Efecte dels grups substituents en la formació de nanopartícules de Fe3O4 per descomposició de complexos de Fe(III)

En aquest treball d’investigació, s’estudiaran nanopartícules magnètiques concretament nanopartícules de magnetita (Fe3O4) on a partir de diferents precursors i amb unes condicions determinades es poden variar la seva forma i la seva mida. Aquestes mides i formes diferents són molt útils a l’hora d’introduir-les dins d’una solució de precursor del material superconductor ceràmic YBa2Cu3O7-δ (YBCO) ja que es produeix un augment significatiu de la densitat de corrent crítica. El mètode sintètic utilitzat en aquests treball d’investigació, és l’anomenat descomposició tèrmica, que ens permet sintetitzar nanopartícules de magnetita amb el corresponent control de mida i de forma desitjats.

Generalized Multiobjective Multitree model solution using MOEA

In a previous paper a novel Generalized Multiobjective Multitree model (GMM-model) was proposed. This model considers for the first time multitree-multicast load balancing with splitting in a multiobjective context, whose mathematical solution is a whole Pareto optimal set that can include several results than it has been possible to find in the publications surveyed. To solve the GMM-model, in this paper a multi-objective evolutionary algorithm (MOEA) inspired by the Strength Pareto Evolutionary Algorithm (SPEA) is proposed. Experimental results considering up to 11 different objectives are presented for the well-known NSF network, with two simultaneous data flows

Aportació de les traduccions rosselloneses del segle XIX a la construcció del sistema lingüísticoliterari català

Les traduccions catalanes impreses al Rosselló en el segle XIX són cinc; totes de temàtica religiosa. Rafael Crusat traduí la Novena al glorios patriarca Sant Josep, Digne Espos de la Sempre Verge Maria (1711) reimpresa al segle XIX; Pere Marcè i Sentaló traduí Los set salms penitencials en versos catalans segons lo sentit literal (1802); d'autor desconegut són el Compendi del catecisme al us de totas las iglesias del imperi francès (1807) i els Cantichs catalans, traduits dels cantichs de Sant Sulpici (1826); Joan Miquel Aymar traduí­ la Carta apostolica de N.S. Pare Pio per la providencia divina papa sobre la definicio dogmatica de la immaculada concepció (1889). Aquestes traduccions es justifiquen per la necessitat comunicativa del català  a la diòcesi d'Elna Perpinyà : els catecismes, les pregàries, els cants i les novenes s'hi feien en català . Ara bé, aquestes traduccions apareixen en un moment en què la llengua catalana roman abandonada a l'oralitat familiar i és precisament arran d'això que tenen un gran mèrit en la construcció de la nostra llengua nacional a la Catalunya Nord. En el segle XIX, el del triomf de la "catalanada", quan el país s'hagués pogut decantar cap al secessionisme lingüístic, tot entronitzant el parlar rossellonès com a llengua local, els traductors d'obres religioses utilitzen una ortografia etimològica i una varietat de llengua supradialectal.

Innovació empresarial en el procés de transmissió de dades mitjançant una aplicació mòbil

Disposar d’informació de qualitat, en el moment oportú i en el volum adequat és el que actualment necessiten les empreses per poder prendre decisions òptimes. L’empresa JCM Technologies no és una excepció i és en la obtenció d’informació del procés productiu de l’empresa on aquest projecte pren part. L’objectiu d’aquest projecte de final de màster ha consistit en desenvolupar un sistema capaç d’aportar a l’empresa informació sobre els resultats obtinguts durant el control de qualitat dels productes, informació de la qual no disposava. Les dades existien però no es podien convertir en informació valuosa perquè no es disposava d’un mecanisme capaç tractar-les. Per complir els objectius marcats s’ha creat un sistema format pels següents elements: una aplicació per dispositius mòbils Android, una base de dades, un nou programa pel control de la qualitat i aplicatiu servidor. L’aplicació permet obtenir i visualitzar la informació. La base de dades és on es guarda la informació que envia el programa del control de qualitat i finalment, l’aplicatiu servidor habilita la comunicació entre els diferents elements descrits. El fet que dóna valor al sistema és que tots els elements que el formen tenen la capacitat de comunicar-se entre ells mitjançant Internet. Gràcies a això, és possible obtenir informació a temps real de la producció que s’està portant a terme a qualsevol punt del món. En conclusió, cal dir que els objectius s’han complert ja que s’ha aconseguit un sistema ràpid i segur. D’aquesta manera JCM Technologies pot disposar d’una informació molt valuosa que li permet que certes decisions no siguin preses a l’atzar.

