Column about meteorites

Somewhere in the endless depths of space, a cosmic catastrophe took place millions of years ago. An asteroid struck the surface of the Moon or Mars and released fragments of rock that set out on a long and unpredictable journey. They travelled through the darkness, orbited the Sun and may even have collided with other bodies several times before finally ending up where we would least expect them – on Earth. But how can we know with certainty that these stones really come from the Moon or Mars?

The Secrets of Lunar Meteorites

On 20 July 1969, humans set foot on the Moon for the first time. The Apollo 11 mission brought back 21.55 kilograms of lunar rock samples, including basalts from Mare Tranquillitatis (Sea of Tranquility), which helped confirm the volcanic origin of the lunar maria. During the subsequent Apollo missions and the Soviet Luna programme, scientists obtained a total of 382 kilograms of lunar rocks. The Apollo 12–17 missions gradually returned a more diverse range of samples, including anorthosites from the lunar highlands. In addition to the American astronauts, samples were also collected by the Soviet Luna 16, 20 and 24 probes, which used automated equipment to return a total of 326 grams of lunar material to Earth. Thanks to these missions, we now know in great detail what the material forming the Moon looks like.

Lunar meteorites can be identified by several characteristic features. They contain a high proportion of plagioclase and almost no water, which corresponds to the environment of the Moon, which lacks an atmosphere and flowing water. Another key to their identification is their oxygen isotope composition, which closely matches the samples brought back by the Apollo missions. Their surfaces also bear traces of micrometeorite bombardment and exposure to the solar wind, showing that they spent millions of years in an airless environment.

Bechar 003

Oued el Hamim 001

Gadamis 003

Adrar 013

El Atchane 024

Bechar 007

Ouargla 008

Ash Shaqqah 002

Martian Meteorites and Bubbles of Time

Meteorites from Mars revealed their secret thanks to microscopic bubbles trapped within their structure, for example in ALH 84001 and other shergottites, nakhlites and chassignites. When scientists analysed the gaseous inclusions inside these rocks, they found that the composition of the gases closely matched the Martian atmosphere as measured by the Viking 1 and 2 landers in 1976. The atmosphere of Mars has a specific ratio of argon, nitrogen and carbon dioxide that differs from that of all other planets and bodies in the Solar System.

Martian meteorites also contain minerals that formed in the presence of water, which is supported by modern analyses carried out by the Curiosity and Perseverance rovers. Curiosity, which has been operating on Mars since 2012, performed detailed mineralogical analyses and confirmed the presence of minerals corresponding to those found in Martian meteorites on Earth. Perseverance, NASA's latest Mars rover, began detailed exploration of the planet's surface in 2021 and is searching for rocks with a composition similar to meteorites found on Earth.

Meteorites from Mars are characterised by a high content of iron oxides, which give the Red Planet its characteristic colour. Each recovered specimen is therefore a small fragment of Mars that has completed an immensely long journey through space.

Amgala 001

Tarkint 001

NWA 17472

How Did Meteorites from Mars and the Moon Reach Earth?

Fragments from distant worlds do not reach Earth by chance. For a rock to leave the surface of Mars or the Moon, an enormous collision with an asteroid must occur. Such an impact ejects rocks into space, where they can orbit for tens of millions of years before gravitational influences shift them onto a collision course with Earth – for example, some Martian meteorites are estimated to have travelled through space for more than 15 million years.

This is precisely why these meteorites are so rare. While ordinary meteorites originate predominantly from the asteroid belt between Mars and Jupiter, fragments from Mars and the Moon account for less than 0.1% of all meteorites found.

Lost Fragments of Asteroid Vesta

Not only Mars and the Moon, but also Vesta, one of the largest asteroids in the main belt, has contributed fragments to meteorite collections on Earth. Their origin was confirmed in particular by the Dawn spacecraft, which studied Vesta from orbit in 2011–2012. Spectral analysis based on the data obtained showed that light reflected from Vesta's surface matches the so-called HED meteorites (howardites, eucrites and diogenites).

The decisive role was played by comparing the mineralogical and chemical composition of HED meteorites with data obtained by the Dawn spacecraft during its survey of Vesta. Spectral measurements of Vesta's surface show a very good match with howardites, eucrites and diogenites, while the oxygen isotope composition was determined through laboratory analyses of the meteorites themselves. Taken together, these findings confirm that HED meteorites originate from Vesta, making it one of the known meteorite parent bodies alongside Mars and the Moon.

