Earth-like planets hosting systems: architectures and properties

The search for Earth-like planets is a subject of great importance in the world of planetology today. Detecting such planets is challenging and requires a great deal of observation time. With future missions such as PLATO or LIFE, one of the main objectives of which is to detect small, moderate-temperature planets like the Earth, it is important to understand in what types of systems these plants form and around which stars we can expect to detect them. We present here a theoretical statistical study of the most favorable conditions for a planetary system to host an ELP (Earth-like planet). Based on three populations of synthetic planetary systems generated using the Bern model around three different types of stars, this study aims to create a profile of a typical system that harbors an ELP. By using an observational bias, we generate new populations that can be compared to observed systems. We initially examine the distribution of ELPs across different categories of theoretical and observed architectures. The changes in architecture resulting from the application of a bias are also investigated, highlighting the relationship between "theoretical" and "biased" architectures. A more detailed analysis is then conducted, linking the “biased” architecture of a system with the physical properties of its innermost observable planet, in order to establish the most favorable conditions for the presence or absence of an ELP in a system. Several quantities, such as the mass, radius, period and water fraction of this planet, emerge as correlated with the presence or the absence of an ELP.