How small inner moons of Saturn were formed

The small inner moons of Saturn look like giant ravioli and spaetzle. Their spectacular shape has been revealed by the Cassini spacecraft. For the first time, researchers of the University of Bern show how these moons were formed. The peculiar shapes are a natural outcome of merging collisions among similar-sized little moons as computer simulations demonstrate.

How small inner moons of Saturn were formed
Formation of Atlas, one of the small inner moons of Saturn. Its flat, ravioli-like shape is the result of a merging collision 
of two similar-sized bodies. The picture is a snapshot in mid-collision, before the moon’s reorientation 
due to tides is completed [Credit: A. Verdier]

When Martin Rubin, astrophysicist at the University of Bern, saw the images of Saturn’s moons Pan and Atlas on the internet, he was puzzled. The close-ups taken by the Cassini spacecraft in April 2017 showed objects that NASA described in its news release as flying-saucers with diameters of about 30 km. With their large ridges and bulbous centres, Pan and Atlas also resembled giant ravioli. Martin Rubin wondered how these peculiar objects had formed and asked his colleague Martin Jutzi whether they could be the outcome of collisions, similar to the one that formed comet Chury as Jutzi had demonstrated earlier with computer simulations.

How small inner moons of Saturn were formed
The top row shows 3 small moons of Saturn imaged by the Cassini spacecraft. Shown at the bottom are the model outcomes
. The simulations not only reproduce the shapes, but may also explain why the ridges on Pan and Atlas look different from 
the rest of their bodies: They are made of smooth material that was squeezed out during the merging process. Cracks 
on the main body could be the result of tensile stresses caused by the deformation of the merging objects. The modelled 
Prometheus-like moon displays the same tips at both ends as seen on the Cassini images 
[Credit: NASA/JPL-Caltech/Space Science Institute/University of Bern]

Martin Jutzi and Adrien Leleu, both members of the NCCR PlanetS, took the challenge of calculating the formation process of the small inner moons of Saturn. The first, simple tests worked well. “But then, we took the tidal forces into consideration and the problems piled up,” remembers Adrien Leleu. “The conditions close to Saturn are very special,” confirms Martin Jutzi. Since Saturn has 95 times more mass than Earth and the inner moons orbit the planet at a distance of less than half the distance between Earth and Moon, the tides are enormous and pull almost everything apart. Therefore, Saturn’s inner moons couldn’t have formed with these peculiar shapes by gradual accretion of material around a single core. An alternative model called pyramidal regime suggests that these moons were formed by a series of mergers of similar sized little moonlets.

How small inner moons of Saturn were formed
The top image shows Saturn’s large moon Iapetus as observed by Cassini. It has an 
oblate spheroid shape and an equatorial ridge. Bottom: The result of the simulation 
of a head-on merger oft two equal-sized bodies with half of the mass of Iapetus 
[Credit: NASA/JPL/Space Science Institute/University of Bern]

Having solved their initial problems, the researchers could verify the pyramidal regime, but even more: They showed that the collisions of the moonlets resulted in exactly the shapes imaged by Cassini. Close to head-on mergers lead to flattened objects with large equatorial ridges, as observed on Atlas and Pan. With slightly more oblique impact angles, collisions resulted in elongated spaetzle-like shapes that closely resembled the 90-km long moon Prometheus as it was photographed by Cassini.

Head-on collisions have high probability

Based on the current orbit of the moons and their orbital environment, the researchers were able to estimate that the impact velocities were of the order of a few 10 m/s. Simulating collisions in this range for various impact angles, they obtained various stable shapes similar to ravioli and spaetzle, but only for low impact angles. “If the impact angle is bigger than ten degrees, the resulting shapes are not stable anymore,” says Adrien Leleu. Any duck-shaped object like comet Chury would fall apart because of Saturn’s tides. “That is why Saturn’s small moons look very different to comets that often have bilobed shapes,” explains Martin Jutzi.

Collison of similar-sized moonlets orbiting around Saturn [Credit: Simulation by Adrien Leleu, 

Martin Jutzi and Martin Rubin / University of Bern]

Interestingly, the head-on collisions are not as rare as one might think. The small inner moons are believed to originate from Saturn’s rings, a thin disk located in the planet’s equatorial plane. Since Saturn isn’t a perfect sphere but rather oblate, it makes it hard for any object to leave this narrow plane. So, near head-on collisions are frequent and the impact angle tends to get even lower in subsequent encounters. “A significant fraction of such merging collisions take place either at the first encounter or after 1-2 hit-and-run events,” the authors summarize in their paper published in Nature Astronomy. “In this respect, Saturn is almost a toy system to study these processes,” says Martin Rubin.

Although the researchers mainly focussed on the small inner moons of Saturn, they also found a possible explanation for a long-standing mystery concerning Saturn’s third largest moon named Iapetus. Why does Iapetus have an oblate shape and a distinctive equatorial ridge? “Our modelling results suggest that these features may be a result of a merger of similar-sized moons taking place with a close to head-on impact angle, similar to the smaller moons,” the researchers summarize.

Source: University of Bern [May 22, 2018]

TANN

Archive

Leave a Reply

Your email address will not be published.