Formation of Massive Rocky Exomoons by Giant Impact

Abstract

The formation of satellites is thought to be a natural by-product of planet formation in our Solar System, and thus, moons of extrasolar planets (exomoons) may be abundant in extrasolar planetary systems, as well. Exomoons have yet to be discovered. However, moons larger than 0.1 Earth masses can be detected and characterized using current transit techniques. Here, we show that collisions between rocky planets with masses between a quarter to ten Earth masses can create impact-generated debris disks that could accrete into moons. Collisions between like-sized objects, at oblique impact angles, and velocities near escape speed create disks massive enough to form satellites that are dynamically stable against planetary tides. Impacts of this type onto a superearth between 2 to 7 Earth masses can launch into orbit enough mass to create a satellite large enough to be detected in Kepler transit data. Impact velocity is a crucial controlling factor on disk mass, which has been overlooked in all prior studies of moon formation via planetary collision.

arXiv comment8 pages, 7 figures

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Cited by in corpus (6)

• Laboratory spectra of hot molecules: data needs for hot super-Earth exoplanets
• Exomoon Candidates from Transit Timing Variations: Eight Kepler systems with TTVs explainable by photometrically unseen exomoons
• Collisional formation of massive exomoons of super-terrestrial exoplanets
• A Pluto-Charon Sonata III. Growth of Charon from a Circum-Pluto Ring of Debris
• The effect of post-Newtonian spin precessions on the evolution of exomoons' obliquity
• Special cases : moons, rings, comets, trojans