Orientalisme, colonialisme i gènere. ‘El Marroc sensual i fanàtic’ d'Aurora Bertrana

Els autors s’endinsen en aquest article en l’estudi de les relacions entre geografia, orientalisme i colonialisme a Europa al tombant del segle passat, tot introduint la perspectiva de gènere i en el marc d'un interès més general per la història del pensament geogràfic contemporani. Ho fan a partir de l’anàlisi contextualitzada d'un text de l’època que fa referència al cas espanyol i a la seva aventura colonial africana. Es tracta del llibre El Marroc sensual i fanàtic (1936) d’Aurora Bertrana, una versió molt elaborada del discurs de la diferència i una bona il•lustració de la literatura de viatges de dones europees, força excepcional i atípica -això sí- en el context literari català i espanyol de l’època

Projecte Comènius a l'IES Aurora Picornell : diversitat a l'escola europea. 'Proyecto Comenius en el IES Aurora Picornell : diversidad en la escuela europea'.

Resumen tomado de la publicación. Incluye tablas de datos e imágenes de las actividades

El programa d'intervenció educativa (PIE) de l'IES Aurora Picornell (2003-2004). 'El programa de intervenció educativa (PIE) del IES Aurora Picornell (2003-2004)'.

Este capítulo forma parte del apartado dedicado a la investigación e innovación pedagógica en las Islas Baleares. Estudio realizado por el Grupo de Investigación y de Formación Educativa y Social (GIFES) del Departamento de Ciencias de la Educación de la Universitat de les Illes Balears. Resumen tomado de la publicación, disponible en castellano y catalán

Aurora Díaz-Plaja : una bibliotecària destacada. 'Aurora Díaz-Plaja : una bibliotecaria destacada'.

Resumen en catalán del autor

R. B. Cunninghame Graham's 'Aurora La Cujiñi' (1898) : an exploration. 'Aurora La Cujiñi (1998) de R. B. Cunninghame Graham : una indagación'.

Resumen en español

La luna y la aurora en poetas del siglo XIX.

Tratamiento que de la luna y la noche hacen los poetas decimonónicos, recurso frecuentemente utilizado en esta época para sus poemas, con muchas finalidades diferentes. Pueden representar a la amada, a la patria, como confidente del poeta, a modo de representación alegórica de inocencia, modestia o castidad, o las diferentes descripciones de la imagen de la luna según el paisaje. También es frecuente entre la poesía del siglo XIX el canto a la aurora, describiéndola de forma colorida, como contrapunto de las descripciones oscuras y azules de la noche, igualmente, es personificada por algunos líricos de la época. El tratamiento de la luna y la aurora refleja la psicología y el estilo de cada poeta.

La Bater??a Aurora : una nueva evaluaci??n de la inteligencia exitosa

Resumen basado en el de la publicaci??n

Aurora Bertrana, una dona extraordinaria

Resumen basado en el de la publicaci??n

Simultaneous observations of reconnection pulses at Cluster and their effects on the cusp aurora seen at Chinese Yellow River Station

While the Cluster spacecraft were located near the high-latitude magnetopause, between 10:10 and 10:40 UT on 16 January 2004, three typical flux transfer event (FTE) signatures were observed. During this interval, simultaneous and conjugated all-sky camera measurements, recorded at Yellow River Station, Svalbard, are available at 630.0 and 557.7nm that show poleward-moving auroral forms (PMAFs), consistent with magnetic reconnection at dayside magnetopause. Simultaneous FTEs seen at the magnetopause mainly move northward, but having duskward (eastward) and tailward velocity components, roughly consistent with the observed direction of motion of the PMAFs in all-sky images. Between the PMAFs meridional keograms, extracted from the all-sky images, show intervals of lower intensity aurora which migrate equatorward just before the PMAFs intensify. This is strong evidence for an equatorward eroding and poleward moving open-closed boundary (OCB) associated with a variable magnetopause reconnection rate under variable IMF conditions. From the durations of the PMAFs we infer that the evolution time of FTEs is 5-11 minutes from its origin on magnetopause to its addition to the polar cap.

Simultaneous observations of reconnection pulses at Cluster and their effects on the cusp aurora observed at the Chinese Yellow River station

While the Cluster spacecraft were located near the high-latitude magnetopause, between 1010 and 1040 UT on 16 January 2004, three typical flux transfer event (FTE) signatures were observed. During this interval, simultaneous and conjugated all‐sky camera measurements, recorded at Yellow River Station, Svalbard, are available at 630.0 and 557.7 nm that show poleward‐moving auroral forms (PMAFs), consistent with magnetic reconnection at the dayside magnetopause. Simultaneous FTEs seen at the magnetopause mainly move northward, but having duskward (eastward) and tailward velocity components, roughly consistent with the observed direction of motion of the PMAFs in all‐sky images. Between the PMAFs meridional keograms, extracted from the all‐sky images, show intervals of lower intensity aurora which migrate equatorward just before the PMAFs intensify. This is strong evidence for an equatorward eroding and poleward moving open‐closed boundary associated with a variable magnetopause reconnection rate under variable IMF conditions. From the durations of the PMAFs, we infer that the evolution time of FTEs is 5–11 minutes from its origin on the magnetopause to its addition to the polar cap.

