[meteorite-list] Seismic Shaking Erased Small Impact Craters On Asteroid Eros

From: Ron Baalke <baalke_at_meteoritecentral.com>
Date: Fri Nov 26 13:42:11 2004
Message-ID: <200411261842.KAA12382_at_zagami.jpl.nasa.gov>

SEISMIC SHAKING ERASED SMALL IMPACT CRATERS ON ASTEROID EROS
>From Lori Stiles, UA News Services, 520-621-1877
November 26, 2004

University of Arizona scientists have discovered why Eros, the largest
near-Earth asteroid, has so few small craters.

When the Near Earth Asteroid Rendezvous (NEAR) mission orbited Eros from
February 2000 to February 2001, it revealed an asteroid covered with
regolith -- a loose layer of rocks, gravel and dust -- and embedded with
numerous large boulders. The spacecraft also found places where the regolith
apparently had slumped, or flowed downhill, exposing fresh surface
underneath.

But what NEAR didn't find were the many small craters that scientists
expected would pock Eros' landscape.

"Either the craters were being erased by something or there are fewer small
asteroids than we thought," James E. Richardson Jr. of UA's planetary
sciences department said.

Richardson concludes from modeling studies that seismic shaking has
obliterated about 90 percent of the asteroid's small impact craters, those
less than 100 meters in diameter, or roughly the length of a football field.
The seismic vibrations result when Eros collides with space debris.

---------------------------------------------------
Contact Information
 James E. Richardson 520.621.6960 jrich_at_lpl.arizona.edu

Related Web site
http://www.lpl.arizona.edu/~jrich/
-----------------------------------------------------

Richardson, Regents' Professor H. Jay Melosh and Professor Richard
Greenberg, all with UA's Lunar and Planetary Laboratory, report the analysis
in the Nov. 26 issue of Science.

"Eros is only about the size of Lake Tahoe -- 20 miles (33 kilometers) long
by 8 miles (13 kilometers) wide," Richardson said. "So it has a very small
volume and a very low gravity. When a one-to-two-meter or larger object hits
Eros, the impact will set off global seismic vibrations. Our analysis shows
how these vibrations easily destabilize regolith overlaying the surface."

A rock-and-dust layer creeps, rather than crashes, down shaking slopes
because of Eros' weak gravity. The regolith not only slides down
horizontally, but also is launched ballistically from the surface and 'hops'
downslope. Very slowly, over time, impact craters fill up and disappear,
Richardson said.

If Eros were still in the main asteroid belt between Mars and Jupiter, a
200-meter crater would fill in about 30 million years. Because Eros is now
outside the asteroid belt, that process takes a thousand times longer, he
added.

Richardson's research results match the NEAR spacecraft evidence. Instead
of the expected 400 craters as small as 20 meters (about 70 feet) per square
kilometer (three-fifths mile) on Eros' surface, there are on average only
about 40 such craters.

The modeling analysis also validates what scientists suspect of Eros'
internal structure.

"The NEAR mission showed Eros to most likely be a fractured monolith, a
body that used to be one competent piece of material," Richardson said. "But
Eros has been fractured throughout by large impacts and is held together
primarily by gravity. The evidence is seen in a series of grooves and ridges
that run across the asteroid's surface both globally and regionally."

Large impacts fracture Eros to its core, but many smaller impacts fracture
only the upper surface. This gradient of big fractures deep inside and
numerous small fractures near the surface is analogous to fractures in the
upper lunar crust, Richardson said. "And we understand the lunar crust --
we've been there. We've put seismometers on the moon. We understand how
seismic energy propagates through this kind of structure."

The UA scientists' analysis of how impact-induced seismic shaking has
modified Eros' surface has a couple of other important implications.

"If we eventually do send spacecraft to mine resources among the near-Earth
asteroids or to deflect an asteroid from a potential collision with the
Earth, knowing internal asteroid structure will help address some of the
strategies we'll need to use. In the nearer future, sample return missions
will encounter successively less porous, more cohesive regolith as they dig
farther down into asteroids like Eros, which has been compacted by seismic
shaking," Richardson noted.

"And it also tells us about the small asteroid environment that we'll
encounter when we do send a spacecraft out into the main asteroid belt,
where Eros spent most of its lifetime. We know the small asteroids -- those
between the size of a beachball and a football stadium -- are out there.
It's just that their 'signature' on asteroids such as Eros is being erased,"
Richardson said.

This finding is important because the cratering record on large asteroids
provides direct evidence for the size and population of small main-belt
asteroids. Earth-based telescopic surveys have catalogued few main-belt
asteroids that small. So scientists have to base population estimates for
these objects primarily on visible cratering records and asteroid
collisional history modeling, Richardson said.
Received on Fri 26 Nov 2004 01:42:06 PM PST