Las órdenes religiosas de España y la colonización de América en la segunda parte del siglo XVIII : estadístacas y otros documentos

http://www.archive.org/details/bordenesreligiosas01maasrich/

Libros de texto de matemáticas en España en los siglos XVIII y XIX

A finales del siglo XVIII, en Europa el conocimiento científico se había desarrollado extraordinariamente. Surgen los nombres de Lavoisier, Ritcher, Coulomb y Celsius entre otros muchos. Se enuncian leyes en química y física; junto a ellas también florece la matemática de la mano de Euler, Lagrange, D«Alambert, Monge, por citar s��lo unos cuantos. Mientras tanto, el atraso de las matemáticas españolas se debía, entre otras causas, al pobre estado en que se encontraban las universidades: aún de tipo medieval y de carácter eclesiástico. Esto lo evidencia Fray Benito Jerónimo Feijoo en la carta titulada Causas del atraso que se padece en España en orden a las ciencias naturales, y el Marqués de la Ensenada quien, en 1748, se lo expresa al rey Fernando VI. Las deficiencias de las universidades tenían que ver con la enseñanza memorística, textos anticuados e interés primordial por disciplinas como derecho, teología y filosofía en detrimento de las matemáticas y las ciencias.

Contribuciones de Laplace al desarrollo de la teoría de la probabilidad: en conmemoración de los 200 años de la publicación del "Essai philosophique sur les probabilités" de 1814

En este artículo se analiza la posición que ocupa Laplace en el desarrollo de la teoría clásica de la probabilidad. Se hace en el marco de los 200 años de la publicación del "Essai philosophique sur les probabilités". El artículo se divide en las siguientes secciones: en la primera se introducen algunas de las características de las matemáticas del periodo. En la segunda, se presentan algunos de los desarrollos fundamentales en la teoría de la probabilidad alcanzados durante los siglos XVII y XVIII. Finalmente, presentamos algunas de las principales contribuciones de Laplace. En general, se considera que con Laplace la teoría clásica de la probabilidad adquiere su forma definitiva.

Electron impact excitation of Ar XVII

Energies for the lowest 49 levels among the 1s(2) and 1snl (n = 2-5) configurations of Ar XVII have been calculated using the GRASP code of Dyall et al. (1989, Comput. Phys. Comm., 55, 424). 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. Furthermore, collision strengths have also been calculated for all the 1176 transitions among the above 49 levels using the Dirac Atomic R-matrix Code (DARC) of Norrington & Grant (2005, Comput. Phys. Commun., in preparation), over a wide energy range up to 580 Ryd. Resonances have been resolved in the threshold region, and effective collision strengths have been obtained over a wide temperature range up to log T-e = 7.2 K. 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 0.1%, whereas results for other parameters are probably accurate to better than 20%.

Radiative rates for transitions in Fe XVII

Energies of the lowest 157 levels belonging to the (1s(2)) 2s(2)2p(6), 2s(2)p(5)3l, 2s(2)2p(5)4l, 2s(2)2p(5)4l, 2s2p(5)5l, 2s2p(6)4l and 2s2p(6)5l configurations of Fe XVII 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 (E I), magnetic dipole (M I), electric quadrupole (E2), and magnetic quadrupole (M2) transitions among these levels. Comparisons are made with the results already available in the literature, and the accuracy of the data is assessed. Our energy levels are expected to be accurate to better than M whereas results for other parameters are probably accurate to better than 20%.

Oscillator strengths for transitions in C-like ions between K XIV and Mn XX

Energy levels and oscillator strengths (transition probabilities) have been calculated for transitions among 46 fine-structure levels of the (1s(2)) 2s(2) 2p(2), 2s2p(3),2p(4), 2s(2)2p3s, 2s(2) 2p3p and 2s(2)2p3d configurations of C-like K XIV, Sc XVI, Ti XVII, V XVIII, Cr XIX and Mn XX using the GRASP code. Configuration interaction and relativistic effects have been included while generating the wavefunctions. Calculated values of energy levels agree within 3% with the experimentally compiled results, and the length and velocity forms of oscillator strengths agree within 20% for a majority of allowed transitions.

Energy levels, radiative rates, and collision strengths for transitions in Fe XVII

Energy levels and radiative rates have been calculated for fine-structure transitions among the lowest 89 levels of the (1s(2)) 2s(2)2p(6), 2s(2) 2p(5) 3 l, 2s(2) 2p(5) 4l, 2s2p(6) 3 l, and 2s2p(6)4l configurations of Fe XVII using the GRASP code of Dyall et al. Collision strengths have also been calculated, for transitions among the lowest 55 levels, using the recently developed Dirac atomic R-matrix code (DARC) of Norrington & Grant. The results are compared with those available in the literature, and the accuracy of the data is assessed.

Relativistic allowed and forbidden transition probabilities for fluorine-like Fe XVIII

Energy levels and the corresponding transition probabilities for allowed and forbidden transitions among the levels of the ground configuration and first 23 excited configurations of fluorine-like Fe XVIII have been calculated using the multiconfigurational Dirac-Fock GRASP code. A total of 379 lowest bound levels of Fe XVIII is presented, and the energy levels are identified in spectroscopic notations. Transition probabilities, oscillator strengths and line strengths for electric dipole (E1), electric quadrupole (E2) and magnetic dipole (M1) transitions among these 379 levels are also presented. The calculated energy levels and transition probabilities are compared with experimental data.

