Meteorite or Meteorwrong

Vesicles in Meteorites

The Dictionary of Geologic Terms (R. Bates & J. Jackson, eds) defines vesicle as "a small cavity in an aphanitic or glassy igneous rock, formed by expansion of a bubble of gas or steam during solidification of the rock." Such a rock is said to be vesicular. Only igneous rocks - rocks that cooled from a molten magma - can have vesicles. Very few (less than 1 in 1000) meteorites have interior vesicles because the interior of most meteorites was never molten. Many terrestrial rocks have vesicles, however. Also, almost every sample of industrial slag that we've seen has vesicles. Vesicles and metal together in the same "rock" are a good field mark for slag.

Terrestrial Rocks with Vesicles

Basalts are the rocks that form when volcanic lava or magma cools. Not all basalts are vesicular, but vesicular basalts are very common on Earth.

Pictured here is a vesicular basalt from Hawaii. The field of view is about 6 cm.

The surface at the top of the photo is where the molten lava was exposed to air. The exposed portion cooled quickly, leaving a glassy, shiny surface. The surface somewhat resembles a meteorite fusion crust. Meteorite fusion crusts are usually smoother than this, however. Also, you can see the circular shapes of broken gas bubbles in the crust of this rock; such features are very rare in meteorite fusion crusts. Click on image for enlargement.

This is also a vesicular basalt. As on the photo above, the crust on top is where the molten lava was exposed to air. Basalts come in a variety of colors, mostly gray or black to rust colored. Click on image for enlargement.

A highly vesicular basalt from Hawaii. Highly vesicular volcanic rock is also known as scoria, or pumice if the density is very low. Click on image for enlargement.

Vesicular rocks occur all over the world. This one is from Australia. Click on image for enlargement. (Photo credit: Max McCosker)


An amygdule is "a gas cavity or vesicle in an igneous rock which is filled with such secondary minerals as zeolites, calcite, quartz, or chalcedony." Such a rock is said to be amygdaloidal. Amygdules form when fluids containing dissolved minerals flow through the rocks and deposit the minerals as solids in the vesicles. Lunar basalts are not amygdaloidal because the Moon is so dry that there are no fluids (and, apparently, there never were). Click on image for enlargement.


Vesicles in Basaltic Meteorites

Vesicles only develop in rocks that cool from a liquid Ė an igneous rock. Most meteorites come from asteroids, and almost all asteroids are too small to have volcanoes, thus very few meteorites are igneous rocks. Most such rocks among the meteorites are basalts. Most common are the eucrites (believed to come from a large asteroid like Vesta that had volcanoes), most of the martian meteorites (Mars has some really big volcanoes), and some lunar meteorites. So far, there have been no vesicular martian or lunar basaltic meteorites discovered. A few eucrites and diogenites are moderately vesicular, however.

On the left is a slice of the eucrite Ibitira (width: probably ~10 cm) and on the right is a slice of the diogenite Dhofar 700. These two meteorites are the most vesicular meteorites of which the author is aware. Among all known meteorites, only 1.36% are eucrites and 0.54% are diogenites. Most eucrites and diogenites are not vesicular. Photo courtesy of Ray Stanford. Click on image for enlargement.



Two vesicular lunar basalts, sample 15556 from the Apollo 15 mission (left, cube is 1 inch) and sample 71155 from the Apollo 17 mission (cube is 1 cm). Note that the vesicles are round, not elongated. This occurs because lunar basaltic magmas had very low viscosity and lunar gravity is low. It is possible that someday someone will find a vesicular basaltic lunar meteorite. Click on image for enlargement.


Vesicles in Meteoritic Impact Melts

When two asteroids collide, melting may occur and gas may be released. Sometimes the impact melt traps gas bubbles when it cools. This is a special kind of igneous meteorite, one even rarer than meteorites of volcanic origin.

A few lunar meteorites have vesicles that formed by impact of asteroidal meteorites on the Moon. A spectacular example is Shişr 166.

