Earth-Moon formation

Earth’s Moon might have played an important role in the development and evolution of life on Earth. The Moon was formed via a giant impact in which a Mars-size projectile collided with the young Earth. The ejected material accumulated in orbit around our planet and formed the Moon.

After its formation, the Moon was much closer to Earth than it is today, which caused high tides several times per day. This may have helped promote the very early evolution of life.



Above: An artist impression shows a potential satellite-forming impact on a proto-planet.   Image credit Michael Elser, University of Zurich

In addition, a stable climate of more than a billion years may be essential to guarantee a suitable environment for life. But without its satellite, Earth would suffer chaotic variations of the direction of its spin axis, which would in turn result in dramatic variations of the climate.

Therefore, concerning the habitability of extrasolar planets, it is reasonable to ask: How common are Earth-Moon planetary systems? Sebastian Elser, Prof. Ben Moore and Dr. Joachim Stadel of the University of Zurich, Switzerland, along with Ryuji Morishima of NASA’s Jet Propulsion Laboratory in Pasadena, California, ran a large set of N-body simulations to study the formation of the rocky planets in our solar system via the collisional growth of thousands of small rocky bodies in a disk around the Sun. They identified numerous satellite-forming collisions during this process and estimated the masses of the generated companions.

Moreover, they took into account the orbital evolution of the satellites, since tidal forces change the spin and orbit of a satellite and can cause it to be lost within a few thousand years in the most extreme cases. Finally, they studied the subsequent collision history, since giant impacts after the epoch of satellite formation may pose a challenge to the survival of a satellite. They find that Earth-Moon planetary systems occur relatively frequently, with more than 1 in 12 terrestrial planets hosting a massive moon. Uncertainties in the study result in a range of 1 in 4 to 1 in 45. Further work and more N-body simulations are needed to obtain more precise results.



This work is being presented at the Extreme Solar Systems II conference in Jackson, Wyoming, and appears in the August 2011 issue of Icarus. The research was financially supported by the University of Zurich.

Extreme Solar Systems II website: http://ciera.northwestern.edu/Jackson2011/

Icarus paper: http://dx.doi.org/10.1016/j.icarus.2011.05.025< /a> http://arxiv.org/abs/1105.4616 (preprint)



Caption 1: This evolutionary “merger tree” illustrates the collision history between the initially small rocky bodies that result in the formation of a single planet-satellite system from one of our simulations. The root of the tree is the final planet and the branches show the numerous collisions that take place early on. The width of the lines give the size of the forming planet, and every knee in the tree illustrates when a merger occurs between two objects. The red branch shows the history of the giant impactor that leads to the formation of the planet’s moon.