The triplet of the He I transitions around 10830 Å not only shows a rich variety of Stokes profiles, but also allows the full magnetic vector in the upper chromosphere to be probed, thus revealing the magnetic structure of loops, current sheets, finely structured supersonic downflows, the chromospheric layers of sunspots (supporting the presence of

The quiet Sun photospheric plasma has a variety of magnetic field strengths going from zero to 1800 G. The empirical characterization of these field strengths requires a probability density function (PDF), i.e., a function P(B) describing the fraction of quiet Sun occupied by each field strength B. We present a method to combine magnetic field

EL ESTUDIO DE LA GENERACION Y LA PROPAGACION DE ONDAS EN LA ATMOSFERA SOLAR ES UN TEMA CANDENTE EN LA INVESTIGACION ASTROFISICA ACTUAL, YA QUE PROPORCIONA INFORMACION SOBRE LA ESTRUCTURA Y LA DINAMICA DE LAS ATMOSFERAS DE LAS ESTRELLAS DE TIPO SOLAR AL MISMO TIEMPO QUE NOS AYUDA A COMPRENDER LOS MECANISMOS DE CALENTAMIENTO CROMOSFERICO Y CORONAL

We present an analysis of simultaneous observations of a sunspot in two different spectral ranges (630 nm and 1565 nm). The dataset was acquired with the POlarimetric LIttrow Spectrograph (POLIS) and the Tenerife Infrared Polarimeter (TIP) at the German Vacuum Tower Telescope (VTT) of Observatorio del Teide. Inversions of both sets of lines are

We took simultaneous observations in Fe I 1.5 µ and Fe I 630 nm of an internetwork region. We discuss the compatibility of the data in the two spectral ranges, and present results for the magnetic field distribution. We show that the larger contribution comes from hG field strengths.

¿Como se forman las galaxias?, ¿Cómo evolucionan?. Éstas son cuestiones fundamentales que las cartografiados profundos de galaxias a alto desplazamiento al rojo tratan de resolver. Una segunda aproximación es reconstruir la historia de la formación estelar a través de sus poblaciones estelares resueltas. La Historia de formación estelar de una