What do meteorites look like?

Maybe you’ve just found a strange rock, or maybe you’ve had one laying around for years.  Maybe someone has approached you with a rock they think is a meteorite, hoping to sell it.

How do you figure out what it is?

That’s a tough question.  There are many different types of meteorites, and an even wider variety of rocks from Earth.  But there are a few things you can look for.

Freshly Fallen Meteorites

When meteorites enter the atmosphere, they’re moving really quickly.  Usually ~ 20 to 40 kilometers per second.  For comparison, the Space Shuttle used to enter the upper atmosphere at ~8 kilometers per second.

Novato
This causes intense heat and pressure to act on the surface of the rock.  The outside of the meteorite vaporizes, and a thin molten layer forms on the outside of the rock.  The body is usually broken up by extreme ram pressures, and these fragments begin to ablate as well.

If any rocks do survive the passage, they almost always bear some scars.  As the fragments are slowed down by the atmosphere, their surfaces begin to cool.  The last molten material on the rock’s surface cools and solidifies on the outside of the meteorite, forming a “fusion crust.”  This layer is usually fairly smooth, but is not the polished texture of a water-worn pebble.

Freshly-fallen meteorites as found:

As you can see, the ~black outer layer is usually ~smooth, but finely textured.  While meteorites themselves almost never contain any bubbles, the outer layer of crust can exhibit small bubbles (but usually doesn’t).  Note that none of these rocks has actually melted through.  Inside, they’re still grainy rocks, for the most part.  See here, #2 for a little more information on what happens as meteorites fall to Earth.

2) Most meteorites start out on a gradient from ~white to ~black inside. Here are a few examples:

Freshly fallen meteorites, naturally broken and cut:

The above album contains freshly-fallen meteorites.  Some are broken, others are cut. Most of the broken stones fragmented in the atmosphere or when they landed on a hard surface.  As you can see, they range from ~light grey to black inside. There are a few other details you might have noticed…a few have started to oxidize (3rd, 6th images).  More on that later.

There are also a few exceptions to the grey-black gradient — namely with pale green meteorites made mostly of olivine or pyroxene. However, these meteorites are exceedingly rare, and only a dozen or so have been seen to fall in recorded history. So, we’ll skip the details on diogenites and visually ~similar meteorites.

So, right after they fall, most meteorites have a black crust on the outside, and they range from ~white to ~black on the inside.  But most meteorites that are found didn’t fall recently.  Most meteorites found on Earth have spent thousands of years here, just waiting to be picked up.  What do those meteorites look like?  Well, there are a few things you should take note of.

Weathered meteorites

~95% of meteorites contain between ~10 and ~20% metallic iron when they fall.  These meteorites begin to oxidize after falling to Earth: a freshly fallen meteorite won’t be rusty, but ~95% of meteorites will begin to show at least minor oxidation within weeks to months.  After a few decades, they’ll be ~thoroughly rusty.  Most meteorites on Earth fell ~hundreds to ~thousands of years ago.  A rusty coloration is fairly typical of most meteorites:

So…rusty rocks.  If you look carefully, you can see that some still have some smooth fusion crust, although it has been weathered to brown or has been mostly chipped off in many cases.  The textures are important — note that the older fusion crust is uniformly textured even on concave surfaces: that’s uncommon for terrestrial rocks.  Weathering on usually Earth starts from the edges/corners, rounding those off first.

Other Defining Characteristics

There are a few other kinds of details you can look for.  ~90+% of all meteorites are “stony” meteorites.  This kind of meteorite usually contains features called chondrules.

What are chondrules?  We’re not sure exactly how they formed, but we know they date back to the earliest days of our solar system, 4.56 billion years ago.  In a nutshell — they’re small spherical droplets of rock, usually about a millimeter in diameter.  They range from 0.1 mm or smaller to ~1 cm across.  In rare cases they can be larger, but they’re usually 1 mm or so.  Here are some examples of chondrules in cut meteorites:

~90% of meteorites will look something like this when cut.  When looking for meteorites, this is what you are most likely to find.  Note that in many of them the chondrules are only faintly visible, if at all.  This is common.  Also, note that many of these stones exhibit visible metal flakes when cut.  A more oxidized meteorite might not have any of these left, but a polished stony meteorite will almost always still have some of these.  Flecks of specular hematite in terrestrial rocks can look similar, but appear darker, and less like native metal.

Also – shock veins.  When asteroids collide with each other in space, they can do so at thousands of miles per hour.  Some become truly broken up and brecciated, while others get only a few thin, usually black, veins of melt.  Here are some examples:

Not all meteorites have these, but they can be a good indicator.  Some terrestrial rocks can look similar, but they’re not too common.

Stony meteorites without chondrules are very rare, and they usually look very much like terrestrial igneous rocks on the inside.  The only good identifying features of these types of meteorites are shock veins and fusion crust.  These meteorites rarely oxidize over time.  In 15 years of hunting in good desert terrain, we have found three such meteorites.  They’re so rare — and usually so hard to identify — that it’s probably not worth spending time looking for them until you know quite a bit about meteorites.  Here are some examples.

