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This article explores the 1953–54 Royal Tour and in particular the planning and eventual reception of the Queen and her party when they arrived in Gibraltar. These events are considered in terms of three overlapping contexts: the imperial, the colonial and the geopolitical. First, the Royal Tour marked not only the debut of a new Queen but also the realization that the British Empire was beginning to fragment with the eruption of independence movements in South Asia and the Middle East. Hence, its international itinerary bound the remaining empire symbolically together, but also served as a reminder of the ‘gaps’ that were beginning to appear. Second, the analysis considers how the Royal Tour presented an opportunity for the local residents of Gibraltar to ‘perform their loyalty’ to the new Queen and the British Empire. The focus on performance is significant because the article does not presume that ‘loyalty’ is simply pre-given. A great deal of work was involved in realizing the reception of the Queens party in May 1954 against a backdrop of a territorial dispute with Spain over the future legal status of Gibraltar. The Royal Tour offered the possibility, therefore, of persuading the British and Spanish governments of the local residents’ qualities including a continued loyalty to the British/imperial Royal Family and indirectly to Britain. Third, the article underscores the significance of such loyal performances by considering Spanish opposition to the Queens visit in the light of Francos efforts to establish his countrys anti-Communist credentials. The Royal Tour, and the Gibraltar leg in particular, are thus show to be an intense locus of performances linked to the politics of empire, colonial rights and anti-imperialism. Animated, happy faces gazing at the sights and decorations show better than words the true feelings of the people of the fortress-colony towards their young, beloved Queen. One correspondent of a British newspaper said that he thought the 27,000 servicemen and civilians on the Rock were so fervidly loyal that they would tear to pieces anyone discovered in their midst with evil designs, and that was sufficient guarantee of their Majestys safety.1 [ABSTRACT FROM AUTHOR]

Knowledge of an animal's home range is a crucial component in making informed management decisions. However, many home range studies are limited by study area size, and therefore may underestimate the size of the home range. In many cases, individuals have been shown to travel outside of the study area and utilize a larger area than estimated by the study design. In this study, data collected by multiple research groups studying bottlenose dolphins on the east coast of Florida were combined to determine how home range estimates increased with increasing study area size. Home range analyses utilized photo-identification data collected from 6 study areas throughout the St Johns River (SJR; Jacksonville, FL, USA) and adjacent waterways, extending a total of 253 km to the southern end of Mosquito Lagoon in the Indian River Lagoon Estuarine System. Univariate kernel density estimates (KDEs) were computed for individuals with 10 or more sightings (n = 20). Kernels were calculated for the primary study area (SJR) first, then additional kernels were calculated by combining the SJR and the next adjacent waterway; this continued in an additive fashion until all study areas were included. The 95% and 50% KDEs calculated for the SJR alone ranged from 21 to 35 km and 4 to 19 km, respectively. The 95% and 50% KDEs calculated for all combined study areas ranged from 116 to 217 km and 9 to 70 km, respectively. This study illustrates the degree to which home range may be underestimated by the use of limited study areas and demonstrates the benefits of conducting collaborative science. [ABSTRACT FROM AUTHOR]

In the wide literature on the brain and neural network dynamics the notion of criticality is being adopted by an increasing number of researchers, with no general agreement on its theoretical definition, but with consensus that criticality makes the brain very sensitive to external stimuli. We adopt the complexity matching principle that the maximal efficiency of communication between two complex networks is realized when both of them are at criticality. We use this principle to establish the value of the neuronal interaction strength at which criticality occurs, yielding a perfect agreement with the adoption of temporal complexity as criticality indicator. The emergence of a scale-free distribution of avalanche size is proved to occur in a supercritical regime. We use an integrate-and-fire model where the randomness of each neuron is only due to the random choice of a new initial condition after firing. The new model shares with that proposed by Izikevich the property of generating excessive periodicity, and with it the annihilation of temporal complexity at supercritical values of the interaction strength. We find that the concentration of inhibitory links can be used as a control parameter and that for a sufficiently large concentration of inhibitory links criticality is recovered again. Finally, we show that the response of a neural network at criticality to a harmonic stimulus is very weak, in accordance with the complexity matching principle. [ABSTRACT FROM AUTHOR]

In order to assess the relationship between metallicity and exoplanetary systems, we compare the abundances of AF-type main-sequence stars with debris disk properties assessed using Herschel observations of an unbiased survey of nearby stars. Hot stars are not as commonly observed, given their unique constraints in data reduction, lack of metal lines, and “astrophysical noise” from rotation speed. Here, we address that deficiency using new and archival spectra of 83 AF-type stars. We measure the abundances of a few species in addition to Fe in order to classify the stars with Ap/Am or Lambda Boo signatures. Lambda Boo stars have a chemical signature of solar-abundant volatile species and sub-solar refractory abundances that is hypothesized to be altered by the pollution of volatiles. Overall, we see no correlation between debris disks and metallicity, primarily because the sample size is cut significantly when using only reliable fits to the spectroscopic data. The abundance measured from the Mg ii 4481 blend is a useful diagnostic because it can be reliably measured at large v·sin(i) and is found to be lower around stars with bright debris disks. We find that Lambda Boo stars have brighter debris disks compared to a bias-free sample of AF stars. The trend with disk brightness and Mg abundances suggests pollution effects can be significant and used as a marker for the stability of planetary systems. We explore trends with other species, such as with the C/O ratios, but are significantly limited by the low number of reliable detections. [ABSTRACT FROM AUTHOR]

Abundance analyses of the two newly discovered R Coronae Borealis (RCB) stars ASAS-RCB-8 and ASAS-RCB-10 were conducted using high-resolution optical spectra and model atmospheres. Their chemical compositions place the pair among the majority class of RCBs. ASAS-RCB-10 is one of the most N-poor majority RCBs with an above average O abundance. Relative to ASAS-RCB-10, ASAS-RCB-8 is H poor by 1.6 dex, O-poor by 0.7 dex but N-rich by 0.8 dex suggesting a higher contamination by CNO-cycled material. [ABSTRACT FROM AUTHOR]