Table 1 contains the atomic parameters and measured solar equivalent widths for FeII and Fe I lines. Table 2 contains the spectroscopic parameters for the 451 stars in the HARPS GTO planet search sample. (2 data files).

We present the results from a multiwavelength campaign on the TeV blazar 1ES 1959+650, performed in 2006 May. Data from the optical, UV, soft- and hard-X-ray, and very high energy (VHE) gamma-ray (E>100 GeV) bands were obtained with the Suzaku and Swift satellites, the MAGIC telescope, and other ground-based facilities. The source spectral energy

Context: The dynamics of the solar core cannot be properly constrained through the analysis of acoustic oscillation modes. Gravity modes (g modes) are necessary to understand the structure and dynamics of the deepest layers of the Sun. Through recent progress on the observation of these modes - both individually and collectively - new information

Aims: We study chromospheric emission to understand the temperature stratification in the solar chromosphere. Methods: We observed the intensity profile of the Ca II H line in a quiet Sun region close to the disk center at the German Vacuum Tower Telescope. We analyze over 105 line profiles from inter-network regions. For comparison with the

We study the excitation and damping of transverse oscillations in a multistranded model of a straight line-tied coronal loop. The transverse geometry of our equilibrium configuration is quite irregular and more realistic than the usual cylindrical loop model. By numerically solving the time-dependent ideal magnetohydrodynamic equations in two

Despite the great developments that have been achieved in the last decade in disentangling most relevant stellar population parameters, in particular with the inclusion of absorption linestrength indices, the age-metallicity degeneracy still lurks in these studies. Here I summarize our effort for developing the stellar population synthesis method