Hallazgos electromiográficos y electroneurográficos en el pie cavo esencial

La etiología del pie cavo cuando ésta es conocida, suele ser debida a un trastorno de tipo neurológico o miopático, aunque en determinados casos nos encontramos con pacientes que padecen esta deformidad en el pie, en los cuales no podemos descubrir ningún antecedente de este tipo, por lo que lo calificamos de pie cavo «esencial». A un grupo de estos pacientes con pie cavo «esencial», en los que no hemos encontrado ningún tipo de antecedente neurológico, lo hemos sometido a una exploración electroneurográfica, encontrando que la mitad de ellos padecían algún trastorno neuropático/miopático, que no había sido detectado en la exploración clínica inicial.Neurological or myopathic diseases are frequently involved in the etiology of flat foot. In some cases, no antecedents of disease can be found and therefore these flat foots are classified as «essential». We have undertaken an electrophysiologic study in a series of patients with «essential» flat food in order to explore unsuspected neurological disorders. In half of the patients, neuropathic and myopathic electroneurographic patterns of different severity were detected

Carbon and oxygen abundances from recombination lines in low-metallicity star-forming galaxies. Implications for chemical evolution

We present deep echelle spectrophotometry of the brightest emission-line knots of the star-forming galaxies He 2-10, Mkn 1271, NGC 3125, NGC 5408, POX 4, SDSS J1253-0312, Tol 1457-262, Tol 1924-416 and the HII region Hubble V in the Local Group dwarf irregular galaxy NGC 6822. The data have been taken with the Very Large Telescope Ultraviolet-Visual Echelle Spectrograph in the 3100-10420 {\AA} range. We determine electron densities and temperatures of the ionized gas from several emission-line intensity ratios for all the objects. We derive the ionic abundances of C$^{2+}$ and/or O$^{2+}$ from faint pure recombination lines (RLs) in several of the objects, permitting to derive their C/H and C/O ratios. We have explored the chemical evolution at low metallicities analysing the C/O vs. O/H, C/O vs. N/O and C/N vs. O/H relations for Galactic and extragalactic HII regions and comparing with results for halo stars and DLAs. We find that HII regions in star-forming dwarf galaxies occupy a different locus in the C/O vs. O/H diagram than those belonging to the inner discs of spiral galaxies, indicating their different chemical evolution histories, and that the bulk of C in the most metal-poor extragalactic HII regions should have the same origin than in halo stars. The comparison between the C/O ratios in HII regions and in stars of the Galactic thick and thin discs seems to give arguments to support the merging scenario for the origin of the Galactic thick disc. Finally, we find an apparent coupling between C and N enrichment at the usual metallicities determined for HII regions and that this coupling breaks in very low-metallicity objects.Comment: 27 pages, 12 figures, Accepted for publication in Monthly Notices of the Royal Astronomical Societ

Integral field spectroscopy of selected areas of the Bright Bar and Orion-S cloud in the Orion Nebula

We present integral field spectroscopy of two selected zones in the Orion Nebula obtained with the Potsdam Multi-Aperture Spectrophotometer (PMAS), covering the optical spectral range from 3500 to 7200 A and with a spatial resolution of 1". The observed zones are located on the prominent Bright Bar and on the brightest area at the northeast of the Orion South cloud, both containing remarkable ionization fronts. We obtain maps of emission line fluxes and ratios, electron density and temperatures, and chemical abundances. We study the ionization structure and morphology of both fields, which ionization fronts show different inclination angles with respect to the plane of the sky. We find that the maps of electron density, O+/H+ and O/H ratios show a rather similar structure. We interpret this as produced by the strong dependence on density of the [OII] lines used to derive the O+ abundance, and that our nominal values of electron density-derived from the [SII] line ratio-may be slightly higher than the appropriate value for the O+ zone. We measure the faint recombination lines of OII in the field at the northeast of the Orion South cloud allowing us to explore the so-called abundance discrepancy problem. We find a rather constant abundance discrepancy across the field and a mean value similar to that determined in other areas of the Orion Nebula, indicating that the particular physical conditions of this ionization front do not contribute to this discrepancy.Comment: 15 pages, 10 figures. Accepted for publication in MNRA

Carbon and oxygen in HII regions of the Magellanic Clouds: abundance discrepancy and chemical evolution

We present C and O abundances in the Magellanic Clouds derived from deep spectra of HII regions. The data have been taken with the Ultraviolet-Visual Echelle Spectrograph at the 8.2-m VLT. The sample comprises 5 HII regions in the Large Magellanic Cloud (LMC) and 4 in the Small Magellanic Cloud (SMC). We measure pure recombination lines (RLs) of CII and OII in all the objects, permitting to derive the abundance discrepancy factors (ADFs) for O^2+, as well as their O/H, C/H and C/O ratios. We compare the ADFs with those of other HII regions in different galaxies. The results suggest a possible metallicity dependence of the ADF for the low-metallicity objects, but more uncertain for high-metallicity objects. We compare nebular and B-type stellar abundances and we find that the stellar abundances agree better with the nebular ones derived from collisionally excited lines (CELs). Comparing these results with other galaxies we observe that stellar abundances seem to agree better with the nebular ones derived from CELs in low-metallicity environments and from RLs in high-metallicity environments. The C/H, O/H and C/O ratios show almost flat radial gradients, in contrast with the spiral galaxies where such gradients are negative. We explore the chemical evolution analysing C/O vs. O/H and comparing with the results of HII regions in other galaxies. The LMC seems to show a similar chemical evolution to the external zones of small spiral galaxies and the SMC behaves as a typical star-forming dwarf galaxy.Comment: Accepted for publication in MNRAS, 17 pages, 11 figures, 8 table