Scientific Methods for Determining the Origin of Meteorites

Every body in the Solar System has a unique “chemical fingerprint” that can be reliably recognised using modern analytical techniques. The most important methods used to determine a meteorite's parent body include:

Chemical Composition and Mineral Components

Martian meteorites contain iron oxides and minerals associated with water, while lunar meteorites are rich in anorthosite.

Isotopic Analysis

The ratios of isotopes of oxygen, nitrogen and noble gases serve as a unique signature for individual planetary bodies. Martian meteorites often contain gases corresponding to the composition of the Red Planet's atmosphere, while lunar meteorites display isotopic characteristics matching rocks brought to Earth during the Apollo missions.

Comparison with Data from Space Missions

Information obtained directly from the surfaces and atmospheres of planetary bodies – for example during the Apollo missions, measurements of the Martian atmosphere by the Viking landers, or analyses carried out by the Dawn spacecraft – provides a reference base. By comparing these data with laboratory results obtained from meteorites, scientists can reliably determine where the samples originated.

Conclusion

Every meteorite, whether it comes from Mars, the Moon or Vesta, is a small but exceptionally valuable witness to events that took place millions or even billions of years ago. These rocks preserve traces of ancient cosmic catastrophes, reveal complex geological processes and offer clues to understanding the past of these distant worlds.

 

 

Author: Terezie Laubrová

 

 

 

This article is protected by copyright under Act No. 121/2000 Coll., the Czech Copyright Act. Any copying, distribution or other use of the content without the author's prior written consent is prohibited. Copyright infringement may be subject to civil and criminal penalties, including compensation for damages and sanctions under Section 270 of the Czech Criminal Code.

Note: The photographs are for illustrative purposes only.

Every meteorite that hits the Earth has a fascinating journey of millions, sometimes billions, of years. It was originally just a tiny speck in the clouds of dust and gas that once gathered into the first cosmic bodies. Later it became part of a larger asteroid, perhaps even a planet, only to be ejected again into deep space in a dramatic collision. Before reaching our planet, it travelled through infinite space, subject to the forces of gravity and collisions with other objects. But how do these space fragments come into existence?

1. Collapse of the solar nebula

It all started about 4.6 billion years ago, when a huge interstellar nebula of dust and gas began to collapse gravitationally. This collapse led to the formation of a proto-sun and, at the same time, a rotating disk of material around the newly formed star.

2. The origin of planetesimals

In the rotating disk, tiny dust particles began to collide and combine due to gravitational and electrostatic forces. Gradually, these tiny particles formed larger bodies - planetesimals. These bodies ranged in size from a few metres to hundreds of kilometres and were the building blocks of future planets.

3. Accretion and collisions

Accretion is a gravitational process in which planetesimals gradually grew. This process took place over millions of years and, through subsequent collisions and mergers, led to the formation of the first planetary embryos, called protoplanets. During these collisions, huge amounts of energy were released, often leading to the fragmentation of some bodies. While some planetesimals continued to clump and grow until they formed protoplanets, others were torn into smaller fragments that remained in interplanetary space. These fragments later became meteoroids - small bodies that travel through space.

4. Differentiation

Depending on whether or not the planetesimal has undergone differentiation - i.e., separation into individual layers - meteorites can be divided into two basic groups. Undifferentiated meteorites, which include chondrites, have retained the composition of the original material from the solar system. The differentiated meteorites include achondrites, iron meteorites and pallasites, which come from bodies that have undergone melting and separation of the layers.

Stony meteorites

Chondrites are the most commonly encountered meteorites, accounting for up to 85% of all meteorites found. They are undifferentiated, original remnants of planetesimals, i.e. the primary building blocks of planets that did not enter the process of melting and differentiation. As a result, they retain a composition very close to the original material that formed the solar system more than 4.5 billion years ago.

Chondrites are characterised by chondrules – tiny spherical inclusions composed mainly of silicate minerals that formed early in the solar system. These chondrules were formed by the rapid melting and cooling of dust particles in the protoplanetary disk, probably due to electrical discharges or shock waves caused by solar activity. After their formation, the chondrules and other dust particles began to clump together and combine with the surrounding material to form larger bodies, some of which have survived in their original form to this day and have fallen to Earth as meteorites.

