Guía metodológica para el desarrollo de planes de competitividad territorial

La tesis presenta una guía metodológica de cómo desarrollar Planes / Agendas de Competitividad a nivel Territorial, basado en experiencias nacionales e internacionales. Se inicia con una exposición de temas conceptuales de Competitividad, en general y a nivel Meso, al igual que de Desarrollo Económico Local, como antecedentes del tema de Tesis. Posteriormente se presenta algunas prácticas de Planes de Competitividad Territorial, haciendo énfasis en los puntos en común de cómo fueron logradas. Por último, se hace una propuesta metodológica a seguirse para la consecución de una Agenda de Competitividad Local.

La metodología Balanced ScoreCard como herramienta de evaluación de los planes estratégicos organizacionales. Estudio de Caso: Corporación Financiera Nacional, Plan estratégico 2006-2008

El propósito de la presente investigación es el de analizar la aplicación del Balanced Scorecard como herramienta de evaluación de los planes estratégicos de la Corporación Financiera Nacional, específicamente para las principales líneas de negocio (crédito y fiducia) además de diseñar un Cuadro de Mando Integral para evaluar los objetivos estratégicos de dichas líneas de negocio incluidos en el Plan Estratégico 2006-2008 de la institución. Durante el desarrollo de la presente investigación, se abordan temas relacionados tanto con la parte teórica, en lo que concierne a la parte conceptual y metodológica del Balanced Scorecard, como ámbitos de la parte empírica en los que se destacan el análisis de la forma de evaluación actual del plan estratégico de la CFN y específicamente del crédito y fiducia determinando sus fortalezas y debilidades. La evaluación conceptual previa, así como el diagnóstico del monitoreo actual del Plan Estratégico de la CFN, permitieron estructurar un mapa estratégico, en donde se evidencien las principales líneas de negocio. Se seleccionaron también los mejores indicadores para los cuatro ámbitos del BSC para el crédito y negocios fiduciarios. Finalmente y en forma complementaria al diseño del Cuadro de Mando Integral de la CFN, se elaboró un demo que presenta los principales resultados en torno a los indicadores identificados.

Incidencia del aprendizaje en los planes de carrera en una empresa de software. Caso de Structured Intelligente

A través de esta investigación se buscó establecer la relación existente entre el aprendizaje y el plan de carrera en una organización real; y lograr una propuesta viable para la empresa y sus empleados sobre estos temas. El estudio está basado en una revisión de aspectos teóricos de forma bibliografía, y se incorporó la revisión de entrevistas, encuestas y observación para el análisis de la situación actual y deseada. Al realizar el estudio se determinaron tres apoyos importantes que sirven a la empresa para la obtención de sus objetivos estratégicos, los cuales son competencias, conocimientos y planes de carrera. El resultado fue las propuestas de gestión por competencias, gestión del conocimiento y planes de carrera, alineadas a la propuesta de planificación estratégica para la empresa Structured Intelligente del Ecuador S.A. Concluyendo que el aprendizaje incide directamente sobre los planes de carrera.

Gestión de riesgo operativo: diseño de una metodología para su identificación y propuesta de planes de acción en cooperativas de ahorro y crédito no reguladas, miembros de una organización representativa

