Características de carcaça de cordeiros Hampshire Down e Santa Inês sob diferentes fotoperíodos

O objetivo deste trabalho foi avaliar o efeito do fotoperíodo e da raça nas características de carcaça de cordeiros machos Hampshire Down e Santa Inês. Sete cordeiros Hampshire Down e sete Santa Inês foram submetidos a fotoperíodo de 12 horas luz x 12 horas escuro (curto) e de 18 horas luz x 6 horas escuro (longo). Após o desmame, os cordeiros foram alojados em baias individuais de acordo com os tratamentos. Ao atingirem 31 kg de peso vivo, foram abatidos e a carcaça e os componentes não-constituintes da carcaça foram pesados. Cordeiros Santa Inês apresentaram peso de carcaça quente superior ao dos Hampshire e maior rendimento comercial. Cordeiros Santa Inês apresentaram maior peso de sangue, coração, pulmão, rins e baço. Já os cordeiros Hampshire Down apresentaram pesos de pele, patas e aparelho gastrintestinal cheio superiores aos do Santa Inês. Os cordeiros Santa Inês apresentaram maior largura de garupa e comprimento de perna do que os Hampshire Down. Os cordeiros Santa Inês apresentaram porcentagem de costela descoberta e baixos maior do que os Hampshire Down, com maior porcentagem de perna. A raça influencia mais as características de carcaça do que o fotoperíodo.

Qualidade de carcaças de cordeiros Corriedale, Bergamácia x Corriedale e Hampshire Down x Corriedale, terminados em pastagem e confinamento

O objetivo deste experimento foi comparar as características qualitativas de carcaças de 36 cordeiros terminados em pastagem de coastcross, sendo 13 Corriedale, 14 Bergamácia x Corriedale e 9 Hampshire Down x Corriedale, e 29 cordeiros terminados em confinamento, sendo 10 Corriedale, 11 Bergamácia x Corriedale e 8 Hampshire Down x Corriedale. As médias das variáveis (escala de 1 a 5) condição corporal: 2,70 e 3,13; conformação: 2,65 e 3,35; e cobertura de gordura: 2,43 e 2,95; foram superiores para os cordeiros do confinamento que para cordeiros em pastagem. Na escala de 1 a 3, foram avaliadas a cor da gordura: 1,66 e 1,94; cor da carne: 1,66 e 1,72; e consistência de gordura: 1,62 e 1,83, respectivamente, para os cordeiros em pastagem e em confinamento. A área de olho de lombo foi significativamente (10,21 vs. 9,03 cm²), bem como a espessura de gordura de cobertura: 1,10 vs. 1,70 mm, foi superior para os cordeiros confinados. As médias das porcentagens de músculo no lombo foram de 54,92 e 57,94%; para gordura, 9,29 e 12,95%; e osso, 35,78 e 29,10%, respectivamente, para cordeiros em pastagem e confinamento. Entre os sistemas de terminação, não houve diferenças para porcentagem de proteína (19,71 e 19,10%, respectivamente), mas houve diferença para teor de lipídios, com 5,43% para cordeiros em pastejo e 11,54% para cordeiros confinados. Para as variáveis analisadas não houve diferenças significativas entre os cruzamentos.

Moonlets wandering on a leash-ring

Since the Voyager flybys, embedded moonlets have been proposed to explain some of the surprising structures observed in Saturn's narrow F ring. Experiments conducted with the Cassini spacecraft support this suggestion. Images of the F ring show bright compact spots, and seven occultations of stars by the F ring, monitored by ultraviolet and infrared experiments, revealed nine events of high optical depth. These results point to a large number of such objects, but it is not clear whether they are solid moonlets or rather loose particle aggregates. Subsequent images suggested an irregular motion of these objects so that a determination of their orbits consistent with the F ring failed. Some of these features seem to cross the whole ring. Here we show that these observations are explained by chaos in the F ring driven mainly by the 'shepherd' moons Prometheus and Pandora. It is characterized by a rather short Lyapunov time of about a few hundred orbital periods. Despite this chaotic diffusion, more than 93 per cent of the F-ring bodies remain confined within the F ring because of the shepherding, but also because of a weak radial mobility contrasted by an effective longitudinal diffusion. This chaotic stirring of all bodies involved prevents the formation of 'propellers' typical of moonlets, but their frequent ring crossings explain the multiple radial 'streaks' seen in the F ring. The related 'thermal' motion causes more frequent collisions between all bodies which steadily replenish F-ring dust and allow for ongoing fragmentation and re-accretion processes (ring recycling).

Some comments on the F ring-Prometheus-Pandora environment

The system formed by the F ring and two close satellites, Prometheus and Pandora, has been analysed since the time that Voyager visited the planet Saturn. During the ring plane crossing in 1995 the satellites were found in different positions as predicted by the Voyager data. Besides the mutual effects of Prometheus and Pandora, they are also disturbed by a massive F ring. Showalter et al. [Icarus 100 (1992) 394] proposed that, the core of the ring has a mass which corresponds to a moonlet varying in size from 15 to 70 kin in radius which can prevent the ring from spreading due to dissipative forces, such as Poynting-Robertson drag and collisions. We have divided this work into two parts. Firstly we analysed the secular interactions between Prometheus-Pandora and a massive F ring using the secular theory. Our results show the variation in eccentricity and inclination of the satellites and the F ring taking into account a massive ring corresponding to a moonlet of different sizes. There is also a population of dust particles in the ring in the company of moonlets at different sizes [Icarus 109 (1997) 304]. We also analysed the behaviour of these particles under the effects of the Poynting-Robertson drag and radiation pressure. Our results show that the time scale proposed for a dust particle to leave the ring is much shorter than predicted before even in the presence of a coorbital moonlet. This result does not agree with the confinement model proposed by Dermott et al. [Nature 284 (1980) 309]. In 2004, Cassini mission will perform repeated observations of the whole system, including observations of the satellites and the F ring environment. These data will help us to better understand this system. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.