Among the most famous of these is the Chelyabinsk meteorite, whose fall was observed on 15 February 2013 over Russia. This extremely bright meteor, known as a superbolide, entered the Earth's atmosphere at a speed of approximately 19 km/s and began to disintegrate at an altitude of around 30 to 50 km above the surface.

On the other hand, there are differentiated stony meteorites, referred to as achondrites. These meteorites come from bodies that have undergone such intense heating that they have melted and chemically stratified into a core, mantle and crust. In the process, they have lost their chondritic structure and more closely resemble terrestrial igneous rocks. Achondrites are often associated with larger bodies such as the Moon, Mars or the asteroid Vesta.

Among the most famous lunar meteorites is Gadamis 001, whose composition matches rocks brought back by the Apollo missions.

If you are fascinated by Mars fragments, it is worth mentioning Amgala 001, a rare meteorite that comes from the surface of the Red Planet. And if you're interested in other achondrites, NWA 7831 (diogenite) is a beautiful example of a sample from the asteroid Vesta.

Iron meteorites

In iron meteorites, differentiation took place so that the heavy metals, especially iron and nickel, were concentrated in the core of the parent body, while the lighter elements remained closer to the surface. This process led to the formation of a dense metal alloy which became the main component of these meteorites. Their structure often contains crystals of kamacite and taenite, two phases of iron-nickel alloy that were formed during extremely slow cooling. Because of this long cooling process, lasting millions to billions of years, Widmanstätten patterns - the unique crystal structures that are the hallmark of iron meteorites - can be observed when some samples are cut and then etched.

The most famous specimens with Widmanstätten patterns include Muonionalusta, Aletai, Saint Aubin, Mundrabilla and many others.

Image description from left to right: Muonionalusta, Aletai, Saint-Aubin, Mundrabilla

Pallasites - a unique blend of stone and metal

Pallasites are a special group of meteorites that contain both stone and iron components. They make up only about 1% of all meteorites found. They are composed of large, well-shaped olivine crystals surrounded by an iron-nickel matrix.

They probably formed at the interface between the metallic core and the silicate mantle of the planetesimals, i.e. in a transition zone where magmatic processes and melt movement occurred. As a result of these geological processes, the metal and minerals were mixed together to form their characteristic structure - crystals of olivine surrounded by a metal alloy.

Important representatives of pallasites are, for example, Sericho, discovered in Kenya, whose olivine crystals have a green tint, or Seymchan, known for its transparent, yellow olivine crystals. Imilac is considered one of the most beautiful pallasites due to its large, translucent olivine crystals.

Image description from left to right: Sericho, Seymchan, Imilac, Brahin

5. Fragmentation and space travel

Fragments released by collisions travel through space as meteoroids. Some of them encounter the Earth's gravitational field during their journey and enter its atmosphere. As they enter the atmosphere, these bodies can disintegrate by heating up, and if some fragments survive this process, they become meteorites that fall to the Earth's surface.

Conclusion

This whole process, from the initial collapse of the solar nebula to the final impact of meteor fragments on Earth, provides valuable information about the formation and evolution of the solar system. The study of meteoric samples is therefore crucial for understanding the chemical and physical conditions under which the first solids in our Universe were formed.

Explore our full selection of meteorites here: Our meteorite offer.

Author: Terezie Laubrova

This article is protected by copyright under Czech law (Act No. 121/2000 Coll., the Copyright Act). Any copying, distribution, or other use of the content without prior written consent from the author is prohibited. Copyright infringement may result in civil and criminal penalties, including damages and sanctions under Section 270 of the Czech Criminal Code.

A meteorite is a fragment of a celestial body that hits the Earth's surface after passing through the atmosphere. However, to understand the whole process of its formation, it is important to first distinguish several terms.

