Disseny i implementació d'una aplicació web que modelitza competicions esportives de judo

El treball final de carrera fa la modelització, el disseny i la implementació d'una aplicació web per gestionar les competicions d'una federació de judo. L'aplicació permet les altes i les baixes dels esportites, la creació de competicions i la seva gestió.

Disseny i implementació d'una aplicació web per a la reserva on-line de localitats d'espectacles

Aquest treball presenta un terminal de reserva d'espectacles. Es tracta d'una aplicació web que permet als seus usuaris registrats reservar localitats de diferents tipus d'espectacles a través d'internet i amb total llibertat d'horaris. L'aplicació s'ha dissenyat amb tecnologia Java (servlets, JSP, beans ...) i s'ha llicenciat com a aplicació de programari lliure amb la llicència GPL.

Disseny, implementació i optimització d'un algorisme per al càlcul de les constants d'isocronia

S'ha desenvolupat una eina de programari capaç de calcular les constants d'isocronia. S'obté també per pantalla dades referents al cost temporal de l'algorisme de càlcul. Les constants d'isocronia obtingudes són recuperables pel Mathematica per a la seva posterior utilització. El càlcul de les constants d'isocronia és molt més òptim temporalment que el càlcul realitzat pel Mathematica. S'ha tingut en compte també l'optimització en la utilització d'espai de memòria.

Utilización de herramientas de simulación en la robótica industrial

Análisis de herramienta de simulación utilizada en el entorno industrial y estudio de las ventajas de la programación "offline" en un entorno productivo. Programación de una célula de trabajo industrial y ampliación posterior de la misma utilizando la herramienta de simulación industrial.

Tailored thoracomyoplasty as a valid treatment option for chronic post-lobectomy empyema

Background: Chronic post-lobectomy empyema is rare but may require space obliteration for infection control. We report our experience by using a tailored thoracomyoplasty for this specific indication with respect to infection control and functional outcome. Patients and Methods: We retrospectively analysed 17 patients (11 men, 6 women) with chronic post-lobectomy empyema and treated by thoracomyoplasty in our institution between 2000 and 2011. All patients underwent an initial treatment attempt by use of chest tube drainage and antibiotics except those with suspicion of pleural aspergillosis (n=6). In 5 patients, bronchus stump insufficiency was identified at preoperative bronchoscopy. A tailored thoracoplasty was combined with a serratus anterior - rhomboid myoplasty which also served to close a broncho-pleural fistula, if present. The first rib was resected in 11/17 patients. Results: The 90-day mortality was 11.7%. Thoracomyoplasty was successful in all surviving patients with respect to infection control, space obliteration and definitive closure of broncho-pleural fistula, irrespective of the type of infection, the presence of a broncho-pleural fistula and whether a 1st rib resection was performed . Post-lobectomy pulmonary function testing before and after thoracoplasty revealed a mean predicted FEV1 of 63.0±8.5% and 51.5±4.2% (p=0.01), and a mean predicted DLCO of 59.8±11.6% and 54.5±12.5%, respectively. Postoperative shoulder girdle dysfunction and scoliosis were prevented in patients willing to undergo intense physiotherapy. Conclusions: Tailored thoracomyoplasty represents a valid option for patients with chronic post-lobectomy empyema without requiring a preceding open window thoracostomy. Space obliteration and infection control was equally obtained with and without first rib resection.

Latissimus dorsi muscle-flap over Gore-Tex patch for coverage of large thoracic defects in paediatric Ewing sarcoma.

Primary rib involvement accounts for 16% of paediatric Ewing sarcoma (ES). Neo-adjuvant chemotherapy and surgical tumor resection may leave large thoracic wall defects requiring complex reconstruction in a growing individual. We report our experience in three children aged 3, 10, and 12 years, in whom single-stage resection and reconstruction were performed using a Gore-Tex Dualmesh patch, covered by a latissimus dorsi rotation flap harvested in continuity with the thoracolumbar fascia. The youngest patient also had a vertical expandable prosthetic titanium rib (VEPTR) anchored to help prevent subsequent scoliosis throughout growth.

