Spatial Demultiplexing in the sub-millimeter wave band using multlayer free-standing frequency selective surfaces

In this paper, we show that a multilayer freestanding slot array can be designed to give an insertion loss which is significantly lower than the value obtainable from a conventional dielectric backed printed frequency selective surface (FSS). This increase in filter efficiency is highlighted by comparing the performance of two structures designed to provide frequency selective beamsplitting in the quasioptical feed train of a submillimeter wave space borne radiometer. A two layer substrateless FSS providing more than 20 dB of isolation between the bands 316.5â??325.5 GHz and 349.5â??358.5 GHz, gives an insertion loss of 0.6 dB when the filter is orientated at 45 incidence in the TM plane, whereas the loss exhibited by a conventional printed FSS is in excess of 2 dB. A similar frequency response can be obtained in the TE plane, but here a triple screen structure is required and the conductor loss is shown to be comparable to the absorption loss of a dielectric backed FSS. Experimental devices have been fabricated using a precision micromachining technique. Transmission measurements performed in the range 250â??360 GHz are in good agreement with the simulated spectral performance of the individual periodic screens and the two multilayer freestanding FSS structures.

Micromachined 300GHz high Q resonant slot frequency selective surface filter

The design of a low loss quasi-optical beam splitter which is required to provide efficient diplexing of the bands 316.5-325.5 GHz and 349.5-358.5 GHz is presented. To minimise the filter insertion loss, the chosen architecture is a three-layer freestanding array of dipole slot elements. Floquet modal analysis and finite element method computer models are used to establish the geometry of the periodic structure and to predict its spectral response. Two different micromachining approaches have been employed to fabricate close packed arrays of 460 mm long elements in the screens that form the basic building block of the 30mm diameter multilayer frequency selective surface. Comparisons between simulated and measured transmission coefficients for the individual dichroic surfaces are used to determine the accuracy of the computer models and to confirm the suitability of the fabrication methods.

Effective collision strengths for transitions in Fe XV

Collision strengths for transitions among the energetically lowest 53 fine-structure levels belonging to the (1s(2)2s(2)2p(6)) 3l(2), 3l3l', 3s4l and 3p4s configurations of Fe XV are computed, over an electron energy range below 160 Ryd, using the Dirac Atomic R-matrix Code (DARC) of Norrington & Grant (2003). Effective collision strengths, obtained after integrating the collision strengths over a Maxwellian distribution of electron energies, have also been calculated. These results of effective collision strengths are tabulated for all 1378 inelastic transitions over a wide temperature range of 10(5) to 10(7) K. Comparisons are also made with other R-matrix calculations and the accuracy of the results is assessed.

SiIX emission lines in spectra obtained with the Solar EUV Research Telescope and Spectrograph (SERTS)

Theoretical electron-density-sensitive emission line ratios involving 2s(2)2p(2)-2s2p(3) transitions in Si IX between 223 and 350 Angstrom are presented. A comparison of these with an extensive dataset of solar-active-region, quiet-Sun, subflare and off-limb observations, obtained during rocket flights by the Solar EUV Research Telescope and Spectrograph (SERTS), reveals generally very good agreement between theory and experiment. This provides support for the accuracy of the line- ratio diagnostics, and hence the atomic data on which they are based. In particular, the density-sensitive intensity ratio I (258.10 Angstrom)/ I (349.87 Angstrom) offers an especially promising diagnostic for studies of coronal plasmas, as it involves two reasonably strong emission lines and varies by more than an order of magnitude over the useful density range of 10(9)-10(11) cm(-3). The 2s(2)2p(2) S-1(0) - 2s2p(3) P-1(1) transition at 259.77 Angstrom is very marginally identified for the first time in the SERTS database, although it has previously been detected in solar flare observations.