• An asteroid is a celestial body, usually made of metal or rock. Most asteroids are found in the asteroid belt between Mars and Jupiter. If two asteroids collide or if there is another strong disturbance, smaller fragments can be released.
• A meteoroid is a smaller fragment that is released from an asteroid or comet and travels through space. Meteoroids are often very small - from grains of dust to pieces several metres long. When a meteoroid enters a collision course with Earth and enters its atmosphere, it turns into a meteor.
• A meteor is a phenomenon that occurs when a meteoroid enters the Earth's atmosphere. At high speeds, the friction of the atmosphere causes the meteoroid to heat up and begin to glow, creating a bright trail of light, often called a "shooting star". If the meteor is very bright and accompanied by a loud sound, it is referred to as a bolide.
• A bolide is a bright meteor that can reach a brightness comparable to the Moon. It usually explodes or shatters into smaller pieces in the atmosphere, which can be heard as a shock wave. Bolides can be so powerful that they can be seen during the day.
• A meteorite is a body formed when a meteoroid survives a passage through the atmosphere and hits the surface of the Earth. Meteorites can be rock, iron or rock-iron, depending on their composition and origin. Some meteorites are very old and contain material from the formation of the solar system.

Where do meteorites come from?

Meteorites are often very interesting relics from a time when our solar system was just forming, and their origins are varied and rich in stories. These unique bodies come from several different sources.

1. Main belt of asteroids

The first and most important origin of meteorites is the asteroid belt, which extends between the orbits of Mars and Jupiter. This region is home to a myriad of asteroids, which are remnants of material from the formation of the solar system. When dramatic collisions occur between these rocky bodies, fragments are released and then travel into deep space. Some of these fragments, driven by the gravity of our planet, end up on Earth as meteorites.

One of the most famous asteroids in the belt is Vesta, the second largest asteroid in the asteroid belt, from which meteorite NWA 14131, for example, is believed to have originated. Many meteorites are thought to have come from the asteroid belt, including Chelyabinsk, Muonionalusta, Wabar, Seymchan, Campo del Cielo and others.

And how did this belt come about?

The asteroid belt is located between the orbits of Mars and Jupiter, in an area between 2 and 4 astronomical units from the Sun. This belt was formed from material that could not coalesce into a full-fledged planet due to the gravitational influence of Jupiter, instead holding a number of smaller objects. Many asteroids formed afterwards as a result of collisions between the original bodies, when larger fragments broke into smaller pieces. These collisions not only shaped the different shapes and sizes of the asteroids, but also allowed the fragments to be released to collide with Earth.

2. Moon and Mars

Another fascinating source of meteorites is the Moon and Mars. When an asteroid hits the surface of the Moon or Mars, it causes materials to be ejected into space. But the process of ejection can be caused by factors other than collisions with other bodies, such as volcanic activity or even gravity pulling fragments outwards. Some of these ejected materials, if they have sufficient velocity, escape the gravitational field of the Moon or Mars and head towards Earth. The journey can take thousands to millions of years before the meteorite finally enters the Earth's atmosphere and hits the surface. We refer to these meteorites as lunar and Martian meteorites. One of the most famous are the lunar meteorite Bechar 003 and the Martian meteorite Amgala 001.

3. Planetary Remains

Some meteorites may be remnants from the time of the formation of the planets. When the planets were forming, there were many collisions that ejected fragments from their surfaces. These fragments, which did not have enough energy to come back, may be on a trajectory that takes them to Earth.

4. The outer solar system

The source of meteorites can be the outer region of the solar system, such as icy moons and Kuiper Belt objects. These objects, often composed of ice and rock, can be subjected to collisions that tear them apart and release fragments into space. Some scientists believe that meteorites may also come from the outer regions of the solar system, including the Kuiper Belt, but none have yet been found that have been conclusively confirmed as coming from this region. The Kuiper belt contains many small icy and rocky bodies that may be potential sources of meteor fragments, but it is not yet possible to identify them conclusively. So for now, these are speculations rather than confirmed finds.

5. Comets

Comets, with their icy cores and dust clouds, also play a role. As these comets approach the Sun, they sublimate the ice and release dust particles that can form meteor showers. When these particles enter the Earth's atmosphere, they turn into bright meteors that light up the night sky.

But are there meteorites from comets?

