Biochemical differences between the red and white meat of tuna and changes in quality during freezing and storage

The differences between the white and red (dark) meat of tuna (Katsuwonus pelamis) in chemical, physical and organoleptic aspects and the rate and pattern of spoilage during freezing and subsequent storage are discussed in this communication. In the indices studied distinct difference is seen between the white and red meat as well as in the head, middle and tail portions of the same fish. The characteristic colour of tuna meat is due to the presence of haemoglobin and myoglobin, the concentrations of which are about 5 times more in red meat than in white meat. The shelf-life of the frozen material varies with the type of the pack, that is, whole fish>chunks>fillets; the fillets being adversely affected during frozen storage.

Selected Solo Music for Saxophone by United States Composers: 1975-2005

This dissertation project identifies important works for solo saxophone by United States composers between 1975 and 2005. The quality, variety, expressiveness, and difficulty of the solo saxophone repertoire during these thirty years is remarkable and remedies, to some extent, the fact that the saxophone had been a largely neglected instrument in the realm of classical music. In twentieth-century music, including Jazz, the saxophone developed, nevertheless, a unique and significant voice as is evident in the saxophone repertoire that expands immensely in many instrumental settings, including the orchestra, solo works, and a wide variety of chamber ensembles. Historically, the saxophone in the United States first found its niche in Vaudeville, military bands, and jazz ensembles, while in Europe composers such as Debussy, D'Indy, Schmitt, Ibert, Glazounov, Heiden, and Desenclos recognized the potential of the instrument and wrote for it. The saxophone is well suited to the intimacy and unique timbral explorations of the solo literature, but only by the middle twentieth century did the repertoire allow the instrument to flourish into a virtuosic and expressive voice presented by successive generations of performers – Marcel Mule, Sigurd Rascher, Cecil Leeson, Jean-Marie Londeix, Fred Hemke, Eugene Rousseau, and Donald Sinta. The very high artistic level of theses soloists was inspiring and dozens of new compositions were commissioned. Through the 1960’s American composers such as Paul Creston, Leslie Bassett, Henry Cowell, Alec Wilder, and others produced eminent works for the saxophone, to be followed by an enormous output of quality compositions between 1975 and 2005. The works chosen for performance were selected from thousands of compositions between 1975 and 2005 researched for this project. The three recital dates were: April 6, 2005, in Gildenhorn Recital Hall, December 4, 2005, in Ulrich Recital Hall, and April 15, 2006, in Gildenhorn Recital Hall. Recordings of these recitals may be obtained in person or online from the Michelle Smith Performing Arts Library of the University of Maryland, College Park.

Short reflections on the history of African communication

This article aims to propose a chronological subdivision in the history of African communication. African communication today is one of the most important axes for implementing development strategies, sustaining education, health, and schooling programmes, and so on. However, many of these programmes fail due to a lack of or ineffective communication between international organisations, local elite and lay people. The reasons for this situation must be found in Africa’s history of communication, which has undergone radical transformations in its different phases. Using the functionalist analysis drawn up by Jakobson, this article proposes a new chronological subdivision of Africa’s history of communication, reflecting on the current contradictions in contemporary communication in Africa.

The periodic variations of a white-light flare observed with ULTRACAM

High time resolution observations of a white-light flare on the active star EQ PegB show evidence of intensity variations with a period of ≈10 s. The period drifts to longer values during the decay phase of the flare. If the oscillation is interpreted as an impulsively-excited, standing-acoustic wave in a flare loop, the period implies a loop length of ≈3.4 Mm and ≈6.8 Mm for the case of the fundamental mode and the second harmonic, respectively. However, the small loop lengths imply a very high modulation depth making the acoustic interpretation unlikely. A more realistic interpretation may be that of a fast-MHD wave, with the modulation of the emission being due to the magnetic field. Alternatively, the variations could be due to a series of reconnection events. The periodic signature may then arise as a result of the lateral separation of individual flare loops or current sheets with oscillatory dynamics (i.e., periodic reconnection).

