PODEMOS SER COMPETITIVOS EN I+D+i , también ahora (Análisis de un caso de éxito: ASTROFÍSICA ESPAÑOLA) Francisco Sánchez Foro España Innova, 6/2/2012 No voy a hablarles esta mañana ni de planetas extrasolares, ni de estrellas de neutrones, agujeros negros, materia obscura, energía obscura, ni de ninguna otra maravilla del misterioso Universo al que pertenecemos. Tampoco es mi intención hacer un discurso apologético, resaltando los mil y un beneficios de la Ciencia y del poder de la investigación para promover la competitividad y la recuperación económica, (todos los aquí presentes ya lo

Informe Semanal ha viajado al Instituto de Astrofísica de Canarias para conocer los últimos proyectos que nos acercan más al Sol.

La colaboración SDSS-III, en la que participa el IAC, anuncia nuevos resultados del proyecto BOSS sobre la enigmática energía oscura y los neutrinos, las elusivas partículas subatómicas claves para entender tanto el origen del universo como las supernovas

The stellar origin of the extremely hydrogen-deficient R Coronae Borealis (RCB) stars has remained a mystery for astronomers since their discovery more than two hundred years ago.  Two competing scenarios are commonly advocated. In the first one, a final helium shell flash occurs on a cooling white dwarf star or a very late thermal pulse is experienced by a post-AGB star. The second scenario involves the merger of two white dwarfs: a carbon–oxygen white dwarf accretes ahelium white dwarf. Evidence from the chemical compositions of RCB stars suggests that most are products of a merger

The effects that interactions produce on galaxy disks and how they modify the subsequent formation of bars need to be distinguished to fully understand the relationship between bars and environment. To this aim we derive the bar fraction in three different environments ranging from the field to Virgo and Coma Clusters, covering an unprecedentedly large range of galaxy luminosities (or, equivalently, stellar masses). We confirm that the fraction of barred galaxies strongly depends on galaxy luminosity. We also show that the difference between the bar fraction distributions as a function of

We use deep Hubble Space Telescope Advanced Camera for Surveys/High Resolution Channel observations of a field within M32 (F1) and an M31 background field (F2) to determine the star formation history (SFH) of M32 from its resolved stellar population. We find that 2-5 Gyr old stars contribute ~40% ± 17% of M32's mass, while ~55% ± 21% of M32's mass comes from stars older than 5 Gyr. The SFH additionally indicates the presence of young (<2 Gyr old), metal-poor ([M/H] ~ –0.7) stars, suggesting that blue straggler stars contribute ~2% of the mass at F1; the remaining ~3% of the mass is in young