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Search Results: 1 - 10 of 187271 matches for " Maria T. Figueras "
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Formoterol May Activate Rat Muscle Regeneration During Cancer Cachexia
Elisabet Ametller,Sílvia Busquets,Gemma Fuster,Maria T. Figueras
Insciences Journal , 2011,
Abstract: PURPOSE: The development of cancer cachexia is the most common manifestation of advanced malignant disease. METHOD: The effects on muscle regeneration of 2-adrenoceptor agonist formoterol (0.3 mg/kg) were tested in cachectic tumour-bearing rats (Yoshida AH-130 ascites hepatoma). RESULTS: Administration of formoterol results in a significant increase in the mass and protein content of tibialis muscle in tumour-bearing-rats. This increase is associated with a decreased myogenin mRNA content together with an increased Pax-7 gene expression. Bupivacaine treatment by local injection results in an important reduction in tibialis weight together with significant increases in Pax-7, myogenin and MyoD gene expression. Formoterol treatment in bupivacaine-treated rats results in significant increases in Pax-7 together with significant decreases in myogenin mRNA content, suggesting that this 2-agonist is favouring muscle regeneration by stimulating the proliferation of satellite cells.Altogether, the data reinforce the potential role of formoterol in the treatment of muscle wasting diseases.
Drets de la Terra
Rosa Maria Laffitte Figueras
Temps d'Educació , 1999,
Abstract:
First detection of the field star overdensity in the Perseus arm
Maria Monguió,Preben Grosb?l,Francesca Figueras
Physics , 2015, DOI: 10.1051/0004-6361/201424896
Abstract: Aims. The main goal of this study is to detect the stellar overdensity associated with the Perseus arm in the anticenter direction. Methods. We used the physical parameters derived from Str\"omgren photometric data to compute the surface density distribution as a function of galactocentric distance for different samples of intermediate young stars. The radial distribution of the interstellar absorption has also been derived. Results. We detected the Perseus arm stellar overdensity at 1.6+-0.2 kpc from the Sun with a significance of 4-5{\sigma} and a surface density amplitude of around 10%, slightly depending on the sample used. Values for the radial scale length of the Galactic disk have been simultaneously fitted obtaining values in the range [2.9,3.5] kpc for the population of the B4-A1 stars. Moreover, the interstellar visual absorption distribution is congruent with a dust layer in front of the Perseus arm. Conclusions. This is the first time that the presence of the Perseus arm stellar overdensity has been detected through individual star counts, and its location matches a variation in the dust distribution. The offset between the dust lane and the overdensity indicates that the Perseus arm is placed inside the co-rotation radius of the Milky Way spiral pattern.
Stellar physical parameters from Str ?mgren photometry. Application to the young stars in the Galactic anticenter survey
Maria Monguió,Francesca Figueras,Preben Grosb?l
Physics , 2014, DOI: 10.1051/0004-6361/201423703
Abstract: Aims. The aim is to derive accurate stellar distances and extinctions for young stars of our survey in the Galactic anticenter direction using the Str\"omgren photometric system. This will allow a detailed mapping of the stellar density and absorption toward the Perseus arm. Methods. We developed a new method for deriving physical parameters from Str\"omgren photometry and also implemented and tested it. This is a model-based method that uses the most recent available stellar atmospheric models and evolutionary tracks to interpolate in a 3D grid of the unreddened indexes [m1], [c1] and Hbeta. Distances derived from both this method and the classical pre-Hipparcos calibrations were tested against Hipparcos parallaxes and found to be accurate. Results. Systematic trends in stellar photometric distances derived from empirical calibrations were detected and quantified. Furthermore, a shift in the atmospheric grids in the range Teff=[7000,9000]K was detected and a correction is proposed. The two methods were used to compute distances and reddening for about 12000 OBA-type stars in our Str\"omgren anticenter survey. Data from the IPHAS and 2MASS catalogs were used to complement the detection of emission line stars and to break the degeneracy between early and late photometric regions. We note that photometric distances can differ by more than 20%, those derived from the empirical calibrations being smaller than those derived with the new method, which agree better with the Hipparcos data.
A cytological study of the O5 chromosomal inversion of Drosophila subobscura (Diptera, Drosophilidae)
Mestres, Francesc;Figueras, Maria Teresa;Serra, Luís;
Genetics and Molecular Biology , 2002, DOI: 10.1590/S1415-47572002000400007
Abstract: the o5 chromosomal inversion has been a cornerstone for understanding different aspects of the american colonization by drosophila subobscura. to obtain more information of this evolutionary event it is important to know the pattern of bands of this inversion in detail. comparing this pattern with that of d. melanogaster it is possible to predict which genes are located inside or close to the o5 inversion and use them as genetic markers. in this study, the complete band pattern of the o5 inversion is presented. furthermore, the most important genes located inside it have been predicted. finally, a constriction located close to the proximal breakage point of the o5 inversion has been observed many times and its possible genetic significance is discussed.
A cytological study of the O5 chromosomal inversion of Drosophila subobscura (Diptera, Drosophilidae)
Mestres Francesc,Figueras Maria Teresa,Serra Luís
Genetics and Molecular Biology , 2002,
Abstract: The O5 chromosomal inversion has been a cornerstone for understanding different aspects of the American colonization by Drosophila subobscura. To obtain more information of this evolutionary event it is important to know the pattern of bands of this inversion in detail. Comparing this pattern with that of D. melanogaster it is possible to predict which genes are located inside or close to the O5 inversion and use them as genetic markers. In this study, the complete band pattern of the O5 inversion is presented. Furthermore, the most important genes located inside it have been predicted. Finally, a constriction located close to the proximal breakage point of the O5 inversion has been observed many times and its possible genetic significance is discussed.
