We monitored the light variations of 58 weak-line T Tauri stars in Taurus, recently discovered in the X-ray wavelength range during the ROSAT All-Sky Survey. We derive photometric periods for 18 stars, all but one being ascribed to rotational modulation by stellar spots. The exception is a 37.6d period assigned to the orbital motion of a new pre

EL TRABAJO RECOGIDO EN LA PRESENTE MEMORIA DESCRIBE UN EXPERIMENTO ENCAMINADO HACIA LA DETECCION DE MODOS GRAVITATORIOS SOLARES. LOS DATOS TOMADOS EN EL OBSERVATORIO DEL TEIDE ENTRE LOS AÑOS 1991 Y 1993, CONSISTEN EN MEDIDAS DIARIAS DE VELOCIDAD SOLAR OBTENIDAS SECUENCIALMENTE EN SEIS POSICIONES DIFERENTES Y SIMETRICAS SOBRE EL DISCO SOLAR. EL

Knowledge of the solar irradiance background is of great importance to solar and stellar physics. In particular, its contribution to the solar oscillations power spectrum is highly relevant as it represents the ultimate limit to the sensitivity of solar oscillations' observations. An analysis of the power spectra of the solar photometric data

A low dispersion objective-prism survey for low-redshift emission-line galaxies (ELGs) is being carried out by the University Complutense de Madrid with the Schmidt telescope at the German-Spanish Observatory of Calar Alto (Almeria, Spain). A 4° full aperture prism, which provides a dispersion of 1950Å/mm, and IIIa-F emulsion combination has been

For the first time have been able to observe and combine a large number of observables for two SO galaxies NGC 5689 and NGC 7332, in order to apply a detailed analysis of their constituent stellar populations. We will discuss our main results from the present study of the two SO galaxies NGC 5689 and NGC 7332, on the basis of our single-age, single

We report here first results concerning stellar oxygen abundances in M33. Non-LTE model atmosphere and non-LTE line formation calculations were used to determine the oxygen abundance of B-type supergiants. By choosing stars located at different projected radial distances to the center of M33, we are able to determine the oxygen abundance gradient