Offensive zones in beach volleyball: differences by gender

Gender differences in anthropometric and athletic properties (e.g. strength) as well as the different net heights (2.24 vs. 2.43 m) on the same field size (8x16 m) would be reflected in the game. The literature about differences between male and female playing characteristics in beach volleyball is scarce. Therefore, the aim of this study was to analyse the differences by gender in the use of offensive zones. Study participants were 20 players (10 female and 10 male) who took part in the European Beach Volleyball Championship 2005 and 2006. Video recordings were made of the 659 points in eight matches played. The beach volleyball court was divided into six zones (z1 to z6). The results showed that men and women use different offensive zones and also were different in the percentages of ball out (15.53 and 27.38% respectively). Concretely, men players used more 1, 2, 4 and 5 zones and women 1 and 5 zones. A few differences were observed in the percentage the ball to the net (7.73 and 5.35% respectively). An understanding of the use of offensive zones is relevant to establish specific tactical training patterns for beach volleyball.

Nuevos horizontes en materia de viajes combinados

Los viajes combinados han ocupado tradicionalmente un lugar destacado dentro de la amplia gama de servicios ofrecidos por los operadores turísticos. Por ello, el Consejo de la Unión Europea adoptó en 1990 la Directiva 90/314/CEE, de 13 de junio, relativa a los viajes combinados, las vacaciones combinadas y los circuitos combinados, con el fin de eliminar, o cuanto menos mitigar, la especial situación de indefensión en que se encontraba aquél que los contrataba. Desde la aprobación de esta Directiva han pasado casi veinticinco años y ante el surgimiento de problemas derivados de la aparición de nuevos modelos de negocio y formas de contratación de los servicios turísticos que ni siquiera se plantearon en aquel momento, se ha hecho necesaria la revisión de una normativa a todas luces obsoleta e incapaz de proteger adecuadamente a los usuarios de estos servicios. Así, el 9 de julio de 2013 la Comisión Europea aprobó la Propuesta de Directiva del Parlamento Europeo y del Consejo relativa a los viajes combinados y los servicios asistidos de viaje, por la que se modifican el Reglamento (CE) nº 2006/2004 y la Directiva 2011/83/UE y por la que se deroga la Directiva 90/314/CEE. El objetivo de este trabajo se centra en analizar las modificaciones propuestas por la C C omisión respecto al ámbito de aplicación de la Directiva 90/314/CEE y su posible repercusión en las legislaciones internas, sobre todo teniendo en cuenta el enfoque de armonización máxima que se pretende dar al nuevo texto.

Unidad 5. Herencia (curso 2011-2012)

Unidad 5. Herencia.

The little-studied cluster Berkeley 90 I. LS III +46 11: a very massive O3.5 If* + O3.5 If* binary

Context. It appears that most (if not all) massive stars are born in multiple systems. At the same time, the most massive binaries are hard to find owing to their low numbers throughout the Galaxy and the implied large distances and extinctions. Aims. We want to study LS III +46 11, identified in this paper as a very massive binary; another nearby massive system, LS III +46 12; and the surrounding stellar cluster, Berkeley 90. Methods. Most of the data used in this paper are multi-epoch high S/N optical spectra, although we also use Lucky Imaging and archival photometry. The spectra are reduced with dedicated pipelines and processed with our own software, such as a spectroscopic-orbit code, CHORIZOS, and MGB. Results. LS III +46 11 is identified as a new very early O-type spectroscopic binary [O3.5 If* + O3.5 If*] and LS III +46 12 as another early O-type system [O4.5 V((f))]. We measure a 97.2-day period for LS III +46 11 and derive minimum masses of 38.80 ± 0.83 M⊙ and 35.60 ± 0.77 M⊙ for its two stars. We measure the extinction to both stars, estimate the distance, search for optical companions, and study the surrounding cluster. In doing so, a variable extinction is found as well as discrepant results for the distance. We discuss possible explanations and suggest that LS III +46 12 may be a hidden binary system where the companion is currently undetected.

A VLT/FLAMES survey for massive binaries in Westerlund 1. IV. Wd1-5 – binary product and a pre-supernova companion for the magnetar CXOU J1647-45?

Context. The first soft gamma-ray repeater was discovered over three decades ago, and was subsequently identified as a magnetar, a class of highly magnetised neutron star. It has been hypothesised that these stars power some of the brightest supernovae known, and that they may form the central engines of some long duration gamma-ray bursts. However there is currently no consenus on the formation channel(s) of these objects. Aims. The presence of a magnetar in the starburst cluster Westerlund 1 implies a progenitor with a mass ≥40 M⊙, which favours its formation in a binary that was disrupted at supernova. To test this hypothesis we conducted a search for the putative pre-SN companion. Methods. This was accomplished via a radial velocity survey to identify high-velocity runaways, with subsequent non-LTE model atmosphere analysis of the resultant candidate, Wd1-5. Results. Wd1-5 closely resembles the primaries in the short-period binaries, Wd1-13 and 44, suggesting a similar evolutionary history, although it currently appears single. It is overluminous for its spectroscopic mass and we find evidence of He- and N-enrichement, O-depletion, and critically C-enrichment, a combination of properties that is difficult to explain under single star evolutionary paradigms. We infer a pre-SN history for Wd1-5 which supposes an initial close binary comprising two stars of comparable (~ 41 M⊙ + 35 M⊙) masses. Efficient mass transfer from the initially more massive component leads to the mass-gainer evolving more rapidly, initiating luminous blue variable/common envelope evolution. Reverse, wind-driven mass transfer during its subsequent WC Wolf-Rayet phase leads to the carbon pollution of Wd1-5, before a type Ibc supernova disrupts the binary system. Under the assumption of a physical association between Wd1-5 and J1647-45, the secondary is identified as the magnetar progenitor; its common envelope evolutionary phase prevents spin-down of its core prior to SN and the seed magnetic field for the magnetar forms either in this phase or during the earlier episode of mass transfer in which it was spun-up. Conclusions. Our results suggest that binarity is a key ingredient in the formation of at least a subset of magnetars by preventing spin-down via core-coupling and potentially generating a seed magnetic field. The apparent formation of a magnetar in a Type Ibc supernova is consistent with recent suggestions that superluminous Type Ibc supernovae are powered by the rapid spin-down of these objects.