Research Projects

Research Group

Origin and Dynamics of Satellites

This project is developed within the framework of the Group of Origin and Dynamics of Satellites (GODS), a research group focused on the physical mechanisms driving the formation, orbital evolution, and detectability of natural satellites, both in the Solar System and in extrasolar planetary systems.

Visit the GODS page
Lunar Evolution

Evolution of the Volatile Content of the Primordial Moon

In this project, I investigate the primordial inventory of volatile and refractory elements in the proto-Moon, as well as the satellite's orbital evolution driven by tidal and disk torques, and how these processes influenced its final composition.

In particular, I focus on tidal-assisted hydrodynamic escape through hydrodynamical simulations and how this process unfolded within different models of lunar formation.

Moon

Relationship Between the Moon’s Shape and Its Primordial Magma Ocean

This project focuses on the magma ocean that likely covered the Moon shortly after its formation and its relationship with the satellite’s orbital evolution.

The Moon’s tidal evolution is investigated while accounting for extensive magma layers on both Earth and the Moon. The study examines the coupling between tidal dissipation and the thermal evolution of the magma ocean, along with the consequences for the Moon’s present-day shape.

Saturn System

Origin of Saturn’s Satellites from Ancient Rings

In this project, I investigate the hypothesis that Saturn's satellites formed through accretion from an ancient ring system using hydrodynamical simulations.

The study explores different models for the tidal evolution of the satellites, including migration induced by the planet’s gaseous envelope. It also examines how the primordial ring system evolved into Saturn’s present-day main rings.

Orbital Dynamics

Dynamics Around Asymmetric Bodies

This project investigates the dynamics around irregularly shaped bodies through N-body numerical simulations, stability maps, and chaos indicators.

Unlike larger bodies, which tend to be nearly spherical, smaller bodies may exhibit pronounced asymmetries capable of producing chaotic regions through eccentricity diffusion and the overlap of spin–orbit resonances.

The study analyses orbital stability around central bodies with different degrees of asymmetry, including the effects of additional gravitational fields and external perturbations.