Every clear night, thousands of tiny fragments of rock and metal burn up in Earth's atmosphere — the brief streaks of light we call shooting stars. Occasionally, a piece survives the fiery journey through the atmosphere and reaches the ground. That survivor is a meteorite.

 

Meteorites are pieces of asteroids, comets, and occasionally other planets or the Moon that have made the 150-million-kilometre journey from space to your hands. They range in age from 4.568 billion years old — older than the Earth itself — to as young as 150 million years for some volcanic rocks from Mars. They are the most ancient solid objects accessible to collectors anywhere on Earth.

 

The word "meteorite" has a precise scientific meaning: it refers specifically to the object after it has landed. A meteoroid is the object in space. A meteor is the luminous phenomenon in the atmosphere — the shooting star. A meteorite is what you hold in your hand.

 

 

 

Humans have known about meteorites for thousands of years, though they did not always understand what they were. Iron meteorites were worked into tools and weapons by cultures from the Arctic to Egypt long before terrestrial iron smelting was developed — the iron daggers of Tutankhamun's tomb, and iron beads found at Egyptian archaeological sites dating to 3200 BCE, are both of meteoritic origin. The Inuit of Greenland used pieces of the Cape York iron meteorite (discovered 1818, weighing 58 tonnes across several masses) as a source of metal for harpoon tips for at least a thousand years before European contact.

 

The scientific recognition of meteorites as extraterrestrial objects came slowly. For centuries, the idea that rocks could fall from the sky was dismissed as superstition by European scientific institutions. The turning point came on April 26, 1803, when over 3,000 stones rained down on the town of L'Aigle in Normandy, France, witnessed by hundreds of people. The French physicist Jean-Baptiste Biot conducted a systematic investigation and presented his findings to the French Academy of Sciences, conclusively demonstrating the extraterrestrial origin of the stones. The science of meteoritics — the study of meteorites — was born.

 

The 19th century saw the first systematic meteorite collections assembled, the first chemical analyses performed, and the first recognition that meteorites could be classified into distinct types. The 20th century brought isotopic dating, electron microscopy, and the discovery that meteorites preserve materials predating the solar system. Today, meteoritics is a mature scientific discipline that intersects with planetary science, cosmochemistry, astrobiology, and nuclear physics.

 

For collectors, the hobby traces its modern roots to the mid-20th century, when dealers began making meteorite specimens widely available beyond institutional collections. The founding of the International Meteorite Collectors Association (IMCA) in 1997 established ethical standards for the trade. The internet transformed the market from the early 2000s onwards, connecting collectors worldwide and dramatically increasing the availability and diversity of specimens. Today, meteorite collecting is a vibrant international community spanning casual hobbyists to serious scientists with home laboratories.

 

 

The Solar System's Raw Materials

To understand meteorites, you need to understand where they come from. Our solar system formed approximately 4.568 billion years ago from a rotating cloud of gas and dust — the solar nebula. As this cloud collapsed under gravity, the centre became the Sun, and the remaining material formed a disk. Within this disk, dust grains collided and stuck together, forming pebbles, then boulders, then planetesimals — the building blocks of planets.

 

Most of the material in the inner solar system was swept up into the planets — Mercury, Venus, Earth, and Mars. But in the region between Mars and Jupiter, the gravitational influence of Jupiter prevented this material from completing the planet-building process. Instead, the objects there — ranging from dust grains to bodies hundreds of kilometres across — collided and fragmented rather than merging. This is the asteroid belt, and it is the source of the vast majority of the meteorites we find on Earth.

 

From Asteroid to Meteorite

The journey from asteroid to your collection typically takes hundreds of millions of years and involves several steps:

 

●       Collision in the asteroid belt: Two asteroids collide, fragmenting one or both and sending pieces into new orbits. Collisions in the asteroid belt have been happening continuously for 4.5 billion years — the asteroid belt is a cosmic demolition derby in slow motion.

●       Orbital evolution: Gravitational perturbations from Jupiter and Mars, combined with subtle thermal forces (the Yarkovsky effect), gradually push fragments into orbital resonances — regions where Jupiter's gravity repeatedly tugs at them in the same direction, changing their orbit until it crosses Earth's path.

●       Atmospheric entry: When a fragment intersects Earth's orbit, it enters the atmosphere at between 11 and 72 km/s. The kinetic energy is converted to heat by compression of the air ahead of the object. The outer surface melts and ablates away, forming the characteristic fusion crust. Most of the original mass is lost during this process.

