Spanish Research Report for 2008

31 páginas, 24 tablasPeer reviewe

Spanish Research Report for 2004

26 páginas, 1 figuras, 24 tablasPeer reviewe

Spanish Research Report for 2006

22 páginas, 1 figura, 20 tablasPeer reviewe

Trabajo de investigación sobre vocabulario y cacografías correspondiente a la zona de influencia del Centro Pedro Barrie de la Maza

Confeccionar el vocabulario usual del niño en un colegio concreto y una tabla de cacografías para trabajar más intensamente sobre ellas y lograr su recuperación. 100 alumnos de tercero de EGB con más nivel de instrucción (bueno, normal y bajo) del Colegio Público Pedro Barrie de la Maza. A cada uno de los niños se le pidió que realizasen doce redacciones que versaban sobre cuatro aspectos diferentes: vida cotidiana, vida social, aspecto cultural y artístico y aspecto moral y religioso. También se les pidió que escribiesen durante 10 minutos las palabras que le sugerían los temas anteriores. Posteriormente, se ha confeccionado una escala de diagnóstico ortográfico. Por último, se extrajo del vocabulario usual del niño todas aquellas palabras con cacografías, bien sean de letras o de tildes, ordenadas alfabéticamente y agrupadas según el tipo de error. Redacciones de los alumnos. Frecuencias. Se incluye una lista con el vocabulario usual del niño y su frecuencia de aparición, una escala de diagnóstico ortográfico para tercero de EGB y una lista de cacografías.GaliciaBiblioteca de Educación del Ministerio de Educación, Cultura y Deporte; Calle San Agustín, 5 - 3 Planta; 28014 Madrid; Tel. +34917748000; Fax +34917748026; [email protected]

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta