Leo I and Leo II are the two most remote dSph galaxies satellites of the Milky Way, situated at about 250 Kpc of it. They are objects of similar size and low metallicity, but their star formation histories appear to be fundamentally different. The very deep HST color-magnitude diagrams (CMDs) of these galaxies reach the position of the oldest

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

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