●       Dark flight and landing: Below about 20 km altitude, the surviving fragment has slowed to terminal velocity — typically 100-400 metres per second — and falls ballistically to Earth. It has cooled enough that the fusion crust has solidified. After landing, it is a meteorite.

 

The Story Inside the Rock

What makes meteorites scientifically extraordinary is what happened to them before the collision that sent them toward Earth. Many spent billions of years inside asteroid parent bodies — objects large enough to have interesting internal geology. Some asteroids melted completely, separating into metallic cores, rocky mantles, and volcanic crusts — just like the Earth. The iron meteorites in your collection are pieces of asteroid cores. The stony-iron pallasites formed at the boundary between core and mantle. The basaltic achondrites are pieces of asteroid crusts.

 

Other asteroids never melted significantly — they remained as primitive assemblages of the original solar nebula material. These are the chondrites, and they preserve the oldest, most pristine materials accessible to science: tiny spheres of once-molten droplets called chondrules, calcium-aluminium-rich inclusions (CAIs) that are the first solid objects to condense from the solar nebula, and occasionally presolar grains — microscopic particles from stellar atmospheres that predate the solar system entirely.

 

 

 

One of the most common questions asked of meteorite dealers is: "I found a rock — could it be a meteorite?" The honest answer is: probably not, but here is how to check. The vast majority of suspected meteorites turn out to be terrestrial rocks — usually iron-rich concretions, slag, or heavily weathered stones. But meteorites are found regularly by people who know what to look for.

 

The Key Indicators

Fusion Crust

The most diagnostic feature of a fresh meteorite is fusion crust — a thin (0.5-2mm) glassy or matte black rind formed by melting of the outer surface during atmospheric entry. On a fresh fall, it is typically jet black, smooth, and covers the entire surface. On older finds, it weathers to brown or is partially missing. Under magnification, fusion crust often shows flow lines, tiny surface bubbles, and contraction cracks.

 

 

Regmaglypts

Many meteorites show characteristic thumbprint-like depressions on their surface called regmaglypts, formed by ablation during atmospheric flight as turbulent airflow removes molten material in a pattern. They range from shallow dimples to deep scoops and are one of the most visually distinctive meteorite features. Not all meteorites have them — irons and oriented stones show them most prominently.

 

Magnetic Response

Most meteorites contain iron-nickel metal and are attracted to a strong magnet. Ordinary chondrites (the most common type) are moderately to strongly magnetic. Iron meteorites are very strongly magnetic. Some meteorite types (lunar, Martian, and some carbonaceous chondrites) are weakly magnetic or non-magnetic — but if a rock shows no magnetic attraction at all, it is less likely to be a meteorite, though not impossible.

 

 

Chondrules

If you can see a cut or broken face on a suspected stony meteorite, look for chondrules — small (typically 0.3-1mm) spherical or sub-spherical structures embedded in a darker matrix. These tiny spheres are unique to chondritic meteorites and do not occur in any terrestrial rock. They are the most reliable indicator that a stony specimen is a meteorite, though not all meteorites contain them.

 

Widmanstätten Pattern

If you have a polished and acid-etched iron meteorite, look for the Widmanstätten pattern — interlocking bands of two iron-nickel alloys (kamacite and taenite) that form during extremely slow cooling in the interiors of asteroid cores. This pattern requires millions of years to develop and is completely impossible to fake or replicate. Its presence proves beyond any doubt that you have an iron meteorite.

 

Density

Meteorites are typically denser than terrestrial rocks of similar size. Iron meteorites are extremely dense — roughly 7.8 g/cm³, nearly three times the density of granite. Stony meteorites are typically 3.3-3.5 g/cm³, noticeably heavier than most common rocks. If a rock feels unexpectedly heavy for its size, that is a positive indicator worth investigating further.

 

What Meteorites Are NOT

Before spending time and money on testing, it helps to know the most common meteorite impostors:

 

●       Slag: Iron or steel slag from smelting and industrial processes is extremely common, dark, often magnetic, and is the single most common suspected meteorite submitted for identification. It is typically vesicular (full of bubbles), has a rough irregular texture, and often shows visible crystalline structure.

●       Iron concretions: Rounded, dark iron-oxide concretions ("Moqui marbles," "Indian paint pots") are common in sedimentary environments. They are often spherical or disc-shaped and weakly magnetic but are terrestrial in origin.