White-light oscillations during a flare on II Peg

We analyse the intensity oscillations observed in the gradual phase of a white-light flare on the RS CV n binary II Peg. Fast Fourier Transform power spectra and Wavelet analysis reveal a period of 220 s. The reliability of the oscillation is tested using several criteria. Oscillating coronal loop models are used to derive physical parameters such as temperature, electron density and magnetic field strength associated with the coronal loop. The derived parameters are consistent with the near-simultaneous X-ray observations of the flare. There is no evidence for oscillations in the quiescent state of the binary.

A new look at the pulsating DB white dwarf GD 358: Line-of-sight velocity measurements and constraints on model atmospheres

We report on our findings of the bright, pulsating, helium atmosphere white dwarf GD 358, based on time-resolved optical spectrophotometry. We identify 5 real pulsation modes and at least 6 combination modes at frequencies consistent with those found in previous observations. The measured Doppler shifts from our spectra show variations with amplitudes of up to 5.5 km s-1 at the frequencies inferred from the flux variations. We conclude that these are variations in the line-of-sight velocities associated with the pulsational motion. We use the observed flux and velocity amplitudes and phases to test theoretical predictions within the convective driving framework, and compare these with similar observations of the hydrogen atmosphere white dwarf pulsators (DAVs). The wavelength dependence of the fractional pulsation amplitudes (chromatic amplitudes) allows us to conclude that all five real modes share the same spherical degree, most likely, l=1. This is consistent with previous identifications based solely on photometry. We find that a high signal-to-noise mean spectrum on its own is not enough to determine the atmospheric parameters and that there are small but significant discrepancies between the observations and model atmospheres. The source of these remains to be identified. While we infer Teff =24 kK and log g ~ 8.0 from the mean spectrum, the chromatic amplitudes, which are a measure of the derivative of the flux with respect to the temperature, unambiguously favour a higher effective temperature, 27 kK, which is more in line with independent determinations from ultra-violet spectra.

SDSS J150722.30+523039.8: a cataclysmic variable formed directly from a detached white dwarf/brown dwarf binary?

We present high-speed, three-colour photometry of the eclipsing cataclysmic variable SDSS J150722.30+523039.8 (hereafter SDSS J1507). This system has an orbital period of 66.61 min, placing it below the observed `period minimum' for cataclysmic variables. We determine the system parameters via a parametrized model of the eclipse fitted to the observed lightcurve by ?2 minimization. We obtain a mass ratio of q = 0.0623 +/- 0.0007 and an orbital inclination . The primary mass is Mw = 0.90 +/- 0.01Msolar. The secondary mass and radius are found to be Mr = 0.056 +/- 0.001Msolar and Rr = 0.096 +/- 0.001Rsolar, respectively. We find a distance to the system of 160 +/- 10pc. The secondary star in SDSS J1507 has a mass substantially below the hydrogen burning limit, making it the second confirmed substellar donor in a cataclysmic variable. The very short orbital period of SDSS J1507 is readily explained if the secondary star is nuclearly evolved, or if SDSS J1507 formed directly from a detached white dwarf/brown dwarf binary. Given the lack of any visible contribution from the secondary star, the very low secondary mass and the low HeI ?6678/Ha emission-line ratio, we argue that SDSS J1507 probably formed directly from a detached white dwarf/brown dwarf binary. If confirmed, SDSS J1507 will be the first such system identified. The implications for binary star evolution, the brown dwarf desert and the common envelope phase are discussed.

The use of cues for attention in ancient Greek art: aspects that influence concentration in the work of art and its elements

The goal of this study is to identify cues for the cognitive process of attention in ancient Greek art, aiming to find confirmation of its possible use by ancient Greek audiences and artists. Evidence of cues that trigger attention’s psychological dispositions was searched through content analysis of image reproductions of ancient Greek sculpture and fine vase painting from the archaic to the Hellenistic period - ca. 7th -1st cent. BC. Through this analysis, it was possible to observe the presence of cues that trigger orientation to the work of art (i.e. amplification, contrast, emotional salience, simplification, symmetry), of a cue that triggers a disseminate attention to the parts of the work (i.e. distribution of elements) and of cues that activate selective attention to specific elements in the work of art (i.e. contrast of elements, salient color, central positioning of elements, composition regarding the flow of elements and significant objects). Results support the universality of those dispositions, probably connected with basic competencies that are hard-wired in the nervous system and in the cognitive processes.

