We have studied the Balmer line shapes of NGC 3516 in order to find the structure of central Emission Line Region (ELR) and the physical parameters of the emitting plasma. The shapes of these broad emission lines show evidences of a multicomponent origin and also features which could be identified as the peaks of a rotating disc. We have proposed a

In the present work, we study correlations between stellar fundamental parameters and the oscillation amplitude for delta Scuti stars. We present this study for a sample of 17 selected delta Scutis belonging to 5 young open clusters. Taking advantage of properties of delta Scutis in clusters, we correct the photometric parameters of our objects for

With over 5 years of GOLF data having some 90% continuity, a new attempt has been made to search for possible solar g modes. Statistical methods are used, based on the minimum of assumptions regarding the solar physics; namely that mode line-widths are small compared with the inverse of the observing time, and that modes are sought in the frequency

El estudio de propiedades de la granulación y las fáculas del centro al borde del disco es un tema clásico en Física Solar. Aunque se ha dedicado mucho trabajo observacional, semi-empírico y teórico a este asunto, todavía no existe acuerdo generalizado sobre el escenario físico adecuado para reproducir los numerosos observables medidos en diversas

The COMPTEL observations of the galactic 1.809 MeV emission attributed to the radioactive decay of 26Al have confirmed the diffuse nature of this interstellar emission line. One of the most significant features of the reconstructed intensity pattern is a flux enhancement towards Cygnus. This region is fairly young and contains a wealth of massive

We present new spectroscopic observations of an old case of anomalous redshift - NGC 7603 and its companion. The redshifts of the two galaxies which are apparently connected by a luminous filament are z=0.029 and z=0.057 respectively. We show that in the luminous filament there are two compact emission line objects with z=0.243 and z=0.391. They