Excitation rates for transitions in Ca XV

Collision strengths for transitions among the energetically lowest 46 fine-structure levels belonging to the (1s(2)) 2s(2)2p(2), 2s2p(3), 2p(4), and 2s(2)2p3l configurations of Ca XV are computed, over a wide electron energy range below 300 Ryd, using the Dirac Atomic R-matrix Code (DARC) of Norrington & Grant (2003). Resonances in the threshold region have been resolved in a fine energy mesh, and excitation rates are determined over a wide electron temperature range below 10(7) K. The results are compared with those available in the literature, and the accuracy of the data is assessed.

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.

Effective collision strengths for transitions among the 3s(2), 3s3p and 3p(2) configurations of Fe xv

Effective collision strengths for transitions among the ten energetically lowest fine-structure levels belonging to the (1s(2)2s(2)2p(6))3s(2), 3s3p and 3p(2) configurations of Fe xv have been calculated in the electron temperature range of 10(5)-10(7) K, using the recent Dirac atomic R-matrix code of Norrington and Grant. The results are compared with the other recently available independent Breit-Pauli R-matrix calculations of Eissner et al (Eissner W, Galavis M E, Mendoza C and Zeippen C J 1999 Astron. Astrophys. Suppl. 137 165) and Griffin et al (Griffin DC, Badnell N R, Pindzola M S and Shaw J A 1999 J. Phys. B: At. Mol. Opt. Phys. 32 2139, 4129). Large differences are observed for many transitions over almost the entire temperature range. These differences are analysed and discussed, and the accuracy of the calculations is assessed.

Energy levels and radiative rates for transitions in Ar XIII, Ar XIV and Ar XV

Energies for 524 levels of Ar XIII, 460 levels of Ar XIV and 156 levels of Ar XV have been calculated using the GRASP code of Dyall et al. (1989). Additionally, radiative rates, oscillator strengths, and line strengths are calculated for all electric dipole (E1), magnetic dipole (M1), electric quadrupole (E2), and magnetic quadrupole (M2) transitions among these levels. Comparisons are made with the limited results available in the literature, and the accuracy of the data is assessed. Our energy levels are estimated to be accurate to better than 1%, whereas results for other parameters are probably accurate to better than 20%. Additionally, the level lifetimes derived from our radiative rates are in excellent agreement with measured values.

Inner-shell photoexcitation of Fe XV and Fe XVI

The configuration-interaction method as implemented in the computer code CIV3 is used to determine energy levels, electric dipole radiative transition wavelengths, oscillator strengths and transition probabilities for inner-shell excitation of transitions in Fe XV and Fe XVI. Specifically, transitions are considered of the type 1s(2) 2s(2) 2p(6) 3s(2) -1s(2) 2s(2) 2p(5) 3l3l' 3l" (l, l' and l" = s,p or d) in FeXV and 1s(2) 2s(2) 2p(6) 3s- 1s(2) 2s(2) 2p(5) 3l3l' (l and l' = s,p or d) in FeXVI, using the relativistic Breit-Pauli approach. An assessment of the accuracy of the derived atomic data is performed.

An investigation of Fe XV emission lines in solar flare spectra

Previously, large discrepancies have been found between theory and observation for Fe XV emission line ratios in solar flare spectra covering the 224-327 angstrom wavelength range, obtained by the Naval Research Laboratory's S082A instrument on board Skylab. These discrepancies have been attributed to either errors in the adopted atomic data or the presence of additional atomic processes not included in the modelling, such as fluorescence. However our analysis of these plus other S082A flare observations (the latter containing Fe XV transitions between 321-482 angstrom), performed using the most recent Fe XV atomic physics calculations in conjunction with a chianti synthetic flare spectrum, indicate that blending of the lines is primarily responsible for the discrepancies. As a result, most Fe XV lines cannot be employed as electron density diagnostics for solar flares, at least at the spectral resolution of S082A and similar instruments (i.e.similar to 0.1 angstrom). An exception is the intensity ratio I(3s3p P-3(2)-3p(2) P-3(1))/I(3s3p P-3(2)-3p(2) D-1(2))=I(321.8 angstrom)/I(327.0 angstrom), which appears to provide good estimates of the electron density at this spectral resolution.

La música práctica en san Agustín: "vestigium" y "signum"

En distintos momentos de su producción intelectual, Agustín se refirió al asunto de la música. En este artículo mostraremos que Agustín uso dos esquemas conceptuales distintos para describir el fenómeno de la música práctica en su relación con el mundo espiritual, el esquema de las Artes Liberales y el de la teoría del signo, y que en virtud de ello la música sería concebida de dos modos diferentes: como vestigium y como signum del mundo espiritual, respectivamente. Al final del artículo analizaremos la diferencia entre las dos concepciones considerando tres elementos: la naturaleza de la relación entre mundo material y espiritual, el contenido espiritual al que remite y la noción de belleza que implica.

Joaquim Mir y la tienda de juguetes: microhistoria de un retrato

¿Puede un retrato pictórico suscitar un ejercicio de microhistoria? Nuestra investigación tratará de aportar una respuesta positiva a esta cuestión, analizando para ello uno de los pocos retratos del pintor postimpresionista Joaquim Mir Trinxet, fechado en 1926. El protagonista representado no es otro que el suegro del pintor, Antoni Estalella i Trinxet, un insigne personaje de Vilanova y la Geltrú (Barcelona) que vivió entre dos siglos. La obra está ambientada en la tienda de juguetes de la familia, convirtiéndose así en una de las escasas pinturas que han captado el interior de una juguetería en la España anterior a la Guerra Civil. Gracias a los trabajos de archivo realizados, este artículo reúne diversos documentos inéditos que permiten reconstruir no sólo la vida del retratado, que llegó a ser corresponsal de Francisco Pi y Margall, sino también el ambiente social, artístico y comercial de Vilanova, en un período que abarca desde la década de 1870 a la primera mitad del siglo XX, en plena “Edad de Oro” de la industria juguetera. Es esta una propuesta de metodología historiográfica cuyo recorrido comienza en el oficio arcaico de la tonelería para desembocar al fin en los albores del comercio moderno de juguetes.

Inventing the Origin of Theatre History: The Modern Uses of Juba II's 'teatriké historia'