The fundamental and unifying line of work is the theoretical studies of the solar and stellar interiors by means of state-of-the-art structure and evolution models.
Our ultimate goal is to develop and test the most accurate solar and stellar models, and then use these models to address several scientific issues. The development of models is carried out along several paths: improvement of the microphysics used in the models (nuclear reaction rates, opacities, equation of state), better modelling of physical processes (e.g. near-surface convection based on 3D hydrodynamic models) and numerical techniques. Models are tested on several different constraints from helioseismology to eclipsing binaries to asteroseismology, also complemented with parallaxes from Gaia.
Some of the scientific problems we are interested in addressing are: the solar abundance problem, solar models for particle physics including work on solar neutrinos, and constraints on exotic properties of matter (e.g. magnetic neutrino dipole) and/or properties of exotic matter (e.g. dark matter candidates). Also, we are interested in any application of stellar models to astrophysical problems. Based on spectroscopic, photometric, asteroseismic and astrometric data (any combination thereof) we work on the characterisation of stellar properties that enable studies from individual objects (such as planet hosting stars) or large-scale populations. For attacking some of these topics, we have also developed BeSPP (Bellaterra Stellar Parameters Pipeline), a state-of-the-art statistical analysis tool based on Bayesian statistics that allow inference of stellar parameters based on different classes of input data and a large library of stellar models containing about 100 million models.
We are part of the Gaia-ESO survey, the Kepler and K2 mission, and are external collaborators in APOGEE, the SDSS-IV experiment for galactic archaeology. We are also members of the Steering Committee of the working group of solar like oscillators of the oncoming NASA mission TESS.