Can Binary Terrestrial Planets Exist?
The possible existence of Earth-like binary planets is being described today at the American Astronomical Society’s Division for Planetary Sciences meeting in Tucson, AZ. Two bodies, each of mass similar to Earth, can form a closely orbiting pair under certain conditions present during the formation of planetary systems. This theoretical proposal is completely unlike the Earth-Moon system or Pluto-Charon, where the two bodies are very different in mass, and arises in some “kissing” collisions where two similar mass bodies encounter each other and become a bound system because of the energy lost in the strong tides raised on each other in the encounter. The resulting binary can then persist for billions of years provided it forms well away from the central star, at half an astronomical unit (the distance between the Earth and Sun) or more. This work is being presented by undergraduate Keegan Ryan, graduate student Miki Nakajima, and Dr. David Stevenson of the California Institute of Technology in Pasadena, CA. The result does not contradict existing data for planets around other stars but suggests that future data may uncover such systems. This is the first such study to examine the possibility of terrestrial binary planets.
During the formation of terrestrial planets, large rocky bodies orbiting around a star occasionally get close enough to interact with one another. If two bodies collide head on or obliquely, then this interaction typically results in accretion where the two bodies merge to form a larger one, perhaps leaving behind a disk of debris from which a moon can form. This is the standard picture for how Earth got its moon and a possible explanation for Pluto’s moon, Charon. If the two bodies collide in a grazing manner but at high velocity, then the two bodies “hit and run” and separate from one another once again, failing to form a bound pair. The research presented today searched for a middle ground — a scenario in which the interaction results in two large bodes that do not merge but still remain locked in orbit. This configuration, termed a terrestrial binary planetary system, would necessarily evolve into a state where the two bodies are tidally locked (with orbital period being almost the same as day length for both planets) and with the centers of the two planets being separated by only three or so planet radii (just like the animation in http://en.wikipedia.org/wiki/Double_planet).
There is a good reason to believe terrestrial binary planetary systems may be possible. In a grazing collision the angular momentum is too high to be contained within a single rotating body (it would fission) and if the bodies barely touch then they could retain their identity. However, it requires an encounter where the bodies are initially approaching each other at low enough velocity.
To test for this possibility, a simulation technique called Smoothed Particle Hydrodynamics (SPH) was utilized. Smoothed Particle Hydrodynamics represents a body as a collection of tens of thousands of particles, and it has been used to study protoplanetary collisions as well as the giant impact hypothesis of the Moon’s formation.
Using SPH, collisions between two rocky Earth-sized bodies were simulated, with impact velocity and impact parameter (a measure of how head-on a collision is) being varied and the output observed. In the cases where the bodies underwent substantial collision,
replicated previous results in which a binary system did not arise but a moon might form. However, by including interactions where the bodies are close enough to undergo a large tidal distortion, initial conditions were found that led to a terrestrial binary planetary system.
Despite the specialized computer hardware used to speed up the calculations, each simulation still took up to a week to run. Much of this time was spent simulating two bodies approaching one another, a situation which could be easily solved analytically. Using SPH during these stretches was unnecessary and time consuming. To combat this, a novel method was introduced to the SPH code which dynamically switched between modeling methods, cutting simulation time down to as little as a day.
With the simulation time long but manageable, the input space was mapped out. Some pairs of impact parameter and impact velocity led to accretion, some led to escape, and some even led to binary systems. Point by point the boundaries between these outcomes began to appear, eventually creating a map of the input space which would give rise to a binary system.
Binary asteroids are well established, and systems that have merged to become dumbbells or other shapes have also been detected. Binary stars are also very common. However, binary (or double) planets involving large bodies have only figured in science fiction to now, for example “Rocheworld,” by Robert Forward.
