Outer solar system not as crowded as astronomers thought

Astronomers found fewer objects in Kuiper Belt than thought.Provided by the Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts
By | Published: October 3, 2008 | Last updated on May 18, 2023
Collision in the Edgeworth-Kuiper Belt
The Edgeworth-Kuiper Belt is named for British astronomer Kenneth Edgeworth and Dutch-American astronomer Gerard Kuiper. (Many refer to it as simply the Kuiper Belt.)
Dan Durda
October 3, 2008
When a treasure hunt comes up empty-handed, the hunters are understandably disappointed. But when astronomers don’t find what they are looking for, the defeat can provide as much information as a successful search.

The search in question, the Taiwanese-American Occultation Survey (TAOS), spent 2 years periodically photographing portions of the sky to look for small chunks of rock and ice orbiting beyond Neptune, in a region of the solar system called the Kuiper Belt. The survey targeted Kuiper Belt objects (KBOs) with sizes between 2 miles (3 kilometers) and 17 miles (28 km).

Because such objects are too small to see directly, the survey watched for stars to dim as KBOs passed in front of (occulted) them. After accumulating more than 200 hours of data watching for stellar flickers lasting a second or less, TAOS did not spot any occultations.

The Kuiper Belt contains objects in a range of sizes: a few very large ones (like the dwarf planets Pluto, Eris, Makemake and Haumea) and many more smaller ones. The similarity of a given size tells us information about the history of planet formation and dynamics. In particular, the size distribution of KBOs reflects a history of agglomeration, in which colliding objects tended to stick together, followed by destructive collisions, where collisional velocities were high enough to shatter the rocks involved.

Astronomers questioned whether they would find more and more objects as sizes decreased further, or whether the distribution leveled out. The fact that no occultations were seen sets a stringent upper limit on the number density of KBOs between 2 and 17 miles (3.2 and 27.3 kilometers) in diameter. The outer solar system hence appears not as crowded as some theories suggest, perhaps because small KBOs have already stuck together to form larger bodies or frequent collisions have ground down small KBOs into even smaller bits below the threshold of the survey.