●       Desert varnish: Dark manganese-oxide coatings on rocks in desert or arid environments can mimic fusion crust. The coating is typically thicker on exposed surfaces and thinner or absent in protected areas.

●       Basalt and dark volcanic rocks: Many people find dark, dense, volcanic rocks and mistake them for meteorites. Basalt is non-magnetic (usually), vesicular, and lacks fusion crust, chondrules, or metal — but the dark colour and density can be deceptive.

 

 

 

 

Meteorites are classified into a hierarchical system based on their composition, mineralogy, and inferred origin. The system can seem bewildering at first, but the basic structure is straightforward. Think of it as a family tree: at the top are three broad types; these divide into groups, which divide further into subtypes.

 

The Three Main Types

1. Stony Meteorites (~94% of all falls)

The most common type. Stony meteorites are composed primarily of silicate minerals (pyroxene, olivine, plagioclase) with varying amounts of iron-nickel metal. They divide into two major categories:

 

●       Chondrites — Primitive, unmelted meteorites that preserve original solar nebula material. They contain chondrules and are the most abundant meteorites found. Named for the chondrules they contain. Think of them as the raw building material of the solar system, unchanged since its formation.

●       Achondrites — Stony meteorites that have been melted and differentiated. They have igneous textures (crystals, flow patterns, brecciation) and come from the crusts and mantles of asteroids, the Moon, or Mars. They lack chondrules.

 

2. Stony-Iron Meteorites (~1% of all falls)

The rarest main type. Stony-irons are a roughly equal mixture of silicate minerals and iron-nickel metal, formed at the core-mantle boundary of differentiated asteroids. There are two main types:

 

●       Pallasites — The most beautiful meteorites. Olivine crystals (often gem-quality peridot) set in a network of iron-nickel metal. When sliced thin and backlit, the olivine crystals transmit light in shades of honey, green, and amber. Among the most prized collector specimens.

●       Mesosiderites — A chaotic mixture of metal and silicate, formed by catastrophic collision between two differentiated asteroids. Less visually ordered than pallasites but scientifically fascinating.

 

3. Iron Meteorites (~5% of all falls, ~30% of finds)

Composed almost entirely of iron-nickel metal. Dense, heavy, strongly magnetic, and often showing the Widmanstätten pattern when cut and etched. Iron meteorites are fragments of the metallic cores of differentiated asteroids — the densest, deepest material that once formed the hearts of small worlds.

 

Iron meteorites are over-represented in meteorite finds (as opposed to witnessed falls) because they are easier to recognise and survive weathering far better than stony meteorites. A stony meteorite exposed to the elements for thousands of years becomes indistinguishable from ordinary rock; an iron meteorite remains obviously metallic for much longer.

 

The Chondrite Groups

Chondrites are divided into groups based on their chemical composition, mineralogy, and the degree to which they have been altered since formation. The main groups are:

 

●       Ordinary chondrites (H, L, LL) — The most abundant meteorites. The letters refer to iron content: H (high metal), L (low metal), LL (low metal, low iron). Numbers after the letter (e.g. H5, L6) indicate petrologic grade — how much thermal metamorphism the meteorite experienced on its parent body, from 3 (most primitive) to 7 (most recrystallised). These are your entry-level chondrites — affordable, widely available, and scientifically significant.

●       Carbonaceous chondrites (CI, CM, CO, CV, CK, CR, CB, CH) — A diverse group of carbon-rich, often dark-coloured chondrites from the outer asteroid belt. They contain organic compounds, sometimes including amino acids — the building blocks of proteins. Some (CI1) match the composition of the Sun's photosphere more closely than any other material. They are typically more expensive than ordinary chondrites due to their scientific significance and fragility.

●       Enstatite chondrites (EH, EL) — Formed in the most chemically reducing conditions of any meteorite group. The silicates are nearly iron-free. Contain unusual sulfide minerals not found elsewhere. Geochemically related to the Earth's composition. Relatively rare.

●       Rumuruti chondrites (R) — Highly oxidized, with nearly no free metal. Very rare — only a few hundred known. The reddish-brown colour of the cut face is characteristic.

 

Petrologic Grade — What the Number Means

The number in a chondrite's classification (e.g. the "5" in "H5" or the "3.2" in "CO3.2") tells you how much processing the rock experienced on its parent body:

 

●       Grade 1-2: Extensive alteration by liquid water on the parent body. Chondrules are dissolved or heavily altered. Phyllosilicate (clay) minerals are abundant. These are the most chemically primitive.