A comparison of theoretical MgVI emission line strengths with active-region observations from serts

R-matrix calculations of electron impact excitation rates in N-like Mg vi are used to derive theoretical electron-density-sensitive emission line ratios involving 2s(2)2p(3)-2s2p(4) transitions in the 269-403 Angstrom wavelength range. A comparison of these with observations of a solar active region, obtained during the 1989 flight of the Solar EUV Rocket Telescope and Spectrograph (SERTS), reveals good agreement between theory and observation for the 2s(2)2p(3) S-4-2s2p(4) P-4 transitions at 399.28, 400.67, and 403.30 Angstrom, and the 2s(2)2p(3) P-2-2s2p(4) D-2 lines at 387.77 and 387.97 Angstrom. However, intensities for the other lines attributed to Mg vi in this spectrum by various authors do not match the present theoretical predictions. We argue that these discrepancies are not due to errors in the adopted atomic data, as previously suggested, but rather to observational uncertainties or mis-identifications. Some of the features previously identified as Mg vi lines in the SERTS spectrum, such as 291.36 and 293.15 Angstrom, are judged to be noise, while others (including 349.16 Angstrom) appear to be blended.

Early-type stars in the Galactic halo from the Palomar-Green survey - III. Completion of a magnitude range limited sample

High-resolution (R approximate to 40 000) echelle spectroscopic observations of 13 high-latitude early-type stars are presented. These stars comprise the final part of a complete magnitude range limited sample based on low-resolution spectroscopy of targets drawn from the Palomar-Green survey. The magnitude range under consideration is 13 less than or equal to B-PG less than or equal to 14.6, corresponding to an approximate distance limit for main-sequence B-type objects of 5 less than or equal to d less than or equal to 40 kpc. Three stars are found to be apparently normal, young stars, based on their positions on the (T-eff, log g) diagram, normal abundance patterns and relatively large projected rotational velocities. A further star, PG 1209+263, was found to belong to the chemically peculiar (CP) silicon star class of objects. The remainder are evolved subluminous stars lying on post- horizontal branch (post-HB) tracks, with the exception of PG 2120+062, which appears to be in a post-asymptotic giant branch evolutionary stage. For the young stars in the sample, we have derived distance and age estimates through comparison of the atmospheric parameters with recent theoretical evolutionary models. We discuss formation scenarios by comparing times-of- flight and evolutionary time-scales. It is found that all stars could have formed in the Galactic disc and been ejected from there soon after their birth, with the exception of PG 1209+263. The adopted proper motion is found to be a crucial factor in the kinematical analysis. We also present some number densities for young B-type halo stars, which indicate that they are extremely scarce objects.

Time signatures of impulsively generated coronal fast wave trains

Impulsively generated short-period fast magneto-acoustic wave trains, guided by solar and stellar coronal loops, are numerically modelled. In the developed stage of the evolution, the wave trains have a characteristic quasi-periodic signature. The quasi-periodicity results from the geometrical dispersion of the guided fast modes, determined by the transverse profile of the loop. A typical feature of the signature is a tadpole wavelet Spectrum: a narrow-spectrum tail precedes a broad-band head. The instantaneous period of the oscillations in the wave train decreases gradually with time. The period and the spectral amplitude evolution are shown to be determined by the steepness of the transverse density profile and the density contrast ratio in the loop. The propagating wave trains recently discovered with the Solar Eclipse Coronal Imaging System (SECIS) instrument are noted to have similar wavelet spectral features, which strengthens the interpretation of SECIS results as guided fast wave trains.

The (in)visible scar. Representation of the body in blogs by women with breast cancer

In this paper we analyze the representation of the body in blogs by women with breast cancer. Taking into account both texts and images, we study the representation of the body on the basis of the body problems proposed by Frank (1995): control, body-relatedness, other-relatedness and desire. In the blogs studied we find a desiring and dyadic body, which is understood as part of a network of affection and care. The diagnosis of cancer can generate both dissociation, when the body is experienced as a threat, and association, a wish to be connected to it. In relation to control, a clear will of predictability is observed but traces of assumption of contingency also appear.

