PLAnetary Transits and Oscillations of stars



PLATO will be leading this effort by combining:

  1. planet detection and radius determination from photometric transits,
  4. identification of bright targets for atmospheric spectroscopy.




Searching for exoplanetary systems. Credit: ESA/C. Carreau

The Uniqueness of our Solar System

While the structure and mass distributions of bodies in our Solar System are well known, we only have indirect and partial knowledge of its formation and evolution. To place our system in context we must look to other systems and study their architectures and composition. From current observations, it has become obvious that the bulk compositions of exoplanets can differ substantially from those of Solar System planets and this must be indicative of the formation process. Thanks to PLATO, the density and composition of exoplanets will be obtained from the measured mass and the radius. In addition, important properties of host stars, such as chemical composition and stellar activity will be measured by PLATO and the associated ground-based follow-up for a large sample of systems. Extending the bulk characterisation towards cool terrestrial Earth-sized planets on Earth-like orbits will be unique to PLATO and key to answering the question: how unique is our Solar System?


Super-Earth exoplanets (1 < Mplanet ≤ 10 MEarth or Rplanet ≤ 2 REarth) for different host star masses in comparison with the position of the habitable zone (green) detected with different methods. As September 2016, there are several planets orbiting in the habitable zone, but we only know either their radius through transit observations (red dots) or their mass through radial velocity measurements (blue dots). Earth, Venus and Mars are shown for reference.


Interiors of terrestrial and gas planets

Many confirmed exoplanets fall into new classes unknown from our Solar System, for example "hot Jupiters", "mini-Neptunes", or "super-Earths" (rocky planets with masses below 10 MEarth). It came as a surprise that gaseous planets can be as small (or light) as a few Earth radii (or masses). As a result, many of the smallest (or lightest) exoplanets known today cannot be classified as either rocky (required for habitability) or gaseous, because their mean densities remain unknown for lack of mass or radius measurements. PLATO will be unique in providing vital constraints for planetary interior models.

Evolution of planetary systems

Planets and their host stars evolve. Giant gas planets cool and contract, a process which can last up to several billion years: this process will be studied by PLATO through accurate measurements of stellar ages. Using accurate radius and mass measurements, we will determine how planets form and evolve by observationally building evolutionary tracks for gaseous exoplanets as functions of stellar properties. Over time, terrestrial planets lose their primary hydrogen atmospheres, develop secondary atmospheres, and may develop life. PLATO will provide key data on terrestrial planets at intermediate orbital distances, including in the habitable zones of solar-like stars with different ages, allowing us to study Earth-like planets at different epochs. Furthermore, the architecture of planetary systems is shaped through physical and dynamical processes on time scales accessible to PLATO asteroseismic dating.

Planetary atmospheres and star-planet interactions

Planets discovered around the bright PLATO stars (mV = 4–11 mag) will be prime targets for spectroscopic transit follow-up observations of their atmospheres (using, e.g., JWST, E-ELT). Small planets with low mean density are particularly interesting as they are likely to have a primordial hydrogen atmosphere. Small planets with high densities are likely to be terrestrial planets with secondary atmospheres. The PLATO catalogue will therefore play a key role in identifying small planet targets of interest at intermediate orbital distances. It will also provide information on planetary albedos and the stratification of planetary atmospheres. Finally, the close-in planets found around stars of different types and ages will provide a huge sample to study the interaction between stars and planets due to, e.g., stellar winds or tides.

Structure and evolution of the Milky Way

The intrinsic luminosity of red giant stars allows us to probe distances up to 10 kpc in our Galaxy and determine accurate ages from asteroseismology. Red giants can thus be efficiently used to map and date the Galactic disc. These data will complement the information on distances and chemical composition obtained by the Gaia mission. In addition, asteroseismic ages provided for PLATO targets can be compared to age determinations by other means, for example to calibrate gyrochronology - the method of estimating stellar ages based on their rotational rates.