A puzzling periodicity in the pulsating DA white dwarf G 117-B15A

We present time-resolved optical spectrophotometry of the pulsating hydrogen atmosphere (DA) white dwarf G 117-B15A. We find three periodicities in the pulsation spectrum (215 s, 272 s, and 304 s) all of which have been found in earlier studies. By comparing the fractional wavelength dependence of the pulsation amplitudes ( chromatic amplitudes) with models, we confirm a previous report that the strongest mode, at 215 s, has l = 1. The chromatic amplitude for the 272 s mode is very puzzling, showing an increase in fractional amplitude with wavelength that cannot be reproduced by the models for any ` at optical wavelengths. Based on archival HST data, we show that while the behaviour of the 215 s mode at ultra-violet wavelengths is as expected from models, the weird behaviour of the 272 s periodicity is not restricted to optical wavelengths in that it fails to show the expected increase in fractional amplitude towards shorter wavelengths. We discuss possible causes for the discrepancies found for the 272 s variation, but find that all are lacking, and conclude that the nature of this periodicity remains unclear.

On the parallax of WD 0346+246: a halo white dwarf candidate

We present a parallax measurement for the very cool degenerate WD 0346+246, the serendipitous discovery of which was reported by Hambly et al, We find an absolute parallax of 36 +/- 5 mas, yielding a distance estimate of 28 +/- 4pc. The resulting absolute visual magnitude of the object is M-V = 16.8 +/- 0.3, making it the second-lowest luminosity white dwarf currently known. We use the distance estimate and measured proper motion to show that the object has kinematics consistent with membership of the Galactic halo. WD 0346+246 is therefore by far the coolest and least luminous of only a handful of plausible halo white dwarf candidates. As such, the object has relevance to the ongoing debate concerning the results of microlensing experiments and the nature of any baryonic dark matter component to the Galactic halo residing in stellar remnants.

White matter fractional anisotrophy predicts balance performance in older adults

Aging is characterized by brain structural changes that may compromise motor functions. In the context of postural control, white matter integrity is crucial for the efficient transfer of visual, proprioceptive and vestibular feedback in the brain. To determine the role of age-related white matter decline as a function of the sensory feedback necessary to correct posture, we acquired diffusion weighted images in young and old subjects. A force platform was used to measure changes in body posture under conditions of compromised proprioceptive and/or visual feedback. In the young group, no significant brain structure-balance relations were found. In the elderly however, the integrity of a cluster in the frontal forceps explained 21% of the variance in postural control when proprioceptive information was compromised. Additionally, when only the vestibular system supplied reliable information, the occipital forceps was the best predictor of balance performance (42%). Age-related white matter decline may thus be predictive of balance performance in the elderly when sensory systems start to degrade.

Type Ia supernovae from exploding oxygen-neon white dwarfs

Context. The progenitor problem of Type Ia supernovae (SNe Ia) is still unsolved. Most of these events are thought to be explosions of carbon-oxygen (CO) white dwarfs (WDs), but for many of the explosion scenarios, particularly those involving the externally triggered detonation of a sub-Chandrasekhar mass WD (sub-M-Ch, WD), there is also a possibility of having an oxygen-neon (ONe) WD as progenitor.

Aims. We simulate detonations of ONe WDs and calculate synthetic observables from these models. The results are compared with detonations in CO WDs of similar mass and observational data of SNe Ia.

Methods. We perform hydrodynamic explosion simulations of detonations in initially hydrostatic ONe WDs for a range of masses below the Chandrasekhar mass (M-Ch), followed by detailed nucleosynthetic postprocessing with a 384-isotope nuclear reaction network. The results are used to calculate synthetic spectra and light curves, which are then compared with observations of SNe Ia. We also perform binary evolution calculations to determine the number of SNe Ia involving ONe WDs relative to the number of other promising progenitor channels.

