EN LA PRESENTE TESIS SE ABORDA UNO DE LOS TEMAS DE MAS INTERES Y ACTUALIDAD DE LA FISICA SOLAR Y EN GENERAL DE LA ESTRUCTURA Y EVOLUCION ESTELAR. LA TECNICA DE OBSERVACION EL GRAN NUMERO DE ELLAS Y SU RIGUROSO ANALISIS HAN PERMITIDO LA DETECCION DE LOS MODOS GRAVITATORIOS DEL ESPECTRO DE OSCILACIONES SOLARES. SU IMPORTANCIA ES EXTRAORDINARIA POR

SE PONE EN PRACTICA DOS TECNICAS DE ALTA RESOLUCION ESPACIAL YA EN USO EN POCOS OBSERVATORIOS OPTIMIZANDO SU RENDIMIENTO. SE DISEÑA CONSTRUYE Y PRUEBA UN NUEVO INTERTEROMETRO QUE MEJORA OSTENSIBLEMENTE LA SENSIBILIDAD RESPECTO A LA TECNICA UTILIZADA HABITUALMENTE. SU IMPORTANCIA ESTRIBA EN LA CAPACIDAD DE RESOLVER LA ESTRUCTURA DE FUENTES

Not Available

The intensities obtained by measurement of the emission lines of neutral and ionized He at visible wavelengths in the April 24, 1981 white light flare are used as an observational basis for future radiative transfer models of such flares. Absolute peak and integrated intensities are given for the 14 lines of He I, as well as for the He II line at

Radial velocity measurements of the sun as a star using a resonant scattering spectrometer have been obtained at Izaña (Tenerife) during long observing seasons from 1976 to 1985. Its analysis shows that except for the global oscillations with periods shorter than one day there are stable signals with longer periods: at ≡13 days with mean amplitude

The publication by Lloyd (1984) of new and revised data for a sample of active nuclei brought the number of published observations of 3C 345 up to over 900, between 1965 and 1980. Since the last major study, by Barbieri et al. (1977), sufficient new data has been produced to merit a complet revision of previous analysis. A compilation of the