La decisión de abordar como tema de tesis la “Gestión de riesgo operativo: diseño de una metodología para su identificación y propuesta de planes de acción en cooperativas de ahorro y crédito no reguladas miembros de una organización representativa”, responde a la preocupación, cada vez más acuciante, de que las cooperativas dispongan de una metodología de identificación de riesgo operativo para reducir posibles pérdidas resultantes de una mala gestión en factores de riesgo, tales como: procesos, políticas, personas, tecnología de información y eventos externos. El estudio se inicia con la revisión de varias fuentes bibliográficas dirigidas a reforzar conocimientos y conceptos, así como a lograr una definición más acertada del contexto. Se completa con una investigación de campo realizada en cuatro cooperativas de tres provincias, seleccionadas por su apertura para participar. El período estudiado fue 2006 – 2010. La recolección de la información se realizó a través de encuestas a los gerentes y directivos, entrevistas al personal operativo y observación de campo. Con los datos obtenidos, se procedió a identificar procesos gobernantes, operativos y de apoyo; y, se levantaron macroprocesos, procesos, subprocesos y actividades del proceso de ventanilla y crédito; para posteriormente identificar los riesgos en cada una de las actividades con el impacto y la probabilidad. De esta forma se aporta con un plan de acción recomendado para prevenir eventos de riesgo. Se concluye afirmando que todas las organizaciones del sector financiero popular y solidario están obligadas, no por Ley, sino por estrategia de seguridad, a gestionar riesgo operativo, como una prioridad ineludible, que no debe limitarse a crear un departamento o área de riesgos, sino creando y desarrollando una verdadera “cultura de riesgo”, como parte de una planificación integral de la entidad, que se la trabaje todos los días.

La discriminación en el derecho a la educación en niños/as con cáncer en Ecuador: situación actual y aspectos a considerar en planes educativos y de salud

La situación que presentan niños/as con cáncer en Ecuador y sus dificultades en el ejercicio del Derecho a la Educación no es un fenómeno nuevo. Desde el año 2009 diversos planes y políticas institucionales han intentado generar una protección de situaciones de vulneración. No obstante, un análisis de la situación posibilita evidenciar que hay desprotección en el ámbito de la educación y ausencia de coordinación entre políticas educativas y de salud. De esta manera, el desarrollo de este trabajo tiene como finalidad aportar en la visibilización en el Ecuador de un fenómeno que se caracteriza por la escasez de estudios, estadísticas y programas de intervención. Para este objetivo, se analizan diversas normativas y referencias sobre la materia en Ecuador y, además, se realiza un grupo focal con padres, madres y abuelas de niños con cáncer. Se concluye que el acceso y ejercicio al derecho a la educación en niños/as con enfermedades catastróficas requiere de la modificación de disposiciones educativas que dificultan este ejercicio y de la conexión entre diversas instituciones estatales. Es indispensable capacitar a toda la comunidad educativa así como desarrollar equipos interdisciplinarios que aborden adecuadamente las necesidades especiales de estos niños.

Observational evidence of a coronal mass ejection distortion directly attributable to a structured solar wind

We present the first observational evidence of the near-Sun distortion of the leading edge of a coronal mass ejection (CME) by the ambient solar wind into a concave structure. On 2007 November 14, a CME was observed by coronagraphs onboard the STEREO-B spacecraft, possessing a circular cross section. Subsequently the CME passed through the field of view of the STEREO-B Heliospheric Imagers where the leading edge was observed to distort into an increasingly concave structure. The CME observations are compared to an analytical flux rope model constrained by a magnetohydrodynamic solar wind solution. The resultant bimodal speed profile is used to kinematically distort a circular structure that replicates the initial shape of the CME. The CME morphology is found to change rapidly over a relatively short distance. This indicates an approximate radial distance in the heliosphere where the solar wind forces begin to dominate over the magnetic forces of the CME influencing the shape of the CME.

Impact of coronal mass ejections, interchange reconnection, and disconnection on heliospheric magnetic field strength

An update of Owens et al. (2008) shows that the relationship between the coronal mass ejection (CME) rate and the heliospheric magnetic field strength predicts a field floor of less than 4 nT at 1 AU. This implies that the record low values measured during this solar minimum do not necessarily contradict the idea that open flux is conserved. The results are consistent with the hypothesis that CMEs add flux to the heliosphere and interchange reconnection between open flux and closed CME loops subtracts flux. An existing model embracing this hypothesis, however, overestimates flux during the current minimum, even though the CME rate has been low. The discrepancy calls for reasonable changes in model assumptions.