A comparative study of the synthesis of 3-substituted catechols using an enzymatic and a chemoenzymatic method

A series of cis-dihydrodiol metabolites, available from the bacterial dioxygenase-catalysed oxidation of monosubstituted benzene substrates using Pseudomonas putida UV4, have been converted to the corresponding catechols using both a heterogeneous catalyst (Pd/C) and a naphthalene cis-diol dehydrogenase enzyme present in whole cells of the recombinant strain Escherichia coli DH5 alpha(pUC129: nar B). A comparative study of the merits of both routes to 3-substituted catechols has been carried out and the two methods have been found to be complementary. A similarity in mechanism for catechol formation under both enzymatic and chemoenzymatic conditions, involving regioselective oxidation of the hydroxyl group at C-1, has been found using deuterium labelled toluene cis-dihydrodiols. The potential, of combining a biocatalytic step (dioxygenase-catalysed cis-dihydroxylation) with a chemocatalytic step (Pd/C-catalysed dehydrogenation), into a one-pot route to catechols, from the parent substituted benzene substrates, has been realised.

Estudio sobre la eficacia del régimen fiscal cooperativo portugués

El ordenamiento jurídico portugués consagra un régimen fiscal especial para el sector cooperativo, basado, al igual que otros ordenamientos como el español o el italiano, en la protección de la mutualidad como forma de organización empresarial especialmente benéfica en el plano social. Para alcanzar ese objetivo, el régimen fiscal cooperativo debe ser selectivo, lo que significa que al legislador se le plantea el reto de establecer criterios para separar, dentro del marco cooperativo, lo que debe ser protegido de lo que no merece protección fiscal. El legislador portugués optó por un modelo basado en dos grupos de ramos cooperativos claramente diferenciados según los beneficios fiscales aplicables, ambos con amplias exenciones fiscales. El presente trabajo no se centra en el contenido de los beneficios aplicables sino en las condiciones que las cooperativas deben reunir para acogerse a esos regímenes fiscales favorables. Estos criterios son: i) una división entre operaciones con socios y operaciones con terceros; ii) una delimitación de las operaciones o actividades cooperativas según estén o no vinculadas con el “fin propio de la cooperativa”; y iii) una estructura prevalentemente mutualista del factor trabajo. Esta fórmula legal tiene su raíz en una legislación de 1929 y se ha mantenido hasta el día de hoy debido en parte a un fenómeno de inercia legislativa. El presente trabajo, basándose en la metodología de la sociología jurídica, asienta en una encuesta dirigida a 64 cooperativas, por la que se buscaba indagar hasta qué punto estos criterios (de acuerdo con los que se seleccionan las cooperativas que pueden acogerse a los regímenes fiscales favorables) cuadran con la realidad cooperativa actual. Como era de esperar, la vetustez del régimen hizo que se encontraran desajustes muy significativos, que reclaman una reforma urgente.

Revisión sistemática de la producción española sobre rendimiento académico entre 1980 y 2011

El bajo rendimiento académico sigue siendo un problema de investigación de gran impacto social. Sin embargo, los resultados científicos no están teniendo repercusión en la mejora, ni en las políticas educativas. En este trabajo nos propusimos identificar, ordenar, analizar y extraer conclusiones sobre la producción española sobre rendimiento académico, con el fin de visualizarla y derivar problemas futuros objeto de investigación. Para ello se llevó a cabo un estudio de revisión en seis etapas, en el que se combinaron procedimientos metodológicos de investigación de síntesis y de investigación bibliométrica. Se identificaron las publicaciones en cuatro bases de datos españolas; posteriormente se analizaron y codificaron los datos extraídos alrededor de nueve indicadores: título, año, tipo de documento, editorial, autor, número autores, institución, comunidad autónoma y tema. Los resultados muestran una producción constante y creciente (1595 referencias), pero dispersa, tanto por el inmenso número de autores que publican, la mayoría con un solo trabajo, como por los lugares donde publican. Las temáticas más tratadas se refieren en primer lugar a modelos explicativos, diagnóstico y tratamiento; en segundo lugar se abordan los factores y variables determinantes del bajo y alto rendimiento académico; en tercer lugar se desarrollan estudios sobre legislación y de otras variables psicológicas y educativas en relación con el rendimiento. Este estudio supone una aproximación sintetizada de la producción sobre rendimiento académico en España, y un primer paso para investigaciones de síntesis posteriores, que nos permitan identificar buenas prácticas para el ejercicio de “prácticas basadas en la evidencia”, y otros problemas de investigación.