●       Grade 3: Least thermally metamorphosed. Chondrules are sharp and distinct, with diverse textures. Most scientifically valuable for studying original solar system conditions.

●       Grade 4-5: Increasing thermal metamorphism. Chondrules still visible but increasingly blurred. Minerals equilibrating.

●       Grade 6: Advanced metamorphism. Chondrules faint. Mineral compositions uniform throughout the rock.

●       Grade 7: Maximum metamorphism. Chondrules obliterated. Granular, recrystallised texture. Rare.

 

Where Did It Come From? — The Achondrite Groups

Achondrites are classified by their parent body — the planet, moon, or asteroid they came from. For collectors, the most important groups are:

 

●       HED meteorites (Howardites, Eucrites, Diogenites) — From the asteroid 4 Vesta, the second-largest asteroid and the only one large enough to have undergone full planetary-style differentiation. Eucrites are Vestan basalts; diogenites are from deeper in the crust; howardites are surface soil breccias mixing both. The Dawn spacecraft confirmed the Vesta connection in 2012.

●       Lunar meteorites — Pieces of the Moon ejected by asteroid impacts. They look like the Apollo samples in thin section and have been confirmed by comparing their chemistry and isotopic composition to lunar rocks returned by the Apollo missions. Collect a piece of the Moon without a NASA budget.

●       Martian meteorites (SNC) — Pieces of Mars. They are igneous rocks of relatively young age (150 million to 1.3 billion years) that match geochemical models of Martian geology and contain trapped Martian atmospheric gases identical to those measured by Viking landers. Shergottites are the most common type and the most accessible for collectors.

●       Angrites — Very ancient achondrites (4.55 billion years old) from an unknown small parent body. Contain a distinctive green mineral (fassaite) not found in any other meteorite type.

●       Ureilites — Dark, carbon-rich achondrites with an unusual mineralogy. Almahata Sitta (2008) is the most famous ureilite — the only meteorite recovered from a tracked asteroid (2008 TC3).

●       Primitive achondrites (brachinites, lodranites, acapulcoites, winonaites) — Meteorites that experienced partial melting but not complete differentiation. They bridge the gap between chondrites and fully differentiated achondrites.

Where to Buy

Meteorites are available from a range of sources, with significant variation in reliability and authenticity:

 

●       IMCA-registered dealers: The International Meteorite Collectors Association (imca.cc) maintains a code of ethics requiring members to sell only authenticated meteorites with accurate classifications. IMCA membership is the primary marker of a trustworthy dealer. Look for the IMCA member number in dealer listings.

●       Established online dealers: Several reputable dealers operate online shops with broad inventory. Prices are typically fair and specimens are authenticated. Buy from dealers who provide classification data, weight, and ideally a reference to the Meteoritical Bulletin entry.

●       Gem and mineral shows: Major gem and mineral shows (Tucson, Denver, Munich) host large meteorite dealer sections. Shows allow you to handle specimens before buying and compare prices across dealers.

●       eBay and general marketplaces: Exercise caution. Genuine meteorites are sold on eBay, but so are fakes, misidentified rocks, and overpriced common material. If buying on eBay, stick to sellers with established meteorite feedback and IMCA membership. Ask for the Meteoritical Bulletin entry for the specimen.

●       Auction houses: Major auction houses (Christie's, Bonhams, Heritage) occasionally sell meteorites, typically at the premium end of the market. Provenance is usually well-documented.

 

 

What to Look for in a Listing

A legitimate meteorite listing should include:

 

●       Name: The official approved meteorite name (e.g. "NWA 869," "Allende," "Sikhote-Alin").

●       Classification: The official type and group (e.g. "L3-6 chondrite," "IIAB iron").

●       Weight: In grams, to at least one decimal place.

●       Country of origin: Where the meteorite was found.

●       Fall or Find: Whether the fall was witnessed or the specimen was found later.

●       TKW: Total Known Weight — the total mass of all recovered material from that fall or find. A low TKW means the meteorite is rare; a high TKW means it is relatively common.

●       Reference: Ideally a Meteoritical Bulletin number (e.g. "MB 91") confirming official classification.

 

What to Expect to Pay

Meteorite prices vary enormously depending on type, rarity, aesthetic quality, and provenance. As a rough guide for beginners:

 

●       Common ordinary chondrites (NWA 869, Gao-Guenie): $1-5 per gram. An excellent entry point. These are genuine meteorites at accessible prices.