Modelling the inner disc of the Milky Way with manifolds. I - A first step
M. Romero-Gomez,E. Athanassoula,T. Antoja,F. Figueras
Physics , 2011, DOI: 10.1111/j.1365-2966.2011.19569.x
Abstract: We study the bar-driven dynamics in the inner part of the Milky Way by using invariant manifolds. This theory has been successfully applied to describe the morphology and kinematics of rings and spirals in external galaxies, and now, for the first time, we apply it to the Milky Way. We compute the orbits confined by the invariant manifolds of the unstable periodic orbits located at the ends of the bar. We discuss whether the COBE/DIRBE bar and the Long bar compose a single bar or two independent bars and perform a number of comparisons which, taken together, argue strongly in favour of the former. More specifically, we favour the possibility that the so-called COBE/DIRBE bar is the boxy/peanut bulge of a bar whose outer thin parts are the so-called Long bar. This possibility is in good agreement both with observations of external galaxies, with orbital structure theory and with simulations. We then analyse in detail the morphology and kinematics given by five representative Galactic potentials. Two have a Ferrers bar, two have a quadrupole bar and the last one a composite bar. We first consider only the COBE/DIRBE bar and then extend it to include the effect of the Long bar. We find that the large-scale structure given by the manifolds describes an inner ring, whose size is similar to the near and far 3-kpc arm, and an outer ring, whose properties resemble those of the Galactic Molecular Ring. We also analyse the kinematics of these two structures, under the different galactic potentials, and find they reproduce the main over-densities found in the galactic longitude-velocity CO diagram. Finally, we consider for what model parameters, the global morphology of the manifolds may reproduce the two outer spiral arms. We conclude that this would necessitate either more massive and more rapidly rotating bars, or including in the potential an extra component describing the spiral arms.
Atrapados en la Explosión del Uso de las Tecnologías de la Información y Comunicación (Catched in the Explosion of the Use of Information and Communication Technologies)
Olimpia Figueras
PNA , 2011,
Abstract: Los cambios en la práctica docente de los profesores subrayan la utilización de las Tecnologías de la Información y la Comunicación (TIC) en la clase de matemáticas. La concepción de la escuela, la forma en que la ense anza tiene lugar en el aula, las actividades y tareas propuestas a los estudiantes y las competencias que los estudiantes deben desarrollar son algunos de los cambios que deben tenerse en mente. El maestro de matemáticas del siglo XXI debe desarrollar competencias diferentes a las incluidas en los objetivos de su formación inicial. En este escenario, surge la siguiente pregunta: Podrá el profesor alcanzar el paso de aquellos expertos que introducen en el currículo de la educación matemática el uso de TIC en el aula? Changes in teachers’ practices underlie the use of Information and Communication Technologies (ICT) within mathematics classrooms. The school’s conception, the way that teaching is carried out in the classroom, activities and tasks proposed to the students, and competencies students must develop, are some of the changes that have to be taken into consideration. The mathematics teacher of the twenty first century must develop competencies that were not expected in his/her initial teacher training. Within this scenario, a question can be raised: Can mathematics teachers keep pace with the experts who introduce ICT in the classroom?
Kinematic groups across the MW disc: Insights from models and from the RAVE catalogue
Antoja T.,Helmi A.,Figueras F.,Romero-Gómez M.
EPJ Web of Conferences , 2012, DOI: 10.1051/epjconf/20121905002
Abstract: With the advent of the Gaia data, the unprecedented kinematic census of great part of the Milky Way disc will allow us to characterise the local kinematic groups and new groups in different disc neighbourhoods. First, we show here that the models predict a stellar kinematic response to the spiral arms and bar strongly dependent on disc position. For example, we find that the kinematic groups induced by the spiral arm models change significantly if one moves only ~0.6kpc in galactocentric radius, but ~2kpc in azimuth. There are more and stronger groups as one approaches the spiral arms. Depending on the spiral pattern speed, the kinematic imprints are more intense in nearby vicinities or far from the Sun. Secondly, we present a preliminary study of the kinematic groups observed by RAVE. This sample will allow us, for the first time, to study the dependence on Galactic position of the (thin and thick) disc moving groups. In the solar neighbourhood, we find the same kinematics groups as detected in previous surveys, but now with better statistics and over a larger spatial volume around the Sun. This indicates that these structures are indeed large scale kinematic features.
Applying the manifold theory to Milky Way models: First steps on morphology and kinematics
Romero-Gómez M.,Athanassoula E.,Antoja T.,Figueras F.
EPJ Web of Conferences , 2012, DOI: 10.1051/epjconf/20121910006
Abstract: We present recent results obtained by applying invariant manifold techniques to analytical models of the Milky Way. It has been shown that invariant manifolds can reproduce successfully the spiral arms and rings in external barred galaxies. Here, for the first time, we apply this theory to Milky Way models. We select five different models from the literature and, using the parameters chosen by the authors of the papers, and three different cases, namely Case 1, where only the COBE/DIRBE bar is included in the potential; Case 2, when the COBE/DIRBE and the Long bar are aligned, and Case 3, when the COBE/DIRBE bar and the Long bar are misaligned. We compute in each case and for each model the orbits trapped by the manifolds. In general, the global morphology of the manifolds can account for the 3-kpc arms and for the Galactic Molecular Ring.
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