This is a sawn slice of lunar meteorite Shişr 166. The gray portions are veins of solidified impact melt. Several vesicles occur in the impact melt. A few of the vesicles are filled with calcite (the whitest material) that precipitated from aqueous fluids after the meteorite landed in Oman. Such features are called amygdules (above).

Another vesicular lunar meteorite are the four paired stones of Dhofar 081/280/910/1224. These stones have vesicles in the glassy matrix because the matrix was once molten and probably consisted of melted regolith that contained solar wind gases. It's probably more accurate to call these cavities vugs, not vesicles, because most are not spherical.

Slices of lunar meteorite Dhofar 910, each about 1 cm across. Notice that the clasts do not have vesicles or vugs but the once-glassy (now devitrified) matrix does. Again, the voids are all less than a millimeter in size. Photos courtesy of Haberer-Meteorites.

Keep in mind, however, that meteorites are very rare and lunar meteorites are exceedingly rare - less than 1 in 1000 meteorites are from the Moon.

Vesicular Meteorite Fusion Crusts

Many stony meteorites have vesicular fusion crusts (for example, see Cynthiana). As the surface melts when the meteorite passes through the atmosphere, gases in the meteorite is are released. Some of that gas becomes trapped in the glassy melt when the melt cools.

Many lunar meteorites are regolith breccias, and some of these have fusion crusts that are thick and highly vesicular. The best examples are QUE 03069 and PCA 02007, although the effect can be also seen in ALHA 81005 and Calcalong Creek. At one time, all of the material of a regolith breccia was fine grained "soil" on the surface of the Moon. Soil grains exposed at the very surface of the Moon absorbed ions emitted by the sun as solar wind. Most of the ions were of gaseous elements like hydrogen, helium, and nitrogen. Impacts of small meteoroids on the Moon mixed and stirred the upper part of the regolith. In a location where there has not been a recent large impact, nearly all the grains in the upper few meters of the regolith will contain solar-wind implanted gases because over millions of years all grains spend some time at the surface. On Earth, the solar wind is absorbed by the atmosphere, so there are no Earth rocks with solar-wind implanted ions. Some meteorites from the asteroid belt have solar-wind gases, but none have the high levels found in lunar meteorites because the Moon is closer to the sun. When the exterior of the meteoroid is heated by the friction of the atmosphere, it melts and the gases are released, forming gas bubbles that get trapped in the glass when the glass cools.

Backscattered-electron image of lunar meteorite PCA 02007, a regolith breccia. At the top and right is the glassy, vesicular fusion crust that occurs on the outside of the meteorite in this photo; the vesicles are black in the image. At the bottom is the brecciated interior of the meteorite. It was never molten, so there are no vesicles. Longest dimension: 1.3 cm. The vesicles are all smaller than 1 mm in diameter. (Image credit: Ryan Zeigler)


This is a photo of tiny lunar meteorite QUE 94281. It has a highly vesicular fusion crust because it is a regolith breccia.

Many people have contacted me saying, "My rock looks just like QUE 94281." Above is a photo that one such person sent me. Superficially, the rocks do resemble QUE 94281, but not in detail. QUE 94281 is a fragment broken from a larger stone, so it has some rough edges, like the rocks above. The fusion crust on QUE 94281 coats only part of the stone. As in PCA 02007 above, the interior of QUE94281 does not contain vesicles (although that's hard to see in this photo) because the interior was never molten. The rocks above are not regolith breccias, but terrestrial basalts, often called scoria. Notice in the upper right stone that there are fewer vesicles in the chilled top than in the interior - the opposite of what is seen in meteorites. Rocks like those in this photo are used for landscaping and in barbeque grills.


Bottom line: If you have a vesicular rock, then it's not a meteorite. Such rocks are very common on Earth but are exceedingly rare among meteorites.



Prepared by: Randy L. Korotev

Department of Earth and Planetary Sciences
Washington University in St. Louis

Please donít contact me about the meteorite you think that
youíve found until you read this and this.



Last revised: 17 April 2019