Although no meteorite has yet been found that is clearly from a comet, based on research into cometary fireballs and transitional objects between comets and asteroids, it is thought that comets can produce meteorites. The most likely candidates are remnants from a parent body originating in the region around Jupiter that could survive entry into Earth's atmosphere. Such meteorites should be rare, dark, faint, porous and contain organic compounds, similar to carbonaceous chondrites. Some meteorite samples, such as Krymka and Supuhee, suggest that cometary meteorites may be identified in the future.

6. Protoplanets

Meteorites also come from protoplanets, which are smaller planetary bodies that formed in the early stages of the solar system. When the surface of these protoplanets was impacted, fragments of their material may have been released and ejected into space. These fragments can then travel through space and, if they have a favourable trajectory, can eventually enter the Earth's atmosphere and fall to the surface as meteorites. An example of such a meteorite is Erg Chech 002, which is a volcanic rock from a protoplanet older than the Earth itself.

What is the fate of the protoplanets?

1. The creation of planets: Some protoplanets that had sufficient mass and were able to attract surrounding material became full-fledged planets. During this process, more planetesimals and other material accumulated, leading to their enlargement and the formation of stable orbits around the Sun.
2. Fragmentation: Many protoplanets were unable to become full-fledged planets and were instead destroyed by collisions with other planetesimals or protoplanets. These collisions led to fragmentation, and the fragments from these protoplanets then became meteoritic material that could be ejected into space.
3. Asteroid belt: Some protoplanets that were in the region between Mars and Jupiter became part of the asteroid belt. This region contains many small bodies that remained unfinished and did not develop into full-fledged planets. As already mentioned, Jupiter's gravity played an important role in this process, destabilizing the orbits of some planetesimals and preventing them from merging into larger bodies.
4. Removal from orbits: Other protoplanets may have been ejected from the solar system due to strong gravitational interactions with other planets such as Jupiter or Saturn. These interactions may have caused the protoplanets to enter hyperbolic orbits and escape the solar system.
5. Causing meteor showers: Fragments from protoplanets that have entered orbits around the Sun can become the source of meteor showers as the Earth passes through the rest of the orbit of these fragments.
6. Change in composition: Remaining protoplanets that have not lost their orbits may have their chemical composition changed by solar radiation, heat, and other factors. These changes can affect their physical and chemical properties.

Overall, protoplanets have had different fates, although most have either disappeared or become part of other planets or the asteroid belt.

Conclusion

Meteorites are fascinating remnants from a time when our solar system was just beginning. They come from different regions, such as the asteroid belt, the Moon, Mars or protoplanets, and can provide valuable information about the origins of the Solar System and the composition of individual bodies in the Universe. Whether they are fragments of disintegrated planets, fragments from an asteroid or fragments from the Moon or Mars, each meteorite contains information about the formation and composition of other bodies in the Universe.

You can find our full range of meteorites here

Author: Terezie Laubrova

This article is protected by copyright under Czech law (Act No. 121/2000 Coll., the Copyright Act). Any copying, distribution, or other use of the content without prior written consent from the author is prohibited. Violation of copyright law may be subject to civil and criminal penalties, including damages and sanctions under Section 270 of the Czech Criminal Code.

The Moon is one of the most famous and visible objects in the night sky, and we notice it almost every day, whether it's a clear night or the sky is only lightly clouded. It is the only natural satellite on our planet whose light illuminates us at night, even though it is really just a reflection of the sun's rays. The Moon is an integral part of our daily lives and inextricably linked to our planet.

Origin

The Earth was born about 4.6 billion years ago by the clumping of planetesimals, which are small bodies that formed from dust and gases in the early solar system. And what did they look like? The Earth's surface was mostly rocky then, and life as we know it today didn't exist yet. The latest theory is that about 100 million years after the Earth formed, a protoplanet comparable in size to Mars, known as Theia, approached our planet and was heading straight for Earth. The collision was inevitable and its consequences could have been catastrophic. This event could have fundamentally changed the evolution of the entire planet, but fortunately, according to this theory, the collision only caused the ejection of material from the Earth, which then formedin its orbit and began to orbit it like the Moon.

Surface

The surface of the Moon is markedly different on the inverted and reversed sides. The inverted side is covered with large dark areas called lunar seas. These seas make up about 31% of the surface and were formed billions of years ago by volcanic activity that created broad pools filled with dark lava material on the Moon. The lighter parts that surround the lunar seas are the lunar highlands and mountains, which are slightly older and more dotted with impact craters.