Repair of tracheomalacia with inflammatory defect and mediastinitis.

We describe a novel repair of an anterior inflammatory tracheal defect with mediastinitis, which occurred after external tracheal suspension of localized intrathoracic tracheomalacia. The malacic tracheal segment of 4-cm length containing the inflammatory tracheal defect was noncircumferentially resected. A temporary endotracheal silicone stent was introduced, and the trachea was closed by a pedicled pectoralis muscle flap reinforced with an embedded rib segment. Retrieval of the stent 5 months postoperatively resulted in a re-epithelialized, persistently stable, noncollapsible tracheal segment that showed the same diameter and configuration as the nonreconstructed part of the trachea.

Hints for a fast precessing relativistic radio jet in LS I+61·303

Here we discuss two consecutive MERLIN observations of the X-ray binary LS I +61◦303. The first observation shows a double-sided jet extending up to about 200 AU on both sides of a central source. The jet shows a bent S-shaped struct ure similar to the one displayed by the well-known precessing jet of SS 433. The precession suggested in the first MERLIN image becomes evident in the second one, showing a one-sided bent jet significantly rotated with respect to the jet of the day before. We conclude that the derived precession of the relativistic (β=0.6) jet explains puzzling previous VLBI results. Moreover , the fact that the precession is fast could be the explanation of the never understood short term (days) variability of the associated gamma-ray source 2CG 135 + 01 / 3EG J0241 + 6103.

VLA multifrequency observations of RSCVn binaries

We present multiepoch Very Large Array (VLA) observations at 1.4 GHz, 4.9 GHz, 8.5 GHz and 14.9 GHz for a sample of eight RS CVn binary systems. Circular polarization measurements of these systems are also reported. Most of the fluxes observed are consistent with incoherent emission from mildly relativistic electrons. Several systems show an increase of the degree of circular polarization with increasing frequency in the optically thin regime, in conflict with predictions by gyrosynchrotron models. We observed a reversal in the sense of circular polarization with increasing frequency in three non-eclipsing systems: EI Eri, DM Uma and HD 8358. We find clear evidence for coherent plasma emission at 1.4 GHz in the quiescent spectrum of HD 8358 during the helicity reversal. The degrees of polarization of the other two systems could also be accounted for by a coherent emission process. The observations of ER Vul revealed two U-shaped flux spectra at the highest frequencies. The U-shape of the spectra may be accounted for by an optically thin gyrosynchrotron source for the low frequency part whereas the high frequency part is dominated by a thermal emission component.

A search for microquasar candidates at low galactic latitudes

Recent studies of relativistic jet sources in the Galaxy, also known as microquasars, have been very useful in trying to understand the accretion/ejection processes that take place near compact objects. However, the number of sources involved in such studies is still small. In an attempt to increase the number of known microquasars we have carried out a search for new Radio Emitting X-ray Binaries (REXBs). These sources are the ones to be observed later with VLBI techniques to unveil their possible microquasar nature. To this end, we have performed a cross-identification between the X-ray ROSAT all sky survey Bright Source Catalog (RBSC) and the radio NRAO VLA Sky Survey (NVSS) catalogs under very restrictive selection criteria for sources with |b|<5 degrees. We have also conducted a deep observational radio and optical study for six of the selected candidates. At the end of this process two of the candidates appear to be promising, and deserve additional observations aimed to confirm their proposed microquasar nature.

One-sided jet at milliarcsecond scales in LSI+61·303

We present Very Long Baseline Interferometry (VLBI) observations of the high mass X-ray binary LSI+61303, carried out with the European VLBI Network (EVN). Over the 11 hour observing run, performed 10 days after a radio outburst, the radio source showed a constant flux density, which allowed sensitive imaging of the emission distribution. The structure in the map shows a clear extension to the southeast. Comparing our data with previous VLBI observations we interpret the extension as a collimated radio jet as found in several other X-ray binaries. Assuming that the structure is the result of an expansion that started at the onset of the outburst, we derive an apparent expansion velocity of 0.003 c, which, in the context of Doppler boosting, corresponds to an intrinsic velocity of at least 0.4 c for an ejection close to the line of sight. From the apparent velocity in all available epochs we are able to establish variations in the ejection angle which imply a precessing accretion disk. Finally we point out that LSI+61303, like SS433 and Cygnus X-1, shows evidence for an emission region almost orthogonal to the relativistic jet.