Properties of the ionized gas in HH202. I: Results from integral field spectroscopy with PMAS

We present results from integral field spectroscopy with the Potsdam multi-Aperture Spectrograph of the head of the Herbig-Haro object HH 202 with a spatial sampling of 1"x1". We have obtained maps of different emission lines, physical conditions --such as electron temperature and density-- and ionic abundances from recombination and collisionally excited lines. We present the first map of the Balmer temperature and of the temperature fluctuation parameter, t^2. We have calculated the t^2 in the plane of the sky, which is substantially smaller than that determined along the line of sight. We have mapped the abundance discrepancy factor of O^{2+}, ADF(O^{2+}), finding its maximum value at the HH 202-S position. We have explored the relations between the ADF(O^{2+}) and the electron density, the Balmer and [O III] temperatures, the ionization degree as well as the t^2 parameter. We do not find clear correlations between these properties and the results seem to support that the ADF and t^2 are independent phenomena. We have found a weak negative correlation between the O^{2+} abundance determined from recombination lines and the temperature, which is the expected behaviour in an ionized nebula, hence it seems that there is not evidence for the presence of super-metal rich droplets in H II regions.Comment: 12 pages, 11 figures. Accepted for publication in MNRA

GRASP algorithms for the robust railway network design problem

This paper analyzes the solvability of a railway network design problem and its robust version. These problems are modeled as integer linear programming problems with binary variables, and their solutions provide topological railway networks maximizing the trip coverage in the presence of a competing mode, both assuming that the network works fine and that links can fail, respectively. Since these problems are computationally intractable for realistic sizes, GRASP heuristics are proposed for finding good feasible solutions. The results obtained in a computational experience indicate that our GRASP algorithms are suitable for railway network design problems. © 2011 Springer Science+Business Media, LLC.We would like to thank the Spanish Ministerio de Fomento under grant PT-2007-003, Ministerio de Ciencia y Educacion under grant MTM2009-14243, the Junta de Andalucia under grant P09-TEP-5022 for supporting this research, the FEDER funds of the European Union and TUSSAM (Seville, Spain). Special thanks are due to two anonymous referees for their valuable comments.García-Archilla, B.; Lozano, AJ.; Mesa, JA.; Perea Rojas Marcos, F. (2011). GRASP algorithms for the robust railway network design problem. Journal of Heuristics. 19(2):399-422. https://doi.org/10.1007/s10732-011-9185-zS399422192Baaj, M., Mahmassani, H.: An AI-based approach for transit route system planning and design. J. Adv. Transp. 25(2), 187–210 (1991)Cancela, H., Robledo, F., Rubino, G.: A grasp algorithm with tree based local search for designing a survivable wide area network backbone. J. Comput. Sci. Technol. 4(1), 52–58 (2004)Díaz, J.A., Luna, D., Luna, R.: A grasp heuristic for the manufacturing cell formation problem. TOP (2011). doi: 10.1007/s11750-010-0159-3Feo, T., Resende, M.: A probabilistic heuristic for a computationally difficult set covering problem. Oper. Res. Lett. 8, 67–71 (1989)Goossens, J., van Hoesel, C., Kroon, L.: A branch-and-cut approach for solving railway line-planning problems. Transp. Sci. 38, 379–393 (2004)Institute of Electrical and Electronics Engineers: IEEE Standard Computer Dictionary: A Compilation of IEEE Standard Computer Glossaries (1990)Laporte, G., Mesa, J., Perea, F.: A game theoretic framework for the robust railway transit network design problem. Transp. Res., Part B, Methodol. 44, 447–459 (2010)Laporte, G., Marín, A., Mesa, J., Perea, F.: Designing robust rapid transit networks with alternative routes. J. Adv. Transp. 45, 54–65 (2011)Marín, A., García-Ródenas, R.: Location of infrastructure in urban railway networks. Comput. Oper. Res. 36, 1461–1477 (2009)Marín, A., Jaramillo, P.: Urban rapid transit network design: accelerated Benders decomposition. Ann. Oper. Res. 169(1), 35–53 (2009)Marín, A., Mesa, J.A., Perea, F.: Integrating robust railway network design and line planning under failures. Lect. Notes Comput. Sci. 5868, 273–292 (2009)Mauttone, A., Urquhart, M.E.: A route set construction algorithm for the transit network design problem. Comput. Oper. Res. 36, 2440–2449 (2009)Murphey, R., Pardalos, P., Pitsoulis, L.: A GRASP for the multitarget multisensor tracking problem. In: Networks. Discrete Mathematics and Theoretical Computer Science Series, vol. 40, pp. 277–302. American Mathematical Society, Providence (1998)Nesmachnow, S., Cancela, H., Alba, E.: Evolutionary algorithms applied to reliable communication network design. Eng. Optim. 39(7), 831–855 (2007)Schöbel, A., Scholl, S.: Line planning with minimal transfers. In: 5th Workshop on Algorithmic Methods and Models for Optimization of Railways, Number 06901 in Dagstuhl Seminar Proceedings (2006

Sinovitis villonodular pigmentada difusa: Revisión de 13 casos

Se hace un estudio retrospectivo de trece pacientes con Sinovitis Villonodular pigmentada, seis localizadas en la rodilla, dos en la muñeca y pie, y uno en tobillo, cadera y codo respectivamente. En cinco de los casos existía una afectación del hueso. Se hace una revisión bibliográfica sobre la etiopatogenia, radiología, métodos diagnósticos y tratamientoA retrospective study of thirteen patients with pigmented villonodular synovitis was made. Six cases were localized in the knee, two in the wrist and feet, and one in ankle, hip and elbow. Five case showed bone invasion, the pathogenesis, radiographical appearance, diagnosis and treatment are discussed