Results. The ejecta structures of our simulated detonations in sub-M-Ch, ONe WDs are similar to those from CO WDs. There are, however, small systematic deviations in the mass fractions and the ejecta velocities. These lead to spectral features that are systematically less blueshifted. Nevertheless, the synthetic observables of our ONe WD explosions are similar to those obtained from CO models.

Conclusions. Our binary evolution calculations show that a significant fraction (3-10%) of potential progenitor systems should contain an ONe WD. The comparison of our ONe models with our CO models of comparable mass (similar to 1.2 M-circle dot) shows that the less blueshifted spectral features fit the observations better, although they are too bright for normal SNe Ia.

Tourist travel via Grand Trunk Railway System : and connections, including Niagara Falls and Gorge, the Highlands of Ontario, comprising Georgian Bay, Muskoka Lakes ; St. Lawrence River, Montreal, Quebec, the Saguenay River, the Rangeley Lakes, White Mountains, and the Atlantic Sea-Coast /

Previous editions of this work have appeared under the title: Gateways of tourist travel.

La administración educativa en España (1900-1971).

Se creó por Real Decreto el 18/04/1900 el Ministerio de Instrucción Pública y Bellas Artes. Se le encomiendan las cuestiones relativas a la enseñanza pública y privada en todos sus grados, el fomento de las ciencias, artes y letras, los archivos, museos y bibliotecas y el Instituto Geográfico y Estadístico. Nace así, un departamento ministerial específicamente dedicado al sector educativo y cultural, que ya se mantendrá hasta nuestros días (salvedad breve paréntesis de 1923-1925). En este tiempo, setenta y cinco años, han sucedido profundos cambios en la sociedad en la educación e incluso en el concepto mismo de la propia administración. En este sentido pueden señalarse cuatro etapas que presentan grandes diferencias importantes para una necesaria y adecuada comprensión de la evolución de la administración educativa. Son: 1. Etapa de consolidación de la autonomía administrativa (1900-1936); 2. Etapa de transición desde fines de la Guerra Civil hasta la promulgación de la Ley en 1955 de Reforma Orgánica del Ministerio; 3. Etapa de fortalecimiento y progresivo deterioro desde 1955-1968; 4. Años transcurridos desde la aprobación de la Ley General de Educación, con los intentos de poner en marcha una nueva administración que responda a las exigencias del nuevos sistema educativo.

Un nuevo concepto de la enseñanza del dibujo : Congreso Internacional sobre Didáctica de las Artes Plásticas (1. 1975. Barcelona).

El dibujo fue el primer protagonista de la escuela nueva de esas inquietudes innovadoras. Los aspectos teóricos apenas cuentan lo importante es mantener la imaginación infantil en estado puro. No es necesario acercarse al modelo, las obras maestras deben dejarse para una etapa posterior. El dibujo entra en el campo pedagógico como vehículo de comunicación infantil y como instrumento terapéutico. El dibujo cumple una función socializante muy de acuerdo con las tendencias educativas del primer cuarto de siglo XX. Pronto se convierte en preocupación general 1900-1960 etapa en la que se celebran congresos y reuniones internacionales para tratar la enseñanza del dibujo, en particular, o la enseñanza estética, en general. Desde el primer Congreso en París de 1900 se votó por la obligatoriedad de su enseñanza a todos los niveles. Es el dibujo de imitación basado en la observación y del dibujo geométrico o representación matemática exacta de las figuras. Dibujar es evaluar relaciones. En 1908 gran importancia al dibujo creativo frente al imitativo. En 1912 es establece un programa de dibujo. A partir del Congreso de 1968 la educación artística es parte integrante en la formación general del hombre. Finalmente prevalece la idea de que el educador artístico no ha de ser más que un informador de técnicas para que el dibujo no pierda su valor emocionalmente individual, pero consiga convertirse en instrumento de juicio y comunicación. Aunque estas ideas de René- Jean Clot hoy se nos quedan cortas.