Search for very high energy gamma-ray emission from pulsar-pulsar wind nebula systems with the MAGIC telescope

The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions.

On the binary nature of the γ-ray sources AGL J2241+4454 (= MWC 656) and HESS J0632+057 (= MWC 148)

We present optical spectroscopy of MWC 656 and MWC 148, the proposed optical counterparts of the gamma-ray sources AGL J2241+4454 and HESS J0632+0 57, respectively. The main parameters of the Halpha emission line (EW, FWHM and centroid velocity) in these stars are modulated on the proposed orbital periods of 60.37 and 321 days, respectively. These modulations are likely produced by the resonant interaction of the Be discs with compact stars in eccentric orbits. We also present radial velocity curves of the optical stars folded on the above periods and obtain the first orbital elements of the two gamma-ray sources thus confirming their binary nature. Our orbital solution support eccentricities e~0.4 and 0.83+-0.08 for MWC 656 and MWC 148, respectively. Further, our orbital elements imply that the X-ray outbursts in HESS J0632+057/MWC 148 are delayed ~0.3 orbital phases after periastron passage, similarly to the case of LS I +61 303. In addition, the optical photometric light curve maxima in AGL J2241+4454/MWC 656 occur ~0.25 phases passed periastron, similar to what is seen in LS I +61 303. We also find that the orbital eccentricity is correlated with orbital period for the known gamma-ray binaries. This is explained by the fact that small stellar separations are required for the efficient triggering of VHE radiation. Another correlation between the EW of Halpha and orbital period is also observed, similarly to the case of Be/X-ray binaries. These correlations are useful to provide estimates of the key orbital parameters Porb and e from the Halpha line in future Be gamma-ray binary candidates.

Exploring the connection between the stellar wind and the non-thermal emission in LS 5039

Context.LS 5039 has been observed with several X-ray instruments so far showing quite steady emission in the long term and no signatures of accretion disk. The source also presents X-ray variability at orbital timescales in flux and photon index. The system harbors an O-type main sequence star with moderate mass-loss. At present, the link between the X-rays and the stellar wind is unclear. Aims.We study the X-ray fluxes, spectra, and absorption properties of LS 5039 at apastron and periastron passages during an epoch of enhanced stellar mass-loss, and the long term evolution of the latter in connection with the X-ray fluxes. Methods.New XMM-Newton observations were performed around periastron and apastron passages in September 2005, when the stellar wind activity was apparently higher. April 2005 Chandra observations on LS 5039 were revisited. Moreover, a compilation of H EW data obtained since 1992, from which the stellar mass-loss evolution can be approximately inferred, was carried out. Results.XMM-Newton observations show higher and harder emission around apastron than around periastron. No signatures of thermal emission or a reflection iron line indicating the presence of an accretion disk are found in the spectrum, and the hydrogen column density () is compatible with being the same in both observations and consistent with the interstellar value. 2005 Chandra observations show a hard X-ray spectrum, and possibly high fluxes, although pileup effects preclude conclusive results from being obtained. The H EW shows yearly variations of 10%, and does not seem to be correlated with X-ray fluxes obtained at similar phases, unlike what is expected in the wind accretion scenario. Conclusions.2005 XMM-Newton and Chandra observations are consistent with 2003 RXTE/PCA results, namely moderate flux and spectral variability at different orbital phases. The constancy of the seems to imply that either the X-ray emitter is located at 1012 cm from the compact object, or the density in the system is 3 to 27 times smaller than that predicted by a spherical symmetric wind model. We suggest that the multiwavelength non-thermal emission of LS 5039 is related to the observed extended radio jets and is unlikely to be produced inside the binary system.

Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303. Six orbital cycles were recorded. Several detections occur at a similar orbital phase, which suggests that the emission is periodic. The strongest gamma-ray emission is not observed when the two stars are closest to one another, implying a strong orbital modulation of the emission or absorption processes.