EL FIN PRINCIPAL DE LA SISMOLOGIA ESTELAR ES OBTENER INFORMACION ACERCA DE LA ESTRUCTURA DE EQUILIBRIO DE LAS ESTRELLAS A PARTIR DE LAS FRECUENCIAS DE SUS MODOS PROPIOS DE OSCILACION. EN ESTE TRABAJO SE HA CONSIDERADO PRINCIPALMENTE LA INFLUENCIA DE LAS CAPAS MAS ALTAS DE LOS INTERIORES ESTELARES EN LAS FRECUENDE LOS MODOS P, HACIENDO UN ESTUDIO

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Two sources selected from the IRAS Point Source Catalogue (PSC) have been spectroscopically identified as galaxies with a Seyfert type active nucleus. The brightest of the first source, IRAS 20210 + 1121, is in close interaction with a companion galaxy at a projected distance of 1.1 kpc and has a perturbed spiral-like morphology. This galaxy

A new method to measure the magnetic field strength of small-scale solar magnetic concentrations is presented. It is based on the center of gravity method (Semel, 1967), is independent of radiative transfer calculations and only observable parameters are needed. This method also provides parameters like filling factor (area fraction occupied by the

We report detailed spatially resolved spectroscopy of the WR nebulae NGC 2359 and RCW 78 surrounding the WN 5 HD 56925 and WN 8 HD 117688 stars. The aim of this work has been to study possible abundance inhomogeneities and the ionization structure of the nebulae, as well as to derive reliable values for the degree of self-enrichment. In NGC 2359

Simultaneous ultraviolet/optical spectrophotometry and infrared photometry for the low excitation symbiotic star BF Cygni are presented. The analysis of the data suggests that three different components are present in the UV to IR energy distribution. A hot subdwarf with R = 0.48 solar radius and T not less than 60,000 K if the distance is 2.3 kpc