The study of polarized dust emission has become entwined with the analysis of the cosmic microwave background (CMB) polarization in the quest for the curl-like B-mode polarization from primordial gravitational waves and the low-multipole E-mode polarization associated with the reionization of the Universe. We used the new Planck PR3 maps to

Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical

This work presents the study of wave propagation and the Rayleigh-Taylor instability in the solar atmosphere using a two-fluid model. The solar atmosphere is strongly stratified and permeated by magnetic fields with a complex configuration, thus creating very different regimes throughout its layers. Of the different layers of the solar atmosphere

En el presente artículo se aborda la tan debatida cuestión de las orientaciones de ciudades romanas combinando dos procedimientos: un análisis estadístico de las orientaciones de una muestra significativa de ciudades romanas en la península ibérica, y los resultados de una investigación basada en la experimentación y reconstrucción de instrumental

This thesis addresses several topics in the study of the more massive and O-rich asymptotic giant branch (AGB) stars in our Galaxy. In particular, the main goals are the exploration of the circumstellar effects on the abundance determination in solar metallicity massive AGB stars by using more realistic pseudo-dynamical model atmospheres and the

El objetivo principal de esta tesis es estudiar la evolución de las galaxias formadoras de estrellas durante los últimos 7 Gyrs. Las galaxias formadoras de estrellas de alto desplazamiento al rojo (z>1) difieren de sus contrapartidas locales en varios aspectos clave. Sus regiones formadoras de estrellas son de un orden de magnitud más grandes y