| <fc #800080>Objectives Summary</fc> | ||
|---|---|---|
| # | Brief Description | Period |
| 1 | Coordinate the PLATO2.0 WP121,130 (PSPM) activities in preparation to PDR | M01-M36 |
| 2 | Coordinate the PLATO2.0 WP375,300 (PDC) activities in preparation to PDR | M12-M24 |
| 3 | Study the rotation-pulsation interaction in intermediate-mass stars | M12-M24 |
| 3.1 | Asteroseismic modeling of rotating stars using SCF models. Develop interface between 1D and 2D models and tests | M12-M24 |
| 4. | Study asteroseismic properties of A-F stars through statistical methods (periodicities) | M12-M24 |
| 4.1 | Find rotation signatures (uniform and radial-differential) | M12-M24 |
| 4.2 | Study the impact of gap-filling methods on the FT method for finding periodicities | M12-M24 |
| 5. | Explore more realistic star-planet gravitational interaction for planetary systems characterization | M12-M24 |
Objective #1 Development of accurate gap-filling method for PLATO2.0
Here we write more in detail the description of the objective and everything we consider important.
Objective #2 Other interesting stuff
Here we write more in detail the description of the objective and everything we consider important.
Objective #5 Explore more realistic star-planet gravitational interaction for planetary systems characterization
Current observational techniques of extrasolar planets such as transits or radial-velocity measurements have revolutionized the detection of them, providing with a large number of planets already detected, and increasing number of candidates. However, these techniques are more sensitive to those planets whose orbits are close to the host star and which sizes are about Jupiter mass. These planets will experience significant tidal forces as a result of their proximity to the host star. Tides are generated both on the planet due to the potential of the star, and on the star due to the planet. These tidal forces are generally expected to lead to the alignment of their rotations axes, synchronization of their rotation and orbital periods, a reduction in orbital ellipticity, an accompanying reduction in semi-major axis, and a conversion of the orbital energy into tidal heating of the planet. The time scales are believed to be very long, in the order of 1 Gyr, but effects on the planet's orbit and its thermal heating can nonetheless be very significant. On the other hand, tidal evolution is a very complex problem, as a consequence the most of the previous studies do not take it into account. Our aim is to explore tidal problem and determine how affects to the planetary system configuration.
- La coordinación se justifica porque estudiamos aspectos teóricos de la dinámica que se complementan perfectamente con las caracterizaciones de los planetas que se hace en el IAC. - Como primera aproximación nos vamos a centrar en la dinámica de planetas gigantes muy cercanos a sus estrellas, donde los efectos gravitatorios son importantes. - Como ahora hay ya observaciones de muchos sistemas planetarios, se puede establecer una metodología.
Notes for the preparation
Mencionar: PERSIA, SpaceInn, Explora, y OPTOCAM- Coger información de la solicitud Severo Ochoa del año anterior (Rafa pide al director)
- Extraer info de PERSIA