Do magnetospheric shear Alfvén waves generate sufficient electron energy flux to power the aurora?

Using a self-consistent drift-kinetic simulation code, we investigate whether electron acceleration owing to shear Alfvén waves in the plasma sheet boundary layer is sufficient to cause auroral brightening in the ionosphere. The free parameters used in the simulation code are guided by in situ observations of wave and plasma parameters in the magnetosphere at distances >4 RE from the Earth. For the perpendicular wavelength used in the study, which maps to ∼4 km at 110 km altitude, there is a clear amplitude threshold which determines whether magnetospheric shear Alfvén waves above the classical auroral acceleration region can excite sufficient electrons to create the aurora. Previous studies reported wave amplitudes that easily exceed this threshold; hence, the results reported in this paper demonstrate that auroral acceleration owing to shear Alfvén waves can occur in the magnetosphere at distances >4 RE from the Earth.

Electron trapping in shear Alfvén waves that power the aurora

Results from 1D Vlasov drift-kinetic plasma simulations reveal how and where auroral electrons are accelerated along Earth’s geomagnetic field. In the warm plasma sheet, electrons become trapped in shear Alfven waves, preventing immediate wave damping. As waves move to regions with larger vTe=vA, their parallel electric field decreases, and the trapped electrons escape their influence. The resulting electron distribution functions compare favorably with in situ observations, demonstrating for the first time a self-consistent link between Alfven waves and electrons that form aurora.

Modeling the observed proton aurora and ionospheric convection responses to changes in the IMF clock angle: 2. Persistence of ionospheric convection

We apply a numerical model of time-dependent ionospheric convection to two directly driven reconnection pulses during a 15-min interval of southward IMF on 26 November 2000. The model requires an input magnetopause reconnection rate variation, which is here derived from the observed variation in the upstream IMF clock angle, q. The reconnection rate is mapped to an ionospheric merging gap, the MLT extent of which is inferred from the Doppler-shifted Lyman-a emission on newly opened field lines, as observed by the FUV instrument on the IMAGE spacecraft. The model is used to reproduce a variety of features observed during this event: SuperDARN observations of the ionospheric convection pattern and transpolar voltage; FUV observations of the growth of patches of newly opened flux; FUVand in situ observations of the location of the Open-Closed field line Boundary (OCB) and a cusp ion step. We adopt a clock angle dependence of the magnetopause reconnection electric field, mapped to the ionosphere, of the form Enosin4(q/2) and estimate the peak value, Eno, by matching observed and modeled variations of both the latitude, LOCB, of the dayside OCB (as inferred from the equatorward edge of cusp proton emissions seen by FUV) and the transpolar voltage FPC (as derived using the mapped potential technique from SuperDARN HF radar data). This analysis also yields the time constant tOCB with which the open-closed boundary relaxes back toward its equilibrium configuration. For the case studied here, we find tOCB = 9.7 ± 1.3 min, consistent with previous inferences from the observed response of ionospheric flow to southward turnings of the IMF. The analysis confirms quantitatively the concepts of ionospheric flow excitation on which the model is based and explains some otherwise anomalous features of the cusp precipitation morphology.

Modeling the observed proton aurora and ionospheric convection responses to changes in the IMF clock angle: 1. Persistence of cusp proton aurora

We employ a numerical model of cusp ion precipitation and proton aurora emission to fit variations of the peak Doppler-shifted Lyman-a intensity observed on 26 November 2000 by the SI-12 channel of the FUV instrument on the IMAGE satellite. The major features of this event appeared in response to two brief swings of the interplanetary magnetic field (IMF) toward a southward orientation. We reproduce the observed spatial distributions of this emission on newly opened field lines by combining the proton emission model with a model of the response of ionospheric convection. The simulations are based on the observed variations of the solar wind proton temperature and concentration and the interplanetary magnetic field clock angle. They also allow for the efficiency, sampling rate, integration time and spatial resolution of the FUV instrument. The good match (correlation coefficient 0.91, significant at the 98% level) between observed and modeled variations confirms the time constant (about 4 min) for the rise and decay of the proton emissions predicted by the model for southward IMF conditions. The implications for the detection of pulsed magnetopause reconnection using proton aurora are discussed for a range of interplanetary conditions.