News

This section includes scientific and technological news from the IAC and its Observatories, as well as press releases on scientific and technological results, astronomical events, educational projects, outreach activities and institutional events.

  • Representation of a system similar to XTE J1859+226. The star is distorted by the gravitational influence of the black hole. The material is pulled out from the star and it orbits around the black hole forming an accretion disc.Source/Jesús Corral Santana
    Las binarias de rayos X son sistemas formados por un objeto compacto (estrella de neutrones o agujero negro) y una estrella de tipo “normal”. El objeto compacto arranca materia de la estrella que orbita alrededor del objeto compacto formando un disco de acreción. Las binarias de rayos X transitorias son un tipo de binarias de rayos X que se caracterizan por estar la mayor parte de su vida en quietud. Ocasionalmente, el sistema entra en erupción, fenómeno relacionado con un brusco aumento del ritmo de acreción de materia sobre el agujero negro. Este aumento de brillo se produce en todas las
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  • Average spectrum of the Balmer lines of the central star of NGC 1360. The upper panel represents the mean intensity profile, the middle one displays the mean circular polarization, and the bottom one the mean nul spectrum (a certain modulation which expec
    A large fraction of planetary nebulae (about 80%) are bipolar or elliptical rather than spherically symmetric. Modern theories invoke magnetic fields, among other causes, to explain the rich variety of aspherical components observed in planetary nebulae (PNe), as ejected matter is trapped along magnetic field lines. But, until recently, this idea was mostly a theoretical claim. But in 2005, Jordan et al. report the detection of kG magnetic fields in the central star of two non-spherical PNe, namely NGC1360 and LSS1362. They observed the circular polarization spectra of these stars with the
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  • Figure caption:Upper panels: Proper motion diagrams for S Ori 70 (left, Omega 2000/HAWK-I data) and S Ori 73 (right, ISAAC/HAWK-I data). The two objects of interest are labelled. All identifiedsources within an area of 4 arcmin2 around the targets are plo
    The proper characterization of the least massive population of the young Sigma Orionis star cluster is required to understand the form of the cluster mass function and its impact on our comprehension of the substellar formation processes. S Ori 70 (T5.5+/-1) and 73, two T-type cluster member candidates, are likely to have masses between 3 and 7 MJup if their age is 3 Myr. It awaits confirmation whether S Ori 73 has a methane atmosphere. We aim to: i) confirm the presence of methane absorption in S Ori 73 by performing methane imaging; ii) study S Ori 70 and 73 cluster membership via
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  • Figure caption: (a) (Teff, log g)-diagram of the delta Scuti, gamma Dor, and hybrid stars detected from the ground (parameters taken from the literature). (b): (Teff, log g)-diagram of the Kepler stars we classified as  delta Scuti, gamma Dor, and hybrid
    The Kepler spacecraft is monitoring the brightness of more than 150,000 stars  in the constellations Cygnus, Lyra,  and Draco. The photometric time series with micromagnitude precision are excellent for the study of stellar oscillations. The oscillations lead to small changes in brightness and are caused by waves trapped inside the stars. The field of asteroseismology uses information from the stellar oscillations to infer information from the stellar internal structure. The delta Scuti and gamma Doradus stars are two classes of oscillating stars of spectral type A and F that are slightly
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