Ramón y Cajal fellow.

  My main line of research focuses on the modeling and interpretation of the Sun’s polarized spectrum in order to unveil the magnetic, thermal, and dynamical structure of the (outer) solar atmosphere. Of relevance, the magnetic field is the common link throughout the atmosphere and the heliosphere, and it is at the heart of almost every physical phenomenon happening on the Sun. It shapes solar activity and it is key for the already more than 100-year old, unsolved problem of the heating of the outer atmosphere (chromosphere, transition region, and corona) of the Sun and other convective stars.

  Interpreting spectro-polarimetric observations of spectral lines tracing the outer layers of the Sun is challenging because they are formed in non-local thermodynamic equilibrium (non-LTE) conditions and their modeling requires complex quantum mechanical and matter-radiation interaction effects that restrain the creation of numerical tools for such a purpose. Modeling the spectral line polarization accounting for these physical ingredients is very computationally intensive, and sophisticated and efficient numerical codes are required to carry out this kind of research. My work has been focused on the development of state-of-the-art (public) software devoted to the study of the magnetism and thermodynamics of the outer atmosphere of the Sun.

  Public codes:
     - HanleRT-TIC: 1.5D synthesis and inversion of spectropolarimetric profiles. gitlab [dot] com/TdPA/hanlert-tic
     - PORTA: 3D synthesis of spectropolarimetric profiles. gitlab [dot] com/polmag/PORTA
     - P-CORONA: Optically thin synthesis of spectropolarimetric profiles of coronal lines. gitlab [dot] com/polmag/P-CORONA