Although located at 150 million kilometers from Earth, the Sun is in our immediate neighborhood compared with all other stars. The observation of the Sun along the decades has provided amazingly detailed views of the structure and day-to-day life of a star; the high-resolution observations achieved from Earth and space in recent years, in particular, have facilitated reaching deep theoretical insights concerning the structure and evolution of stellar atmospheres and interiors.
The Sun constitutes a physics laboratory where the complex interactions between the matter (atoms, electrons and ions, or molecules) and the magnetic field can be studied in conditions difficult to reach in devices on Earth. Of particular interest for the public are the spectacular phenomena displayed by its atmosphere, its role in generating the magnetized clouds that, after traversing the interplanetary space, can impact on Earth's magnetosphere and lead to the potentially dangerous solar storms, and the mysteries of the solar interior. Understanding of all those phenomena is gained by a combination of refined theoretical methods and direct or indirect observation using leading-edge technologies.
The solar physics group at the IAC enjoys a leadership position in different branches of solar research in the world. This is exemplified by the award of four large research grants by the European Research Council in the past years to researchers of the group, by its leading role in the European Solar Telescope project, and by its participation in other international networks and instrument projects. Globally, the group combines theoretical methods (magneto-fluid dynamics and plasma physics, radiation transfer), including 3D numerical radiation-MHD modeling, and state-of-the-art observational and diagnostic techniques, to achieve deep understanding of what constitutes and drives the structure and activity of our star.
Solar Physics (FS)
-
PublicationMOLPOP-CEP: an exact, fast code for multi-level systemsWe present MOLPOP-CEP, a universal line transfer code that allows the exact calculation of multi-level line emission from a slab with variable physical...
-
PublicationMorphology and Dynamics of Solar Prominences from 3D MHD SimulationsIn this paper we present a numerical study of the time evolution of solar prominences embedded in sheared magnetic arcades. The prominence is represented by a...
-
PublicationMorphology and evolution of umbral dots and their substructuresContext: Substructures - dark lanes and tails - of umbral dots (UDs) were predicted by numerical simulations of magnetoconvection and have been detected later...
-
ProjectMulti-Conjugate Adaptive Optics for ESTIAC is developing a Multi-Conjugate Adaptive Optics (MCAO) bench, with the purpose of demonstrating in laboratory solutions of some of the main problems related...
-
PublicationMulti-layer Study of Wave Propagation in SunspotsWe analyze the propagation of waves in sunspots from the photosphere to the chromosphere using time series of co-spatial Ca II H intensity spectra (including...
-
PublicationMulti-parametric Study of Rising 3D Buoyant Flux Tubes in an Adiabatic Stratification Using AMRWe study the buoyant rise of magnetic flux tubes embedded in an adiabatic stratification using two-and three-dimensional, magnetohydrodynamic simulations. We...
-
PublicationMultiline Spectropolarimetry of the Quiet Sun at 5250 and 6302 ÅThe reliability of quiet-Sun magnetic field diagnostics based on the Fe I lines at 6302 Å has been questioned by recent work. Here we present the results of a...
-
PublicationMultiline Stokes Synthesis of Ellerman Bombs: Obtaining Seamless Information from Photosphere to ChromosphereMagnetic reconnection in the lower atmosphere is a critical process in determining the chromospheric dynamics, such as Ellerman bombs and UV bursts. Because the...
-
PublicationMultiline Zeeman signatures through line additionContext: To obtain a significant Zeeman signature in the polarised spectra of a magnetic star, we usually “add” the contributions of numerous spectral lines...