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In order to understand the influence of magnetic fields on the propagation properties of waves, as derived from different local helioseismology techniques, forward modeling of waves is required. Such calculations need a model in magnetohydrostatic equilibrium as an initial atmosphere through which to propagate oscillations. We provide a method to

Magnetic fields not only provide a basic tool for observing galaxies but constitute an important clue to interpret many dynamic processes taking place in them, mainly in spiral and irregular galaxies. As in the Sun, magnetic fields become important where gravity becomes lower, i.e. in the outermost regions. Any peripheric feature should be

In the analysis of X-ray fluorescence spectra from planetary surfaces, it is traditionally assumed that the observed surface is a plane-parallel, smooth, and homogeneous medium. The spectral and spatial resolutions of the instruments that have been used to measure X-ray emission from planetary surfaces to date have been such that this has been a

According to its spectral type B2 Ib/I I (Klare & Neckel 1977; Schmidt & Carruthers 1996), HD163899 is a supergiant star. The star presents p and g-mode pulsations (Saio et al. 2006). In such a post-main sequence (post MS) star, the helium core is radiative with a very large Brunt-Väisälä frequency which produces a strong damping. The presence of

HH 262 is a group of emitting knots displaying an `hour-glass' morphology in the Hα and [SII] lines, located 3.5 arcmin to the north-east of the young stellar object L1551-IRS5, in Taurus. We present new results of the kinematics and physical conditions of HH 262 based on Integral Field Spectroscopy covering a field of ~1.5 × 3 arcmin2, which