Iron and stony-iron meteorites are very rare, but are easy to recognize.  These classes make up ~2% of meteorites, and they are mostly metallic.

All of the above meteorites would be very strongly attracted to a magnet.  As much as a piece of solid iron.  They’re typically fairly easy to identify.  Note: many have deep indentations in their surfaces, but no “bubbles.”

But be careful — many terrestrial rocks also contain (magnetic) iron, and people have been concentrating iron to make tools (and thus, slag), for thousands of years.  Most iron-bearing, magnetic rocks on Earth are from Earth.

Which raises an important idea: if hunting for meteorites, it is very important that you be familiar with characteristics that meteorites do not have.  Many meteorites have been found by people familiar with rocks, their surroundings, their farms, etc., who noticed something out of place.  They didn’t know what meteorites looked like; they just noticed that a rock didn’t look like the other ones around.

Most of the rocks in this image are dark / rusty brown and slightly magnetic. Can you spot the meteorite? Click on the image for a closer look.  Click here for a spoiler.

 

Knowing what meteorites look like is only half of the battle.  If you want to find a meteorite, a general understanding of geology is extremely helpful. If you learn as much as you can about different rocks and how they form, you will be much better equipped to identify rocks (and meteorites) in the field.

Common Meteor-Wrongs

Here are some photographs of pieces of a very common meteor-wrong — man-made slag.  These are not meteorites:

Image credits: 1 2 3 4 5 6 7 8 9 10 11 12.

Note the bubbles, large, bubbly flow features, and “skin” that often forms on the surface of pooling slag.  Meteorites don’t “melt-through” when they’re coming through the atmosphere, so when you see characteristics that suggest your rock was literally flowing or molten like lava, you know it’s not a meteorite.  The molten surface of slag is very different in texture from a fusion crust (compare to other images above), and the large bubbles are almost all below this smooth skin.

One or two of the above specimens don’t look half bad.  The 7th image in particular isn’t a bad wrong, but the few included flint fragments suggest it’s not a meteorite — a few pieces of unmelted rock appear to have been incorporated into the molten metal.  Small amounts of sand and rock can adhere to a rusting meteorite though; this can give a grossly similar appearance, so be careful.  I’d probably suggest cutting a specimen if in doubt.  If you see vesicles or vugs, you’re almost certainly out of luck.

Another common wrong — manganese slag (source):


Manganese slag feels quite dense, is often ~a little magnetic, looks silvery/metallic when polished, and has a rusty-to-black exterior (that often rubs off on your fingers as a fine black dust).  What’s wrong with it?  The surface of manganese slag specimens is often quite rough, but not very rusty: that fine black dust that’s hard to get off of your hands is manganese oxide, and it’s not similar to typical iron ‘rust.’  And while manganese is dense/feels like metal, an iron meteorite would be made of ~90% iron, and would be very strongly attracted to a magnet.  All metallic meteorites are  strongly magnetic.  Most manganese slag isn’t very magnetic.  Some of it contains quite a bit of iron.  It’s usually easy to tell apart from a meteorite because it is metallic, but granular in structure and its surface looks metallic, but very rough.  Not like oxidizing iron, which develops a thin layer of red-brown oxides.

Why can’t a meteorite be made mostly of manganese, aluminum, copper, or some other metal?  Earth is geologically and hydrologically one of the most active bodies in the solar system — second, perhaps, only to Jupiter’s sulfur-rich moon, Io.  Complex hydrologic reactions need to take place on Earth in order for these metals to naturally precipitate, and we can be fairly certain that it’s not happening anywhere else in the Solar System.  You need large amounts of liquid water to carry acids or bases in addition to extended exposure to geothermal heat to drive these kinds of chemical reactions.  The few bodies that have enough geologic heat to drive these kinds of reactions, like Io and Venus, are bone dry, and the few bodies with enough water to support these kinds of reactions, like Europa and Enceladus, are extremely cold.  Earth is a pretty unique place in our Solar System.  That’s reflected by its geology.

Most iron meteorites formed by a very simple general sort of process: chondritic material was melted by heat from impacts or heat released by the radioactive decay of elements.  There’s ~no natural way to concentrate large amounts of manganese, copper, etc. metals in such a process.

It’s much more common for these metals to be concentrated by people, by prehistoric smelting or modern manufacturing.  Most pieces of metal that are brought into labs are simply industrial waste.  Which makes sense — people have been refining different metals for thousands of years, and leaving the waste just about everywhere.

If you have a strange piece of metal, or a metallic rock, and it’s not strongly attracted to a magnet, it’s not a meteorite.  There are no exceptions.  If you have something metallic, but not magnetic, it’s almost certainly man-made.  If not, it’s still terrestrial.