●       Iron meteorites (Sikhote-Alin shrapnel, Canyon Diablo): $2-20 per gram depending on size and form. Etched slices showing the Widmanstätten pattern command premiums.

●       Pallasites (Sericho): $10-30 per gram for standard slices, more for museum-quality etched pieces with exceptional olivine.

●       Carbonaceous chondrites (Allende, NWA 869): $5-50 per gram depending on type. CM2 witnessed falls (Aguas Zarcas, Winchcombe) command $100-500/g or more.

●       Lunar meteorites: $100-1000+ per gram. Genuine Moon rocks are rare and expensive.

●       Martian meteorites (shergottites): $50-500 per gram. Witnessed falls (Zagami, Tissint) are at the high end.

●       Witnessed falls: A significant premium over equivalent finds, reflecting the scientific and historical value of documented recovery.

 

 

Forms and Presentation

Meteorites are sold in several forms, each with different display properties and price implications:

 

●       Whole stones / individuals: The complete meteorite as found, with natural fusion crust exterior. Best for displaying natural features.

●       Part slices: Cut through the meteorite to reveal the interior on one or two faces, with natural crust remaining on the other surfaces. The most popular collector form — shows both interior and exterior.

●       Full slices: Cut completely through the meteorite, showing the interior on both faces. No natural surface remains. Good for studying internal structure.

●       End cuts / endcuts: A slice from one end of the meteorite, with natural crust on one face and a cut interior on the other. Similar to part slices.

●       Fragments: Irregular pieces broken from a larger stone. Affordable but no fusion crust.

●       Micro-mounts: Tiny fragments (under 1g) in gem jars or membrane boxes. An economical way to own rare meteorite types.

 

Storage

Proper storage protects your meteorites from deterioration. The main enemies are moisture (which causes rusting in metal-bearing meteorites and destroys carbonaceous material), handling contamination, and physical damage.

 

●       Store iron and metal-bearing stony meteorites in a low-humidity environment. A sealed container with silica gel desiccant is ideal for long-term storage of valuable pieces.

●       Carbonaceous chondrites (CM, CI, CR types) are particularly sensitive to moisture and handling. Store in sealed membrane boxes or glass-topped boxes and handle with nitrile gloves only.

●       Avoid displaying meteorites near windows where humidity and temperature fluctuate seasonally.

●       Museum-quality display cases with UV-filtering glass protect against both light degradation and casual handling.

 

Handling

Skin oils introduce contaminants that can affect both the meteorite's chemistry (relevant if the specimen ever undergoes scientific analysis) and its surface condition. For significant specimens, handle with nitrile gloves. For robust ordinary chondrites and irons at display level, brief bare-hand contact is acceptable — just wash your hands beforehand and avoid prolonged contact.

 

Never clean meteorites with water — particularly carbonaceous chondrites, which are water-sensitive. Iron meteorites can be lightly brushed to remove loose dust. If a metal-bearing meteorite shows active rusting (red-orange surface oxidation), consult a conservator or experienced dealer before attempting treatment.

 

Documentation

A meteorite without provenance is worth less — scientifically and financially. Keep records for every specimen:

 

●       Name and official classification

●       Weight at acquisition

●       Source / dealer name

●       Date of acquisition

●       Price paid (useful for insurance and future valuation)

●       Any certificates of authenticity provided

●       Meteoritical Bulletin reference number if applicable

 

Photography is also valuable — a good macro photograph of each specimen's fusion crust and interior creates a permanent record of its condition at acquisition.

 

There is no single right way to collect meteorites. Some collectors focus on witnessed falls — meteorites whose fall was observed by people, often with documented trajectories. Others collect by type, trying to assemble a representative example of every major classification. Some focus on single iconic falls (Allende, Sikhote-Alin, Chelyabinsk) at different sizes and forms. Others focus on Canadian heritage material, unusual scientific specimens, or aesthetically exceptional pieces.

 

The most satisfying collections tend to have a coherent philosophy behind them — a reason why each piece belongs. Here are some approaches worth considering as a beginner:

 

●       The "one of each type" approach: Acquire one representative specimen from each major classification — H chondrite, L chondrite, LL chondrite, iron (IAB, IIAB, IIIAB, IVA), pallasite, mesosiderite, eucrite, diogenite, howardite, ureilite, carbonaceous chondrite, lunar, and Martian. This gives you the full range of solar system material in one comprehensive suite.

●       The witnessed falls approach: Focus exclusively on meteorites whose fall was observed. Each specimen comes with a story — a specific date, a specific place, people who saw it fall. This approach prioritises historical and cultural value alongside scientific significance.

