The SFH of galaxies can be studied with detail in nearby systems which are resolvable into individual stars. In such case, the color-magnitude (CM) diagram can be plotted. Perhaps, the most powerful method nowadays available for the study of the SFH of galaxies is to compare their observed CM diagrams with sets of synthetic CM diagrams computed

We present observations of the new Local Group galaxy candidates Cassiopeia dSph, Pegasus dSph=AndVI and Camelopardalis A. Our deep color-magnitude diagrams show that the first two galaxies are certainly Local group members, and likely dSph galaxies at a distance similar to that of the Andromeda galaxy. Cam A seems to be a star forming galaxy

A Fourier analysis of the intensity distribution in the planes of nine spiral galaxies is performed. In terms of the arm classification scheme of cite[Elmegreen & Elmegreen (1987)]{ee87} seven of the galaxies have well-defined arms (classes 12 and 9) and two have intermediate-type arms (class 5). The galaxies studied are NGC 157, 753, 895, 4321

Time series of high-resolution white-light images of six solar pores, observed in 1993 and 1995 at the Swedish Vacuum Solar Telescope (La Palma), are analyzed. The pores constitute an almost ideal laboratory in which to study the interaction of a vertical magnetic field with surrounding convective motions, without the perturbation of the inclined

Not Available

We have performed a study of the influence of the environment on the rate of star formation (SFR) in a sample of galaxies in nearby compact groups. The sample has been chosen from the Catalog of Hickson Compact Groups of Galaxies. High‐quality Hα images of the sample of galaxies in 16 compact groups were obtained and combined with additional deep