The radial width of a coronal mass ejection between 0.1 and 0.4 AU estimated from the heliospheric imager on STEREO

On 15-17 February 2008, a CME with an approximately circular cross section was tracked through successive images obtained by the Heliospheric Imager (HI) instrument onboard the STEREO-A spacecraft. Reasoning that an idealised flux rope is cylindrical in shape with a circular cross-section, best fit circles are used to determine the radial width of the CME. As part of the process the radial velocity and longitude of propagation are determined by fits to elongation-time maps as 252±5 km/s and 70±5° respectively. With the longitude known, the radial size is calculated from the images, taking projection effects into account. The radial width of the CME, S (AU), obeys a power law with heliocentric distance, R, as the CME travels between 0.1 and 0.4 AU, such that S=0.26 R0.6±0.1. The exponent value obtained is compared to published studies based on statistical surveys of in situ spacecraft observations of ICMEs between 0.3 and 1.0 AU, and general agreement is found. This paper demonstrates the new opportunities provided by HI to track the radial width of CMEs through the previously unobservable zone between the LASCO field of view and Helios in situ measurements.

Role of coronal mass ejections in the heliospheric Hale cycle

The 11-year solar cycle variation in the heliospheric magnetic field strength can be explained by the temporary buildup of closed flux released by coronal mass ejections (CMEs). If this explanation is correct, and the total open magnetic flux is conserved, then the interplanetary-CME closed flux must eventually open via reconnection with open flux close to the Sun. In this case each CME will move the reconnected open flux by at least the CME footpoint separation distance. Since the polarity of CME footpoints tends to follow a pattern similar to the Hale cycle of sunspot polarity, repeated CME eruption and subsequent reconnection will naturally result in latitudinal transport of open solar flux. We demonstrate how this process can reverse the coronal and heliospheric fields, and we calculate that the amount of flux involved is sufficient to accomplish the reversal within the 11 years of the solar cycle.

Coronal mass ejections and magnetic flux buildup in the heliosphere

To test for magnetic flux buildup in the heliosphere from coronal mass ejections (CMEs), we simulate heliospheric flux as a constant background open flux with a time-varying interplanetary CME (ICME) contribution. As flux carried by ejecta can only contribute to the heliospheric flux budget while it remains closed, the ICME flux opening rate is an important factor. Two separate forms for the ICME flux opening rate are considered: (1) constant and (2) exponentially decaying with time. Coronagraph observations are used to determine the CME occurrence rates, while in situ observations are used to estimate the magnetic flux content of a typical ICME. Both static equilibrium and dynamic simulations, using the constant and exponential ICME flux opening models, require flux opening timescales of ∼50 days in order to match the observed doubling in the magnetic field intensity at 1 AU over the solar cycle. Such timescales are equivalent to a change in the ICME closed flux of only ∼7–12% between 1 and 5 AU, consistent with CSE signatures; no flux buildup results. The dynamic simulation yields a solar cycle flux variation with high variability that matches the overall variability of the observed magnetic field intensity remarkably well, including the double peak forming the Gnevyshev gap.

On the evolution of the solar wind between 1 and 5 AU at the time of the Cassini Jupiter flyby: Multispacecraft observations of interplanetary coronal mass ejections including the formation of a merged interaction region

The Cassini flyby of Jupiter occurred at a time near solar maximum. Consequently, the pre-Jupiter data set reveals clear and numerous transient perturbations to the Parker Spiral solar wind structure. Limited plasma data are available at Cassini for this period due to pointing restrictions imposed on the instrument. This renders the identification of the nature of such structures ambiguous, as determinations based on the magnetic field data alone are unreliable. However, a fortuitous alignment of the planets during this encounter allowed us to trace these structures back to those observed previously by the Wind spacecraft near the Earth. Of the phenomena that we are satisfactorily able to trace back to their manifestation at 1 AU, two are identified as being due to interplanetary coronal mass ejections. One event at Cassini is shown to be a merged interaction region, which is formed from the compression of a magnetic cloud by two anomalously fast solar wind streams. The flux-rope structure associated with this magnetic cloud is not as apparent at Cassini and has most likely been compressed and deformed. Confirmation of the validity of the ballistic projections used here is provided by results obtained from a one-dimensional magnetohydrodynamic projection of solar wind parameters measured upstream near the Earth. It is found that when the Earth and Cassini are within a few tens of degrees in heliospheric longitude, the results of this one-dimensional model predict the actual conditions measured at 5 AU to an impressive degree. Finally, the validity of the use of such one-dimensional projections in obtaining quasi-solar wind parameters at the outer planets is discussed.