The far side of the Moon, on the other hand, is much lighter and almost completely devoid of lunar seas, which make up only 2% of the surface on this side, while the rest is covered with high mountains and craters.

Craters on the Moon

Over several billion years, countless meteorites have struck the Moon, as well as the Earth, leaving craters. They are not as visible on our planet as they are on the Moon, because our planet has been shaped and changed over billions of years. Active geological processes, such as volcanic activity, erosion by water and wind, and the movement of tectonic plates, have smoothed or covered these craters.

However, the Moon has no atmosphere, water cycle, tectonic activity or geological activity, which means that all meteorite and comet impacts remain virtually unchanged. Because of these natural manifestations, the craters that have formed on the Moon are still visible and remain preserved.

The largest crater on the Moon, known as South Pole-Aitken, lies on the far side of the Moon, near its south pole. This huge impact crater is 2 240 km across and an impressive 13 km deep.

The lunar surface is also covered with a layer of regolith - a dusty substance formed from fragments of shattered material resulting from the constant impact of meteorites. This regolith covers the entire Moon, and its thickness varies from region to region, from a few centimetres to several metres.

Function

Tides

The Moon's gravity pulls water towards the Earth, causing the oceans to bulge towards it. This bulge is known as a tide, a rise in the water level at a particular point on Earth. On the other side of the planet, where the Moon does not act directly, a tide is created when the ocean level drops. This phenomenon is caused by the Earth being pulled towards the Moon more strongly than the water itself, creating an area of low water on the side facing away from the Moon.

There are two tides on Earth every day. This means that in a 24-hour period, the water level rises twice and falls twice. This cycle lasts approximately 12 hours and 25 minutes due to the rotation of the Earth and the motion of the Moon around it.

Stabilisation of the Earth's axis

The Earth rotates on its axis, which is an imaginary line around which the planet moves. This axis is not perpendicular to the plane of its orbit around the Sun, but is inclined at an angle of approximately 23.5 degrees. This tilt is responsible for the change of seasons, as different parts of the Earth receive more or less solar radiation as it orbits the Sun, resulting in temperature changes throughout the year.

Although the Moon' s gravity does not stop this movement completely, it slows it down considerably. This makes the tilt of the Earth's axis much more stable, which means that the climatic conditions on Earth are favourable for life. Without the Moon, the tilt of the axis could fluctuate, leading to dramatic changes in climate.

Illuminating the night

The Moon provides natural light at night, which in the past was important for orientation of humans and animals who relied on Moonlight for nighttime activities. Although the Moon itself does not shine, its light is a reflection of the sun's rays that bounce off its surface.

Influencing the Earth's rotation

The gravitational pull of the Moon actually slows down the rotation of the Earth, leading to a gradual lengthening of the day. This process is known as tidal friction. At present, the length of the day is increasing by about 1.7 milliseconds per century. This phenomenon is very slow, but over billions of years it has a major impact on day length.

What else does the Moon bring us?

Lunar meteorites originate from the Moon, which are authentic fragments from the surface of the Moon that are formed when another body, such as an asteroid, hits it. On impact, the material is ejected at tremendous speed, and if it is fast enough, it escapes the Moon's gravitational pull and reaches space. The journey through space can take thousands to millions of years, but some debris may eventually head for Earth, where it is caught by Earth's gravity. They then enter the atmosphere and, if they survive the passage, hit the surface. The Moon is the source of only about 0.08% of all meteorites found, making lunar meteorites extremely rare.

One of the most famous lunar meteorites is Bechar 003, which was found in 2022 in Algeria.

Conclusion

The Moon, our faithful satellite, plays an irreplaceable role on Earth . From stabilising the tilt of the Earth's axis to shaping the tides, its influence extends far beyond the mere beauty of the night sky. Although it is one of the largest moons in the solar system relative to the size of its parent planet, its real value lies in how it helps maintain stable conditions for life on Earth. The Moon is not only a fascinating object to observe, but also a key factor in the geological and climatic processes on our planet.

You can also purchase an authentic fragment of the Moon in our e-shop: Lunar meteorites.

