HED Meteorites
HED meteorites are a group of achondrites originating from asteroid Vesta, including eucrites, diogenites, and howardites. These differentiated meteorites provide insight into early planetary crust formation.
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NWA 18048 Eucrite-pmict Meteorite End Cut, 1530.00g, Main Mass, Mixed Clast Structure -
NWA 18452 Eucrite-br Meteorite Slice, 33.79g, Mirror Polished, UV Fluorescent & Phosphorescent -
NWA 17918 Diogenite-pm Meteorite Slice, HED Achondrite, 9.29g, Polymict Breccia from Vesta -
NWA 18048 Eucrite-pmict Meteorite Slice, 128.81g, Mirror Polished, Vivid Clast Boundaries -
NWA 18048 Eucrite-pmict Meteorite Slice, 119.29g, Mirror Polished Impact Breccia -
NWA 18048 Eucrite-pmict Meteorite Slice, 120.00g, Mirror Polished HED Achondrite from Vesta -
NWA 18048 Eucrite-pmict Meteorite Slice, 133.72g, Mirror Polished, HED Achondrite from Vesta -
NWA 17918 Diogenite-pm Meteorite End Cut, 13.33g, Polished Breccia Texture from Vesta -
NWA 17708 Howardite Meteorite Part Slice, Achondrite, 12.00g, Fusion Crust Preserved -
NWA 17708 Howardite Meteorite Part Slice, Achondrite, 6.15g, Partial Fusion Crust -
NWA 17708 Howardite Meteorite Part Slice, Achondrite, 4.24g, Fresh Fusion Crust -
NWA 17708 Howardite Meteorite End Cut, 350.42g, Fresh Fusion Crust, HED Achondrite from Vesta -
NWA 17708 Howardite Meteorite Slice, 38.80g, Fresh Fusion Crust -
NWA 17708 Howardite Meteorite End Cut, 29.12g, 50% Fusion Crust Coverage -
NWA 17708 Howardite Meteorite Slice, 34.51g, Rippled Fusion Crust, HED Achondrite from Vesta -
NWA 17708 Howardite Meteorite Slice, 26.23g, Rippled Fusion Crust on 50% Edge -
NWA 17708 Howardite Meteorite Part Slice, 21.31g, 50% Fresh Fusion Crust -
NWA 17708 Howardite Meteorite Slice, 35.21g, Fresh Fusion Crust on 50% Edge -
NWA 17708 Howardite Meteorite Individual, 36.92g, Fresh Fusion Crust, HED Achondrite from Vesta -
NWA 17708 Howardite Meteorite Slice, 38.73g, Fusion Crust on 50% Edge, HED Achondrite from Vesta
About HED Meteorites
Howardites, Eucrites, and Diogenites For Sale
HED meteorites are a group of achondrites representing igneous material from a differentiated asteroid, most commonly linked to asteroid 4 Vesta. These meteorites preserve both crustal and deeper geological history from an early planetary body that formed, melted, and evolved during the early Solar System.
The HED group includes howardites, eucrites, and diogenites, each with distinct mineralogy, texture, and origin within the Vestan system. Some formed as basaltic crust, others as deeper plutonic material, while others are brecciated mixtures created by repeated impact events.
Each specimen offered by Treasure Coast Meteorite Co. is carefully sourced, authenticated, and selected for quality, stability, and collector appeal.
What Are HED Meteorites?
HED meteorites are a group of achondrites that originated from the differentiated asteroid Vesta. The name “HED” refers to howardites, eucrites, and diogenites—three closely related meteorite types formed through igneous processes.
Unlike primitive chondrites, HED meteorites represent material from a parent body that experienced melting, separation into layers, and crust formation early in Solar System history. As a result, they are more comparable to volcanic and crustal rocks found on Earth.
Origin: Asteroid Vesta
HED meteorites are widely accepted to originate from asteroid Vesta, one of the largest and most geologically complex bodies in the asteroid belt.
Data from NASA’s Dawn mission confirmed strong compositional matches between Vesta’s surface and HED meteorites found on Earth. Vesta is a differentiated body with a crust, mantle, and core structure, meaning HED meteorites provide direct samples of a small protoplanet that underwent planetary-style evolution.
These meteorites were ejected from Vesta by large impact events and eventually delivered to Earth over millions of years.
The Three HED Types
Eucrites
Eucrites are basaltic rocks formed from surface or near-surface lava flows on Vesta. They are typically fine-grained and often display brecciated textures or distinct clasts.
Diogenites
Diogenites originate deeper within Vesta’s crust and are composed primarily of orthopyroxene. They tend to be coarser-grained and represent slower cooling at depth.
Howardites
Howardites are regolith breccias formed by impact mixing of eucrite and diogenite material on Vesta’s surface. These specimens often display visually striking mixtures of light and dark clasts.
Together, these three types represent different layers and geological processes within the same parent body.
Why Collectors Value HED Meteorites
HED meteorites occupy a unique position in meteorite collecting. They are:
- Planetary crust material from a differentiated body
- Scientifically significant, with a well-established link to Vesta
- Visually diverse, ranging from clean basaltic textures to complex breccias
- More accessible than lunar or Martian meteorites while still representing planetary geology
For collectors, HED meteorites offer a direct connection to early planetary formation without the extreme rarity and cost associated with lunar or Martian material.
Collecting HED Meteorites
Because HED meteorites encompass multiple subtypes and textures, they provide a wide range of collecting opportunities:
- Eucrites for basaltic crust material
- Diogenites for deep crust samples
- Howardites for mixed regolith breccias
Each specimen represents a different part of Vesta’s geological history, making them particularly appealing for collectors interested in planetary differentiation and impact processes.