In 2005,the Japanese spacecraft Hayabusa  revealed that the near-Earth asteroid (25143) Itokawa  has a strange peanut shape, leading to questions about why. Now, using ground-based observations, a group has measured the speed at which Itokawa spins and how that spin rate is changing over time and combined these observations with theoretical work on how asteroids radiate heat.

To probe its internal structure, Stephen Lowry of the University of Kent and colleagues used images gathered from 2001 to 2013. They analyzed images from  ESO's New Technology Telescope (NTT) at the La Silla Observatory in Chile, Palomar Observatory 60-inch Telescope (California), Table Mountain Observatory (California), Steward Observatory 60-inch Telescope (Arizona), Steward Observatory 90-inch Bok Telescope (Arizona), 2-metre Liverpool Telescope (La Palma), 2.5-metre Isaac Newton Telescope (La Palma) and the Palomar Observatory 5-meter Hale Telescope (California).

To measure its brightness variation as it rotates. This timing data was then used to deduce the asteroid's spin period very accurately and determine how it is changing over time. When combined with knowledge of the asteroid's shape this allowed them to explore its interior — revealing the complexity within its core for the first time. The density of the interior was found to vary from 1.75 to 2.85 grammes per cubic centimeter. The two densities refer to Itokawa’s two distinct parts.




A schematic view of the strange peanut-shaped asteroid Itokawa. The shape model used for this view is based on the images collected by JAXA's Hayabusa spacecraft. Credit: ESO. Acknowledgement: JAXA)

"This is the first time we have ever been able to to determine what it is like inside an asteroid," explains Lowry. "We can see that Itokawa has a highly varied structure — this finding is a significant step forward in our understanding of rocky bodies in the Solar System."

The spin of an asteroid and other small bodies in space can be affected by sunlight. This phenomenon, known as the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, occurs when absorbed light from the Sun is re-emitted from the surface of the object in the form of heat. When the shape of the asteroid is very irregular the heat is not radiated evenly and this creates a tiny, but continuous, torque on the body and changes its spin rate. A rough analogy for the YORP effect; if one were to shine an intense enough light beam on a propeller it would slowly start spinning due to a similar effect. Lowry and colleagues were the first to observe the effect in action on a small asteroid known as 2000 PH5, now known as 54509 YORP. 


They measured that the YORP effect was slowly accelerating the rate at which Itokawa spins. The change in rotation period is tiny — a mere 0.045 seconds per year. But this was very different from what was expected and can only be explained if the two parts of the asteroid's peanut shape have different densities.

This is the first time that astronomers have found evidence for the highly varied internal structure of asteroids. Up until now, the properties of asteroid interiors could only be inferred using rough overall density measurements. This rare glimpse into the diverse innards of Itokawa has led to much speculation regarding its formation. One possibility is that it formed from the two components of a double asteroid after they bumped together and merged.

Lowry added, "Finding that asteroids don't have homogeneous interiors has far-reaching implications, particularly for models of binary asteroid formation. It could also help with work on reducing the danger of asteroid collisions with Earth, or with plans for future trips to these rocky bodies."

This new ability to probe the interior of an asteroid is a significant step forward, and may help to unlock many secrets of these mysterious objects.


Paper: “The Internal Structure of Asteroid (25143) Itokawa as Revealed by Detection of YORP Spin-up”, by Lowry et al., upcoming in the journal Astronomy  &  Astrophysics. Source: ESO