El rol del Centro de Estudios Estratégicos de Defensa de la Unión de Naciones Suramericanas en la formación de un pensamiento estratégico regional

El presente estudio de caso analiza los aportes del Centro de Estudios Estratégicos de Defensa (CEED) de la Unión de Naciones Suramericanas (Unasur) en la formación de un pensamiento estratégico regional. Cuatro años han transcurrido desde la creación de dicho Centro, por lo que resulta pertinente estudiar sus principales logros y los aportes realizados al Consejo de Defensa Suramericano (CDS) para la formación de un pensamiento estratégico regional en materia de seguridad y defensa.

Seguridad democrática, presencia de la policía y conflicto en Colombia

Este artículo evalúa uno de los componentes fundamentales de la política más icónica del gobierno de Álvaro Uribe: la ´ Seguridad Democrática. En particular, se evalúa el impacto sobre la intensidad del conflicto armado de los despliegues y refuerzos de policía en municipios con poca o nula presencia policial antes de agosto de 2002. Para ello se utiliza el estimador de diferencia en diferencias que compara el cambio en la dinámica del conflicto una vez se asignan los nuevos efectivos a los municipios receptores, relativo al cambio ocurrido simultáneamente en los municipios no receptores. Nuestros resultados sugieren que tanto los despliegues (instauración de inspecciones de policía en municipios que carecían de ´estas) como los refuerzos (envío de nuevos efectivos a municipios con poca presencia policial previa) generan incrementos en el número de ataques guerrilleros. Por otro lado, también hay evidencia que en los casos en los que la asignación de efectivos policiales estuvo acompañada de la movilización de tropas del ejército el conflicto disminuyó en las áreas afectadas, lo que sugiere que la coordinación de las fuerzas armadas resulta clave para el éxito de iniciativas regionales de seguridad.

Hallazgos radiológicos de la enfermedad pulmonar en pacientes Colombianos con esclerodermia

La esclerosis sistémica (ES) es una enfermedad autoinmune multisistémica que afecta principalmente la piel, los pulmones, el tracto gastrointestinal, el corazón y los riñones. La enfermedad pulmonar, presente en casi el 100% de los casos, es el factor con mayor influencia en la mortalidad. El propósito de este estudio es realizar un análisis detallado de la enfermedad pulmonar por tomografía computarizada de alta resolución(TCAR) en pacientes Colombianos con ES, para lo cual se realizó un estudio de prevalencia analítica en 44 pacientes con ES valorados en el Hospital Universitario Mayor Méderi en los últimos 7 años. Los resultados mostraron características demográficas y clínicas similares a las previamente descritas. La prevalencia de enfermedad pulmonar intersticial fue alta, y los hallazgos de fibrosis pulmonar como vidrio esmerilado y panal de abejas se asociaron con la presencia del autoanticuerpo antiSCL70. La medida del diámetro esofágico por TCAR fue mayor en los pacientes con disfagia, antiSCL 70 y linfopenia, los cuales son marcadores de mal pronóstico.

Teaching deaf children how to use telecommunication devices for the deaf

This paper discusses the use of telecommunication devices for the deaf (TDD) and teaching children how to use such devices.

Probing the large-scale topology of the heliospheric magnetic field using Jovian electrons

Jupiter’s magnetosphere acts as a point source of near-relativistic electrons within the heliosphere. In this study, three solar cycles of Jovian electron data in near-Earth space are examined. Jovian electron intensity is found to peak for an ideal Parker spiral connection, but with considerable spread about this point. Assuming the peak in Jovian electron counts indicates the best magnetic connection to Jupiter, we find a clear trend for fast and slow solar wind to be over- and under-wound with respect to the ideal Parker spiral, respectively. This is shown to be well explained in terms of solar wind stream interactions. Thus, modulation of Jovian electrons by corotating interaction regions (CIRs) may primarily be the result of changing magnetic connection, rather than CIRs acting as barriers to cross-field diffusion. By using Jovian electrons to remote sensing magnetic connectivity with Jupiter’s magnetosphere, we suggest that they provide a means to validate solar wind models between 1 and 5 AU, even when suitable in situ solar wind observations are not available. Furthermore, using Jovian electron observations as probes of heliospheric magnetic topology could provide insight into heliospheric magnetic field braiding and turbulence, as well as any systematic under-winding of the heliospheric magnetic field relative to the Parker spiral from footpoint motion of the magnetic field.

Galactic cosmic ray hazard in the unusual extended solar minimum between solar cycle 23 and 24

Galactic cosmic rays (GCRs) are extremely difficult to shield against and pose one of the most severe long-term hazards for human exploration of space. The recent solar minimum between solar cycles 23 and 24 shows a prolonged period of reduced solar activity and low interplanetary magnetic field strengths. As a result, the modulation of GCRs is very weak, and the fluxes of GCRs are near their highest levels in the last 25 years in the fall of 2009. Here we explore the dose rates of GCRs in the current prolonged solar minimum and make predictions for the Lunar Reconnaissance Orbiter (LRO) Cosmic Ray Telescope for the Effects of Radiation (CRaTER), which is now measuring GCRs in the lunar environment. Our results confirm the weak modulation of GCRs leading to the largest dose rates seen in the last 25 years over a prolonged period of little solar activity.

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.

Cone model-based SEP event calculations for applications to multipoint observations

The problem of modeling solar energetic particle (SEP) events is important to both space weather research and forecasting, and yet it has seen relatively little progress. Most important SEP events are associated with coronal mass ejections (CMEs) that drive coronal and interplanetary shocks. These shocks can continuously produce accelerated particles from the ambient medium to well beyond 1 AU. This paper describes an effort to model real SEP events using a Center for Integrated Space weather Modeling (CISM) MHD solar wind simulation including a cone model of CMEs to initiate the related shocks. In addition to providing observation-inspired shock geometry and characteristics, this MHD simulation describes the time-dependent observer field line connections to the shock source. As a first approximation, we assume a shock jump-parameterized source strength and spectrum, and that scatter-free transport occurs outside of the shock source, thus emphasizing the role the shock evolution plays in determining the modeled SEP event profile. Three halo CME events on May 12, 1997, November 4, 1997 and December 13, 2006 are used to test the modeling approach. While challenges arise in the identification and characterization of the shocks in the MHD model results, this approach illustrates the importance to SEP event modeling of globally simulating the underlying heliospheric event. The results also suggest the potential utility of such a model for forcasting and for interpretation of separated multipoint measurements such as those expected from the STEREO mission.

The variation of solar wind correlation lengths over three solar cycles

We present the results of a study of solar wind velocity and magnetic field correlation lengths over the last 35 years. The correlation length of the magnetic field magnitude λ | B| increases on average by a factor of two at solar maxima compared to solar minima. The correlation lengths of the components of the magnetic field λ_{B_{XYZ}} and of the velocity λ_{V_{YZ}} do not show this change and have similar values, indicating a continual turbulent correlation length of around 1.4×106 km. We conclude that a linear relation between λ | B|, VB 2, and Kp suggests that the former is related to the total magnetic energy in the solar wind and an estimate of the average size of geoeffective structures, which is, in turn, proportional to VB 2. By looking at the distribution of daily correlation lengths we show that the solar minimum values of λ | B| correspond to the turbulent outer scale. A tail of larger λ | B| values is present at solar maximum causing the increase in mean value.

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.