results obtained in relation to the pupils. They show their opinions on the difficulties they came across, their evaluations, relationships between these and other groups of students showing similar characteristics. Another paper will be dedicated to the teacher's opinions and a comparison between both groups

Dificultades en la enseñanza-aprendizaje de los problemas de física y química : II. Opiniones del profesor

Analysing the ideas with which teachers and pupils confront problems in physics and chemistry. The starting point for this analysis is the compilation of difficulties and causes of failure involved in solving problems raised in a didactic investigation of the subjects. This second part -referring to the teachers- shows the relationships between difficulties faced as well as distinguishing between groups of teachers who share similar ideas about problem solving education. Finally a comparison is made between the two sections -teachers and pupils- with implications to teaching and learning

Clues on Regularity in the Structure and Kinematics of Elliptical Galaxies from Self-consistent Hydrodynamical Simulations: the Dynamical Fundamental Plane

[Abridged] We have analysed the parameters characterising the mass, size and velocity dispersion both at the baryonic scale and at the halo scales of two samples of relaxed elliptical-like-objects (ELOs) identified, at z=0, in a set of self-consistent hydrodynamical simulations operating in the context of a concordance cosmological model. At the halo scale they have been found to satisfy virial relations; at the scale of the baryonic object the (logarithms of the) ELO stellar masses, projected stellar half-mass radii, and stellar central l.o.s. velocity dispersions define a flattened ellipsoid close to a plane (the intrinsic dynamical plane, IDP), tilted relative to the virial one, whose observational manifestation is the observed FP. The ELO samples have been found to show systematic trends with the mass scale in both, the relative content and the relative distributions of the baryonic and the dark mass ELO components, so that homology is broken in the spatial mass distribution (resulting in the IDP tilt), but ELOs are still a two-parameter family where the two parameters are correlated. The physical origin of these trends presumably lies in the systematic decrease, with increasing ELO mass, of the relative amount of dissipation experienced by the baryonic mass component along ELO stellar mass assembly. ELOs also show kinematical segregation, but it does not appreciably change with the mass scale. The non-homogeneous population of IDPs explains the role played by the virial mass to determine the correlations among intrinsic parameters. In this paper we also show that the central stellar line-of-sight velocity dispersion of ELOs, is a fair empirical estimator of the virial mass, and this explains the central role played by this quantity at determining the observational correlations.Comment: 20 pages, 17 Figures. Only changed to a more readable styl

The Lack of Structural and Dynamical Evolution of Elliptical Galaxies since z ~ 1.5: Clues from Self-Consistent Hydrodynamical Simulations

We present results of a study on the evolution of the parameters characterizing the structure and dynamics of the relaxed elliptical-like objects (ELOs) identified at z=0, z=1 and z=1.5 in a set of hydrodynamical, self-consistent simulations operating in the context of a concordance cosmological model. The values of the stellar mass, the stellar half-mass radius and the stellar mean-square velocity have been measured in each ELO and found to populate, at any z, a flattened ellipsoid close to a plane (the dynamical plane, DP). Our simulations indicate that, at the intermediate zs considered, individual ELOs evolve, increasing the values of these parameters as a consequence of on-going mass assembly, but, nevertheless, their DP is roughly preserved within its scatter, in agreement with observations of the Fundamental Plane of ellipticals at different zs. We briefly discuss how this lack of significant dynamical and structural evolution in ELO samples arises, in terms of the two different phases operating in the mass aggregation history of their dark matter halos. According with our simulations, most dissipation involved in ELO formation takes place at the early violent phase, causing the stellar mass, the stellar half-mass radius and the stellar mean-square velocity parameters to settle down to the DP, and, moreover, the transformation of most of the available gas into stars. In the subsequent slow phase, ELO stellar mass growth preferentially occurs through non-dissipative processes, so that the DP is preserved and the ELO star formation rate considerably decreases. These results hint, for the first time, to a possible way of explaining, in the context of cosmological simulations, different apparently paradoxical observational results on ellipticals.Comment: 12 pages, 1 figure. Minor changes to match the published versio

Large-scale gas dynamics in the adhesion model: Implications for the two-phase massive galaxy formation scenario

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 RAS © 2011 The AuthorsPublished by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedWe have studied the mass assembly and star formation histories of massive galaxies identified at low redshift in different cosmological hydrodynamical simulations. To this end, we have carried out a detailed follow-up backwards in time of their constituent mass elements (sampled by particles) of different types. After that, the configurations they depict at progressively higher zs were carefully analysed. The analyses show that these histories share common generic patterns, irrespective of particular circumstances. In any case, however, the results we have found are different depending on the particle type. The most outstanding differences follow. We have found that by z∼ 3.5-6, mass elements identified as stellar particles at z= 0 exhibit a gaseous cosmic-web-like morphology with scales of ∼1 physical Mpc, where the densest mass elements have already turned into stars by z∼ 6. These settings are in fact the densest pieces of the cosmic web, where no hot particles show up, and dynamically organized as a hierarchy of flow convergence regions (FCRs), that is, attraction basins for mass flows. At high z FCRs undergo fast contractive deformations with very low angular momentum, shrinking them violently. Indeed, by z∼ 1 most of the gaseous or stellar mass they contain shows up as bound to a massive elliptical-like object at their centres, with typical half-mass radii of rmass star∼ 2-3kpc. After this, a second phase comes about where the mass assembly rate is much slower and characterized by mergers involving angular momentum. On the other hand, mass elements identified at the diffuse hot coronae surrounding massive galaxies at z= 0 do not display a clear web-like morphology at any z. Diffuse gas is heated when FCRs go through contractive deformations. Most of this gas remains hot and with low density throughout the evolution. To shed light on the physical foundations of the behaviour revealed by our analyses (i.e. a two-phase formation process with different implications for diffuse or shocked mass elements), as well as on their possible observational implications, these patterns have been confronted with some generic properties of singular flows as described by the adhesion model (i.e. potential character of the velocity field, singular versus regular points, dressing, locality when a spectrum of perturbations is implemented). We have found that the common patterns the simulations show can be interpreted as a natural consequence of flow properties that, moreover, could explain different generic observational results from massive galaxies or their samples. We briefly discuss some of themThis work was partially supported by the DGES (Spain) through the grants AYA2009-12792-C03-02 and AYA2009-12792- C03-03 from the PNAyA, as well as by the regional Madrid V PRICIT programme through the ASTROMADRID network (CAM S2009/ESP-1496