Non-radial solar wind flows induced by the motion of interplanetary coronal mass ejections

A survey of the non-radial flows (NRFs) during nearly five years of interplanetary observations revealed the average non-radial speed of the solar wind flows to be �30 km/s, with approximately one-half of the large (>100 km/s) NRFs associated with ICMEs. Conversely, the average non-radial flow speed upstream of all ICMEs is �100 km/s, with just over one-third preceded by large NRFs. These upstream flow deflections are analysed in the context of the large-scale structure of the driving ICME. We chose 5 magnetic clouds with relatively uncomplicated upstream flow deflections. Using variance analysis it was possible to infer the local axis orientation, and to qualitatively estimate the point of interception of the spacecraft with the ICME. For all 5 events the observed upstream flows were in agreement with the point of interception predicted by variance analysis. Thus we conclude that the upstream flow deflections in these events are in accord with the current concept of the large scale structure of an ICME: a curved axial loop connected to the Sun, bounded by a curved (though not necessarily circular)cross section.

Predictions of the arrival time of coronal mass ejections at 1AU: an analysis of the causes of errors

Three existing models of Interplanetary Coronal Mass Ejection (ICME) transit between the Sun and the Earth are compared to coronagraph and in situ observations: all three models are found to perform with a similar level of accuracy (i.e. an average error between observed and predicted 1AU transit times of approximately 11 h). To improve long-term space weather prediction, factors influencing CME transit are investigated. Both the removal of the plane of sky projection (as suffered by coronagraph derived speeds of Earth directed CMEs) and the use of observed values of solar wind speed, fail to significantly improve transit time prediction. However, a correlation is found to exist between the late/early arrival of an ICME and the width of the preceding sheath region, suggesting that the error is a geometrical effect that can only be removed by a more accurate determination of a CME trajectory and expansion. The correlation between magnetic field intensity and speed of ejecta at 1AU is also investigated. It is found to be weak in the body of the ICME, but strong in the sheath, if the upstream solar wind conditions are taken into account.

Characteristic magnetic field and speed properties of interplanetary coronal mass ejections and their sheath regions

Prediction of the solar wind conditions in near-Earth space, arising from both quasi-steady and transient structures, is essential for space weather forecasting. To achieve forecast lead times of a day or more, such predictions must be made on the basis of remote solar observations. A number of empirical prediction schemes have been proposed to forecast the transit time and speed of coronal mass ejections (CMEs) at 1 AU. However, the current lack of magnetic field measurements in the corona severely limits our ability to forecast the 1 AU magnetic field strengths resulting from interplanetary CMEs (ICMEs). In this study we investigate the relation between the characteristic magnetic field strengths and speeds of both magnetic cloud and noncloud ICMEs at 1 AU. Correlation between field and speed is found to be significant only in the sheath region ahead of magnetic clouds, not within the clouds themselves. The lack of such a relation in the sheaths ahead of noncloud ICMEs is consistent with such ICMEs being skimming encounters of magnetic clouds, though other explanations are also put forward. Linear fits to the radial speed profiles of ejecta reveal that faster-traveling ICMEs are also expanding more at 1 AU. We combine these empirical relations to form a prediction scheme for the magnetic field strength in the sheaths ahead of magnetic clouds and also suggest a method for predicting the radial speed profile through an ICME on the basis of upstream measurements.