●       The scientific approach: Build a collection that tracks a specific scientific theme — aqueous alteration in carbonaceous chondrites, the HED suite from Vesta, the range of Martian meteorite types, or iron meteorite structural diversity.

●       The display approach: Prioritise specimens that look exceptional — etched iron slices, backlit pallasite slabs, large whole stones with complete fusion crust. Aesthetics and display quality drive selection.

 

 

 

For Canadian collectors, there is a particularly meaningful category: Canadian falls and finds. Canada has produced some of the most scientifically significant meteorites in the global record, despite having one of the most challenging recovery environments on Earth.

 

●       Tagish Lake (2000, British Columbia/Yukon) — One of the most primitive and scientifically significant carbonaceous chondrites ever recovered. Fell onto a frozen lake in January, preserved in ice and collected quickly. Contains nanodiamond presolar grains and complex organic chemistry. Among the most studied meteorites of the 21st century.

●       Abee (1952, Alberta) — The largest witnessed enstatite chondrite fall in history at 107 kilograms. Contains minerals first discovered on Earth in this single meteorite. A cornerstone of enstatite chondrite science.

●       Grimsby (2009, Ontario) — Documented by six all-sky cameras, infrasound detectors, and Doppler radar. One of the best-characterised falls in Canadian history, with a computed pre-atmospheric orbit.

●       Springwater (1931, Saskatchewan) — Canada's only pallasite, a main group anomalous specimen. The 53 kg main mass is on display at the Royal Ontario Museum in Toronto.

●       Bruderheim (1960, Alberta) — Canada's largest recovered fall at over 300 kg in hundreds of stones. A cornerstone of noble gas and cosmic ray exposure age research.

●       Whitecourt (find, ~900 CE, Alberta) — Iron meteorites associated with a confirmed impact crater, one of fewer than 20 crater-meteorite pairs known globally. Only about 1,100 years old — geologically instantaneous.

 

Canadian meteorite material carries particular meaning for collectors in this country — it is our piece of the sky, fallen on our soil. We make a point of stocking Canadian material whenever possible.

 

Meteorites occupy an unusual legal position that varies by country and jurisdiction. In Canada:

 

●       Meteorites found in Canada are legal to collect and own without restriction within the country.

●       Exporting a meteorite from Canada requires a cultural property export permit under the Cultural Property Export and Import Act (CPEIA). The permit process is generally straightforward but adds administrative steps for cross-border sales.

●       Meteorites found on private property in Canada belong to the landowner by default. Always obtain permission before searching on private land.

●       Crown land (federal or provincial public land) is generally accessible for meteorite hunting unless it is a protected area (national park, provincial park, ecological reserve).

 

In the United States, meteorites found on federal public lands (BLM land, national forests) are the property of the federal government and collecting them without a permit is illegal. Private land finds belong to the landowner. State and local rules vary.

 

For collectors buying internationally, the key concern is export permits from the country of origin. NWA (Northwest Africa) meteorites from Morocco, Algeria, and other North African countries are typically sold without export documentation — a legally grey area that reflects the practical realities of the desert recovery trade rather than formal legal compliance. Meteorites from Oman, Saudi Arabia, and some other countries have stricter export rules. Lunar and Martian meteorites have no special legal status beyond ordinary meteorite regulations.

Databases and References

●       Meteoritical Bulletin Database (metbull.lpi.usra.edu) — The official database of all approved meteorite names and classifications. Free and publicly accessible. The first stop for any classification question.

●       Meteoritics & Planetary Science (meteoriticalsociety.org) — The primary scientific journal for meteorite research.

●       IMCA (imca.cc) — International Meteorite Collectors Association. Member directory and code of ethics.

 

Books

●       Rocks from Space — O. Richard Norton & Lawrence Chitwood. The standard introductory text for collectors. Excellent photographs and accessible writing.

●       Meteorites: A Petrologic, Chemical and Isotopic Synthesis — Robert Hutchison. The graduate-level reference text. Dense but comprehensive.

●       Meteorites and Their Parent Planets — Harry McSween. Excellent treatment of the geological context of meteorites.

 

Online Communities

●       The Meteorite Exchange (meteorite.com) — Forums, articles, and dealer listings.

●       Meteorite-list (email discussion list) — Long-running community of collectors and researchers.

●       Meteocracy (YouTube) — Accessible videos on meteorite classification, new discoveries, and collector topics.