Shape and kinematics of elliptical galaxies: evolution due to merging at z < 1.5

[EN]Aims. We investigate the evolution in the shape and kinematics of elliptical galaxies in a cosmological framework. Methods. We identified relaxed, elliptical-like objects (ELOs) at redshifts z = 0, z = 0.5, z = 1 and z = 1.5 within a set of hydrodynamic, self-consistent simulations completed for a concordance cosmological model. Results. The population of elliptical systems that we analysed evolve systematically with time becoming rounder in general by z = 0 and also more velocity dispersion supported. We found that this is due primarily to major dry mergers where only a modest amount of angular momentum is involved in the merger event. Despite the general trend, in a significant number of cases the merger event involves a relatively high amount of specific angular momentum, which causes the system in general to acquire higher rotational support and/or a more oblate shape. These evolutionary patterns persist when we study our systems in projection, in simulating true observations, and thus should be evident in future observations.Peer reviewe

Amputación Pirogoff modificada aplicada a la cirugía oncológica del pie

Los sarcomas óseos y de tejidos blandos del pie son infrecuentes, representando menos del 10% de todos los sarcomas de la extremidad inferior. El tratamiento más frecuente de los sarcomas del pie es la amputación por debajo de la rodilla, debido a la imposibilidad de conseguir márgenes amplios, pero en determinados casos de tumores del antepié se puede optar por una amputación parcial del pie con margen amplio. Se presenta una serie de tres casos de amputación de Pirogoff modificada aplicada a la resección oncológica tumoral. La amputación de Pirogoff consiste en una artrodesis calcaneotibial con resección del astrágalo, rotando el calcáneo 90°. La modificación de la técnica de amputación del Pirogoff, en la que se conservan ambos maléolos con escisión de la carilla articular favorece la estabilidad en el plano lateral y ayuda a una más rápida artrodesis. Es muy importante mantener los principios oncológicos de la resección tumoral.Bone and soft-tissue sarcomata of the foot are infrequent neoplasms, representing less than 10% of all lower limb sarcomata. The most frequent therapeutic measure for foot sarcomata is amputation below the knee, due to the difficulty to achieve ample (onco-)-surgical margins, yet in a number of cases of forefoottumours there is an option for partial foot amputation with ample surgical margins. We report a series of three cases of modified Pirogoff's amputation as applied to oncosurgical tumour resection. Pirogoff's amputation is a calcaneo-tibial arthrodesis with resection of the talus and 90° rotation of the calcaneus. The here reported modification of the Pirogoff amputation, in which both malleoli are preserved yet with excision of the articular surface, favours lateral-plane stability and promotes a quicker arthrodesis. It is highly important to observe and maintain the oncologic surgery principles for tumour resection

Clues on the Physical Origin of the Fundamental Plane from Self-consistent Hydrodynamical Simulations

We report on a study of the parameters characterizing the mass and velocity distributions of two samples of relaxed elliptical-like objects (ELOs) identified, at z=0, in a set of self-consistent hydrodynamical simulations operating in the context of a concordance cosmological model. Star formation (SF) has been phenomenologically implemented in the simulations in the framework of the turbulent sequential scenario through a threshold gas density and an efficiency parameter. Each ELO sample is characterized by the values these parameters take. We have found that the (logarithms of the) ELO stellar masses, projected stellar half-mass radii, and stellar central line-of-sight (LOS) velocity dispersions define dynamical fundamental planes (FPs). Zero points depend on the particular values that the SF parameters take, while slopes do not change. The ELO samples have been found to show systematic trends with the mass scale in both the relative content and the relative distributions of the baryonic and the dark mass ELO components. The physical origin of these trends lies in the systematic decrease, with increasing ELO mass, of the relative dissipation experienced by the baryonic mass component along ELO mass assembly, resulting in a tilt of the dynamical FP relative to the virial plane. The dynamical FPs shown by the two ELO samples are consistent with that shown by the SDSS elliptical sample in the same variables, with no further need for any relevant contribution from stellar population effects to explain the observed tilt. These effects could, however, have contributed to the scatter of the observed FP, as the dynamical FPs have been found to be thinner than the observed one. The results we report on hint, for the first time, at a possible way to understand the tilt of the observed FP in a cosmological context.Comment: 12 pages, 1 figure. Accepted to Astrophysical Journal Letter