Electromagnetic radiation initiated by hadronic jets from microquasars in the ISM

Microquasars are potential candidates to produce a non-negligible fraction of the observed galactic cosmic rays. The protons accelerated at the jet termination shock interact with the interstellar medium and may produce detectable fluxes of extended emission at different energy bands: high-energy and very high-energy gamma-rays produced by neutral pion-decay, synchrotron and bremsstrahlung emission in a wide energy range generated by the secondary electrons produced by charged pion-decay. We discuss the association between this scenario and some of the unidentified EGRET sources in the galactic plane.

A numerical model for the gamma-ray emission of the microquasar LS 5039

The possible association between the microquasar LS 5039 and the EGRET source 3EG J1824-1514 suggests that microquasars could also be sources of high energy gamma-rays. In this paper, we explore, with a detailed numerical model, if this system can produce the emission detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. The computed spectrum reproduces the observed spectral characteristics at very high energy.

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.

The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Observations of the extraordinarily bright optical afterglow (OA) of GRB 991208 started 2.1 d after the event. The flux decay constant of the OA in the R-band is -2.30 +/- 0.07 up to 5 d, which is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant -3.2 +/- 0.2, the fastest one ever seen in a GRB OA. A negative detection in several all-sky films taken simultaneously to the event implies either a previous additional break prior to 2 d after the occurrence of the GRB (as expected from the jet effect). The existence of a second break might indicate a steepening in the electron spectrum or the superposition of two events. Once the afterglow emission vanished, contribution of a bright underlying SN is found, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our determination of z = 0.706 indicates that GRB 991208 is at 3.7 Gpc, implying an isotropic energy release of 1.15 x 10E53 erg which may be relaxed by beaming by a factor > 100. Precise astrometry indicates that the GRB coincides within 0.2' with the host galaxy, thus given support to a massive star origin. The absolute magnitude is M_B = -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of 11.5 +/- 7.1 Mo/yr. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow is determined 3.5 day after the burst (Dec 12.0) implying a cooling frequency below the optical band, i.e. supporting a jet model with p = -2.30 as the index of the power-law electron distribution.

Microquasars as high energy gamma-ray sources

Galactic microquasars are certainly one of the most recent additions to the field of high energy astrophysics and have attracted increasing interest over the last decade. However, the high energy part of the spectrum of microquasars is the most poorly known, mainly due the lack of sensitive instrumentation in the past. Microquasars are now primary targets for all of the observatories working in the X-ray and gamma-ray domains. They also appear as the possible counterparts for some of the unidentified sources of high-energy gamma-rays detected by the experiment EGRET on board the satellite COMPTON-GRO. This paper provides a general review of the main observational results obtained up to now as well as a summary of the scenarios for production of high-energy gamma-rays at the present moment.

Exploring the high frequency emission of radio loud X-ray binaries

We report millimetre-wave continuum observations of the X-ray binaries Cygnus X-3, SS 433, LSI+61 303, Cygnus X-1 and GRS 1915+105. The observations were carried out with the IRAM 30 m-antenna at 250 GHz (1.25 mm) from 1998 March 14 to March 20. These millimetre measurements are complemented with centimetre observations from the Ryle Telescope, at 15 GHz (2.0 cm) and from the Green Bank Interferometer at 2.25 and 8.3 GHz (13 and 3.6 cm). Both Cygnus X-3 and SS 433 underwent moderate flaring events during our observations, whose main spectral evolution properties are described and interpreted. A significant spectral steepening was observed in both sources during the flare decay, that is likely to be caused by adiabatic expansion, inverse Compton and synchrotron losses. Finally, we also report 250 GHz upper limits for three additional undetected X-ray binary stars: LSI+65 010, LSI+61 235 and X Per.

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.

UBVRI photometry of G, K, M Hipparcos stars. II.

As indicated by Grenon (1989), the data of the present series of reports on the UBVRI photometry of late-type stars in the Hipparcos Input Catalog are to be employed in computations of Hipparcos observing time, as well as in evaluating the observability of faint stars by the satellite. Attention is here given to late type stars in the V = 8-12 range, including distant red giants in the Galactic plane (Hipparcos proposal 189), as well as high proper motion stars included in the G, LTT, LP, and MCC catalogs.