NEAR Science Update: Cratering and Explosions
The craters on Eros are among its most spectacular and beautiful features. I
am not sure why, but I find something about rugged terrain to be exciting,
and I suspect it’s hard-wired in the human brain. For some reason, when
artists wish to inspire us, they paint intrepid explorers or ancient hermits
at the edge of a great cliff, or on a mountain top, or peering over clouds
into a magnificent valley – but whether the artists are 19th century
Americans or 11th century Chinese, they do not picture the subjects standing
in the midst of vast flat plains extending to the horizon. And when I talk
to people who live in flat country or who visit there, I often hear
complaints about the lack of topography, but I never hear of people being
inspired by flatness. Fortunately for those of us who like topography, on
Eros there is hardly a flat spot to be found.
Much of the ruggedness comes from the huge number of craters. We saw last
time how the density of craters allows us to infer relative ages of
surfaces, but there is much more we can learn. This is because a cratering
event excavates far below the surface of an object and thereby exposes its
interior, performing a natural experiment that we could not perform on our
own. Not only does this give us a chance to see what the interior is made
of, we can often infer mechanical properties of the target, using our
knowledge of how craters are formed.
We think that impacts on asteroids occur at a typical velocity of around 5
km/s. That is in itself a complicated story for another day, because it
reflects the distributions of bodies in the asteroid belt, or specifically
how many objects of a given size are found in a given orbit. The problem is,
the objects that would make the craters we now see on Eros are so small and
so far from Earth that we have no way to detect them – not even using the
Space Telescope – so we have no direct knowledge of how many such objects
there are or where they may be. Nevertheless, if we assume that these
objects, that we cannot see, have the same orbital distributions as the much
larger objects that we can see, then we can calculate the average speeds at
which objects would collide if their orbits happen to intersect. That is
where numbers like 5 km/s come from, and we don’t really know how good they
are.
High as these impact speeds are, they are small compared to the speeds at
which an asteroid would typically impact Earth (a very small asteroid, we
would hope). This is because of Earth’s gravity, which pulls any impactor
inward and accelerates it to speeds of 15 km/s or more, depending on where
the impactor came from (that is, what its initial orbit was). At such high
speeds, an impact is more like an explosion than the mere penetration of one
object by another. This is what Daniel Barringer did not appreciate when he
convinced himself and numerous unlucky investors that fortunes could be made
by mining the iron from the meteorite that made Barringer Crater.
A hypervelocity impact at a speed of 15 km/s on Earth, or even the slower 5
km/s impacts in the asteroid belt, would be completely outside our everyday
experience. Even high powered rifles fire bullets at speeds below 1 km/s, so
Barringer would never have been able to see for himself the effects of a
hypervelocity impact. What he did not understand was that a projectile
moving even at 3 km/s carries as much kinetic energy as the explosive energy
in the same mass of TNT. A projectile at 15 km/s carries even more energy,
higher by the square of the velocity, or 25 times more than a 3 km/s
projectile. When an impact occurs in rock at 15 km/s, the peak pressures
reach 500 GPa. The GPa, or gigapascal, may be an unfamiliar unit of
pressure, but it corresponds to 9900 times atmospheric pressure, and even a
few GPa suffices to crush the strongest steels we know how to make.
Hence when the iron meteorite hit the ground to make Barringer Crater, it
was completely crushed, and partly melted and vaporized, even though iron
meteorites are made of very strong material. Much of the original projectile
mass was expelled from the crater. Not only that, but the original size of
the meteorite was much smaller than Barringer thought – maybe only 30 meters
in diameter if the impact occurred at 20 km/s, even though the crater itself
is a kilometer wide. This meteorite (30 meters is too small to be considered
an asteroid) carried an energy equal to that of a 10 megaton thermonuclear
bomb. Such was the explosive nature of the impact, and if Barringer had
understood it, he would not have died a ruined man. However, Barringer might
never have become interested in the crater if he had discerned that there
was no fortune to made, and that – in my scientist’s mind – would have been
a tragedy.
