The Martian moons Phobos and Deimos have numerous characteristics common to other small bodies of the solar system (small moons or asteroids), i.e. a small size, irregular shape, heavily cratered surface, reflectance spectra of the surface, surface features like grooves or boulders, and low bulk density. Some of these characteristics have been used to argue that the Martian satellites are asteroids captured by Mars. Alternative scenarios, like accretion in Mars’ orbit, have been proposed, which are also compatible with the surface or bulk characteristics of these two small bodies. The later theory has also been proposed for the small-sized Saturnian moons, and is also being studied for the Martian moons.
The goal of the session is to summon results of various analyses like interpretation of surface observations, interior modeling, or dynamics, in order to decipher which common features are the most relevant to the origin and evolution of Phobos, Deimos and other small bodies of the solar system.
We are inviting contributions presenting studies on the origin and fate, comparative studies, new findings, spacecraft observations, ground-based measurements, current and future research opportunities of Phobos, Deimos and other small solar system bodies.