Emission lines of Na-like ions in spectra obtained with the Solar EUV Research Telescope and Spectrograph (SERTS)

Theoretical emission-line ratios involving transitions in the 236-412 Angstrom wavelength range are presented for the Na-like ions Ar viii, Cr xiv, Mn xv, Fe xvi, Co xvii, Ni xviii and Zn xx. A comparison of these with an extensive data set of the 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 indicates that most of the Na-like ion lines are reliably detected in the SERTS observations, and hence may be employed with confidence in solar spectral analyses. However, the features in the SERTS spectra at 236.34 and 300.25 Angstrom, originally identified as the Ni xviii 3p (2) P-3/2 -3d (2) D- 3/2 and Cr xiv 3p (2) P-3/2 -3d (2) D-5/2 transitions, respectively, are found to be due to emission lines of Ar xiii (236.34 Angstrom) and possibly S v or Ni vi (300.25 Angstrom). The Co xvii 3s (2) S-3p (2) P-3/2 line at 312.55 Angstrom is always badly blended with an Fe xv feature at the same wavelength, but Mn xv 3s (2) S-3p (2) P-1/2 at 384.75 Angstrom may not always be as affected by second-order emission from Fe xii 192.37 Angstrom as previously thought. On the other hand, we find that the Zn xx 3s (2) S-3p (2) P-3/2 transition can sometimes make a significant contribution to the Zn xx/Fe xiii 256.43- Angstrom blend, and hence care must be taken when using this feature as an Fe xiii electron density diagnostic. A line in the SERTS-89 active region spectrum at 265.00 Angstrom has been re-assessed, and we confirm its identification as the Fe xvi 3p (2) P-3/2 -3d (2) D-3/2 transition.

Radiative rates and electron impact excitation rates for H-like Ar XVIII

Aims. In this paper we report on calculations for energy levels, radiative rates, collision strengths, and effective collision strengths for
transitions among the lowest 25 levels of the n ≤ 5 configurations of H-like Ar xviii.
Methods. The general-purpose relativistic atomic structure package (grasp) andDirac atomic R-matrix code (darc) are adopted for
the calculations.
Results. Radiative rates, oscillator strengths, and line strengths are reported for all electric dipole (E1), magnetic dipole (M1), electric
quadrupole (E2), and magnetic quadrupole (M2) transitions among the 25 levels. Furthermore, collision strengths and effective
collision strengths are listed for all 300 transitions among the above 25 levels over a wide energy (temperature) range up to 800 Ryd
(107.4 K).

"Cómo pintar el aire". Fundamentos científicos de la perspectiva atmosférica

La perspectiva aérea o atmosférica es juzgada por los pintores como parte esencial de la pintura, una vez establecidos los presupuestos geométricos de la representación naturalista mediante la perspectiva lineal. Leonardo da Vinci fue el primer autor en definir la perspectiva aérea o atmosférica, conocidos ya a través de L. B. Alberti los fundamentos geométricos de la perspectiva lineal en el tratado De Pictura (1435). Doscientos años después, tras la influyente publicación del Optics de Newton, contextualizadas bajo el espíritu racionalista del siglo XVIII, el artículo estudia las recomendaciones que desde la ciencia y los científicos (específicamente a través de tres figuras relevantes: Brook Taylor, J. H. Lambert y Gaspard Monge) se dan a los pintores con la pretensión de arbitrar una medición exacta del color, en confrontación con el tradicional empirismo del mundo artístico. Este tema puede considerarse un capítulo de gran interés en la larga historia de la pintura y la representación de los fenómenos atmosféricos, cuyos antecedentes teóricos tienen su inicio en el Débat sur le Coloris de la Académie Française del siglo XVII y sus resultados, conducirán hacia el nacimiento de la moderna Teoría del color, en respuesta a una cuestión tan compleja sobre cómo pintar el aire.

Type XVIII collagen degradation products in acute lung injury

Introduction In acute lung injury, repair of the damaged alveolar-capillary barrier is an essential part of recovery. Endostatin is a 20 to 28 kDa proteolytic fragment of the basement membrane collagen XVIII, which has been shown to inhibit angiogenesis via action on endothelial cells. We hypothesised that endostatin may have a role in inhibiting lung repair in patients with lung injury. The aims of the study were to determine if endostatin is elevated in the plasma/bronchoalveolar lavage fluid of patients with acute lung injury and ascertain whether the levels reflect the severity of injury and alveolar inflammation, and to assess if endostatin changes occur early after the injurious lung stimuli of one lung ventilation and lipopolysaccharide (LPS) challenge.

Effective collision strengths for transitions of Ni XVII

Electron impact excitation collision strengths are required for the analysis and interpretation of stellar observations. This calculation aims to provide fine structure effective collision strengths for the Ni XVII ion using a method which includes contributions from resonances. A DARC calculation has been performed, involving 37 J pi states. The effective collision strengths are calculated by averaging the electron collision strengths over a Maxwellian distribution of electron velocities. The non-zero effective collision strengths for transitions between the fine structure levels are given for electron temperatures (T(e)) in the range log(10) T(e)(K) = 4.5 - 8.5. Data for several transitions from the ground state are discussed in this paper.