This research line aims at testing the details of the internal stellar structure using different observational approaches: Exploitation of seismic data from space satellites, ground support and follow-up of these space missions and also the study of binary stars in other galaxies.
To do this several theoretical tools have been developed, among them, numerical codes of stellar structures, numerical codes for non-adiabatic stellar pulsations and numerical codes for stellar rotation. We have also developed precise time series analysis to extract pulsation frequencies for truncated time series. This
experience is being used to participate in the French-European mission COROT and in the future USA mission Kepler, in the ESA mission PLATO and in the proposed Spanish-BRITE nanosatellite. It is important to note the group responsible of this research line is co-leading the high resolution infrared spectrograph CARMENES for the 3.5m CAHA telescope.
Particularly the main objective is to study in detail the internal structure of stars using either their membership to a binary system or their oscillations. Many theoretical stellar structures are possible with the usual external observables: effective temperature, gravity, surface abundance. The most obvious example is that of pulsating
pre-main sequence stars occupying the same position in the HR diagram as main sequence classical pulsators. The detail of how stars transport energy and momentum from its deep core is not yet understood. Our group is completely autonomous to carry out the modelling of any type of stellar structure test: the data coming from space mission and supported by simultaneous ground based additional observations are analysed and compared with theoretical predictions.
The feedback generated by this test bench is in the basis of our objectives. A non-exhaustive list of items to be addressed by these techniques are:
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