A new shadow-ring device for measuring diffuse solar radiation at the surface

A new shadow-ring device for measuring diffuse solar radiation at the surface is presented. In this device the seasonal variation of shadow is followed by moving the detector horizontally. This unique characteristic facilitates its application for long and continuous periods of time. The blocking effect caused by the ring and other related geometric properties are formulated considering the diffuse solar radiation isotropic. The correction factor, shadow size, and ring-detector distance are derived as a function of radius and width of the ring, sun position, and local latitude. The largest blocking occurs during summer, when the ring-detector distance and the shadow width are the smallest, and it is compensated by a smaller blocking effect in the winter period. The performance of the new device is verified comparing daily values of diffuse solar radiation measured simultaneously with a similar device from Kipp & Zonen, Inc. The results show a very good agreement (within 2.5%) between both devices. The new device was also able to reproduce the radiometric properties of the local atmosphere based on 3-yr-long measurements of direct solar radiation using a pyrheliometer. The new device can be applied to estimate daily values of diffuse solar radiation at the surface in the range of 30degreesN-30degreesS with results comparable to other similar apparatuses.

The strands of the F ring disturbed by its closest satellites

Some Voyager images showed that the F ring of Saturn is composed of at least four separate, non-intersecting, strands covering about 45 degrees in longitude. According to Murray et al. [Murray, C.D., Gordon, M., Giuliatti Winter, S.M. Unraveling the strands of Saturn's F ring. Icarus 129, 304, 1997.] this structure may be caused by undetected satellites embedded in the gaps.Due to precession, the satellites Prometheus and Pandora and the ring particles can experience periodic close encounters. Giuliatti Winter et al. [Giuliatti Winter, S.M, Murray, C.D., Gordon, M. Perturbations to Saturn's F-ring strands at their closest approach to Prometheus. Plan. Space Sciences, 48, 817, 2000.] analysed the behaviour of these four strands at closest approach with the satellite Prometheus. Their work suggests that Prometheus can induce the ring particles to scatter in the direction of the planet, thus increasing the population of small bodies in this region.In this work we analysed the effects of Prometheus on the radial structure of Saturn's F ring during the Voyager and early Cassini epochs. Our results show that at Voyager epoch Prometheus, and also Pandora, had a negligible influence in the strands. However, during the Cassini encounter Prometheus could affect the strands significantly, scattering particles of the inner strand in the direction of the planet. This process can contribute to the replenishment of material in the region between the F ring and the A ring, where two rings have recently been discovered [Porco, C. et al. Cassini imaging science. Initial results on Saturn's rings and small Satellites. Science, 307, 1226, 2005].We also analyse the behaviour of undetected satellites under the effects of these two satellites by computing the Lyapunov Characteristic Exponent. Our results show that these satellites have a chaotic behaviour which leads to a much more complex scenario. The new satellite S/2004 S6 also presents a chaotic behaviour with can alter the dynamic of the system, since this satellite crosses the orbit of the strands. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved.

Sino-aortic denervation causes right atrial beta adrenoceptor down-regulation

Rat isolated right atria obtained 1 wk after sinoaortic denervation were less sensitive to the chronotropic actions of beta-agonists than were tissues obtained from animals that underwent sham surgery or no surgery at all. The potencies, but not the maximal responses for two high efficacy agonists, norepinephrine and isoproterenol, were reduced about 3- to 4-fold. Sinoaortic denervation (SAD) caused about a 3-fold decrease in potency and about a 60% decrease in maximal response for a low efficacy agonist, prenalterol. The changes in the actions of these agonists occurred in the absence of any changes in the subtype of beta receptor mediating the chronotropic response. The results of analyses of the data for prenalterol showed that SAD caused a decrease in the operational efficacy of this agonist without any changes in its K-D value for beta-1 adrenoceptors. SAD had no effect on the responses of the tissue to blockade of uptake 1 and uptake 2, suggesting no compensatory changes in the removal processes caused the decreased potency. The results of radioligand binding assays showed that SAD caused a decrease in the maximal binding of I-125-cyanopindolol without altering its K-D. Also, the results of competition binding assays confirmed the lack of effect of SAD on the K-D for prenalterol. The SAD-induced changes in the actions of agonists acting at right atrial beta-1 receptors were caused by a down-regulation of beta-1 adrenoceptors, which probably occurred in response to SAD-induced increases in sympathetic tone.

Periodic collisions between the moon Prometheus and Saturn's F ring

Saturn's F ring, which lies 3,400 km beyond the edge of the main ring system, was discovered by the Pioneer 11 spacecraft(1) in 1979. It is a narrow, eccentric ring which shows an unusual 'braided' appearance in several Voyager 1 images' obtained in 1980, although it appears more regular in images from Voyager 2 obtained nine months later(3). The discovery of the moons Pandora and Prometheus orbiting on either side of the ring provided a partial explanation for some of the observed features(4). Recent observations of Prometheus(5,6) by the Hubble Space Telescope show, surprisingly, that it is lagging behind its expected position by similar to 20 degrees. By modelling the dynamical evolution of the entire Prometheus-F ring-Pandora system, we show here that Prometheus probably encountered the core of the F ring in 1994 and that it may still be entering parts of the ring once per orbit. Collisions with objects in the F ring provide a plausible explanation for the observed lag and imply that the mass of the F ring is probably less than 25% that of Prometheus.