Author: Terezie Laubrova

This article is protected by copyright under Czech law (Act No. 121/2000 Coll., the Copyright Act). Any copying, distribution, or other use of the content without prior written consent from the author is prohibited. Violation of copyright law may be subject to civil and criminal penalties, including damages and sanctions under Section 270 of the Czech Criminal Code.

Updated: 23 September 2026

Buying meteorites can be a fascinating and unique hobby, but it also requires a little caution. It is not enough simply to find a piece that appeals to you – it is important to make sure that the seller is trustworthy and reliable. We have specialised in selling authentic meteorites for several years and offer our customers a number of advantages that you will not find elsewhere. Whether you are buying a meteorite simply for enjoyment, as a gift or as an interesting scientific specimen, we will help you choose the right one.

1. Guarantee of authenticity and quality (IMCA 6180)

We are proud members of the International Meteorite Collectors Association (IMCA) – an international association of meteorite collectors. Thanks to this membership, we guarantee the authenticity of every meteorite specimen in our selection.

Our meteorites are selected with exceptional care and come exclusively from verified suppliers. Each piece undergoes a detailed inspection that confirms its authenticity, origin and quality.

We also issue certificates of authenticity for our meteorites:

– a physical certificate in the box is already included in the price,

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– a printed certificate is available for an additional charge.

With us, you can be sure that you are holding a genuine piece of space, not an imitation.

2. Wide selection of different types of meteorites

We have the largest selection of meteorites in the Czech Republic and one of the largest in Europe, both in terms of the number of specimens offered and the variety of individual types. Our selection includes a wide range of meteorites – from iron meteorites and stony meteorites to rare pallasites and carbonaceous chondrites. Our meteorites come from different locations around the world and include not only famous specimens such as Campo del Cielo, Muonionalusta, Sikhote Alin or Aletai, but also less common and rarer specimens such as Imilac, Erg Chech 002, Kaalijärv and others that will appeal even to passionate collectors.

3. Clear and easy selection

Looking only for iron meteorites? No problem – everything is clearly organised either by type or by surface treatment. By type, you can choose iron, stony or stony-iron meteorites. Thanks to our intuitive system, you can easily browse the individual categories, and all categories are accompanied by high-quality images to make your choice easier.

If, on the other hand, you are looking for a specific treatment, such as slices or slabs, simply visit the cut and polished meteorites category. Here you will find everything you need, with detailed photographs of each specimen. Thanks to this well-organised selection, you can quickly find exactly the meteorite that will fit perfectly into your collection.

4. Unique specimens with a story

Every meteorite has its own story, which is why we select pieces with an interesting origin and history. We offer meteorites from various historical impacts and events that have something fascinating about them. We have also prepared an article featuring some of the most interesting meteorite stories, which you can read here.

5. New types are added regularly

We actively search for new types of meteorites to expand our selection even further. We try to add new arrivals regularly, so if you follow our website, you are sure to discover something new. You can also follow us on our Facebook page, where we share new arrivals and interesting facts.

6. Years of experience and reliability

We have many years of experience in selling meteorites and pride ourselves on reliability and honesty. Our satisfied customers often return to us, which we see as proof that we provide quality service and which motivates us to keep improving. You can find customer reviews of our e-shop here.

7. Practical boxes with attractive graphics, suitable for a collection or as a gift

If you do not want your meteorite simply lying on a shelf, we offer a practical and creative solution in the form of our special boxes. Each meteorite is carefully placed in a box with a graphic background. On the back, you will find a certificate of authenticity with a photograph of the meteorite, its weight, dimensions and our security hologram. This ready-to-display box is ideal not only as a shelf decoration, but also as a unique gift that will delight any space enthusiast. You can find our complete box collection here.

Conclusion

If you are looking for a meteorite to enrich your collection, or if you are simply fascinated by space, you are in the right place. Here you will find carefully selected meteorites, expert support and quality service with fast shipping. Treat yourself to a unique experience and bring a piece of space into your home – we are here for you and will be happy to help you choose. You can find all our meteorites here.

 

Author: Terezie Laubrová

This article is protected by copyright under Act No. 121/2000 Coll., the Copyright Act. Any copying, distribution or other use of the content without the author's prior written consent is prohibited. Copyright infringement may be subject to civil and criminal penalties, including compensation for damages and sanctions pursuant to Section 270 of the Criminal Code.