Lunar Meteorite

Dhofar 1627 and 1980
(paired stones)



Dhofar 1627. Click on image for enlargement.

(photo credit: anonymous finder)

A slice of Dhofar 1627. Click on image for enlargement.

(photo credit: Randy Korotev)

A bigger slice of Dhofar 1627. Click on image for enlargement.
(photo credit: Randy Korotev)

Several slices of Dhofar 1980. Click on image for enlargement

(photo credit: Randy Korotev)

Close-up of two pieces of Dhofar 1980

(photo credit: Randy Korotev)

Photomicrograph of a thin section prepared from the two slices above. Click on image for enlargement.

(photo credit: Axel Wittmann)


from The Meteoritical Bulletin, No. 100

Dhofar 1627

Zufar, Oman
Found: 2010
Mass: 86.1 g

Lunar meteorite (feldspathic breccia)

History: An 86.1g stone was found in the desert.

Physical characteristics: The stone lacks a fusion crust and shows fractures on the surface. The interior is rich in angular or slightly rounded clasts (to 1 cm). Some clasts are dark gray, a few are white, and the matrix is stained red by hematite.

Petrography: (S. Seddio and B. Jolliff, WUSL) A polished 18.1 mm by 8.75 mm section reveals rounded or subrounded lithic clasts of very fine grained, glassy matrix impact-melt breccia and poikilitic melt breccia fragments plus mineral clasts, welded together to form a well-consolidated, clast-rich breccia. Lithic clasts range from feldspathic, aphanitic, glassy-matrix breccias to somewhat more mafic granulitic clasts in which poikiloblastic pyroxene encloses plagioclase grains. Such clasts are abundant and typically contain partially resorbed magnesian (~Fo75) olivine grains. Plagioclase mineral clasts and grains in lithic clasts are partially converted to maskelynite and are coarsely fractured where crystalline. Fine feldspathic glass veins transect some clasts. Lithic clasts and mineral grains contain fractures, but fractures tend to be healed and closed at grain boundaries. Some of the larger fractures have been filled with terrestrial calcite, celestite, and Fe-oxide or Fe-oxyhydroxide, especially near Fe-Ni metal grains.

Geochemistry: The most abundant minerals include plagioclase (An87.2-98.6Ab1.4-8.9Or<0.1-4.3), low-Ca pyroxene (En64.1-77.0Fs17.6-33.3Wo2.6-11.2, Fe/Mn=41-70), high-Ca pyroxene (En34.8-49.9Fs13.2-30.5Wo34.7-38.8, Fe/Mn=50-70), and olivine (Fo64.2-75.9, Fe/Mn=76-118). Fe-Ni metal, troilite, merrillite, and poikilitic ilmenite surround crystals of plagioclase and pyroxene. Most Fe-Ni metal grains (up to 1-mm in size) are rimmed by iron oxide/oxyhydroxide. Bulk composition (R. Korotev, WUSL): 0.54% Na2O; 5.8% FeO, 530 ppm Ni, 1000 ppm Sr, 7.8 ppm Sm, 2.7 ppm Th.

Classification: Achondrite (lunar clast-rich melt breccia).

Specimens: 17.2 g is on deposit at WUSL. The main mass is held by the anonymous finder.


from The Meteoritical Bulletin, No. 103

Dhofar 1980

Zufar, Oman
Found: 2012 December
Mass: 23.5

Classification: Lunar meteorite (feldspathic breccia)

History: Found during a foot search.

Physical characteristics: Six stones with masses of 5.8, 5.5, 4.9, 3.2, 3.2, and 0.9 g and ~2.5 to 1.5 cm in maximum size. Two stones contain significant dark, speckled fusion crust that cover most of one face of the respective stones. Shapes are angular to sub-rounded and colors range from grey, reddish, and tan with dark, sub-mm veins that connect melt pods. A 1.2-g slice of the 5.5-g stone shows a well consolidated rock with a brecciated texture of angular clasts that exhibit orange staining, and a few that are light colored. These clasts are set in a very fine-grained, gray groundmass that accounts for ~20 vol% of the sample.

Petrography: (A. Wittmann, WUSL) A 23.3 by 15.9 mm petrographic thin section exhibits a well consolidated, crystalline, melt rock that contains abundant angular, dark, apahnitic clasts, and light, angular to sub-rounded clasts that display rusty, orange staining. The complex, clast-rich, intergranular melt rock has a groundmass of 10 µm feldspar, olivine, and pyroxene, plus minor merrillite, FeNi metal, and troilite grains. Monomineralic clasts include <1 mm plagioclase, olivine, pyroxene, and spherical FeNi metal grains that are variably deformed and partly assimilated. Polymineralic clasts include dark, microcrystalline, intergranular lithic clasts that contain up to 100 µm mineral clasts of plagioclase; medium to fine-grained poikilitic lithic clasts with noritic and anorthositic mineralogies; medium-grained anorthositic clasts with granulitic textures; medium-grained anorthositic cumulate clasts of >0.3 mm feldspar with interstitial, poikilitic pyroxene and FeNi metal particles; and medium to fine-grained sub-ophitic domains of feldspar laths, zoned pigeonite, rhyolitic mesostasis, armalcolite, troilite, and FeNi metal intergrown with schreibersite. Silicate minerals frequently show reduced birefringence and intense brittle deformation. Many olivine and magnesian pyroxene clasts are extensively altered to phyllosilicates, and plagioclase shows orange staining in places. Other common alteration phases are SrSO4, CaSO4, CaCO3, and Fe-oxides that fill fractures; Fe-oxides also replace metal and troilite.

Geochemistry: Mineral compositions and geochemistry: (A. Wittmann, P. Carpenter, WUSL) Feldspar (Ab2.7-14.6An84-97Or0.1-1.9; n=21) is the most abundant component, followed by pyroxene that is mainly pigeonite (En61-75Fs20-31Wo5-14; Fe/Mn = 38-75; n=18), minor augite (En76-79Fs46-50Wo36-39; Fe/Mn = 41-48; n=3), and rare low-Ca pyroxene (En75-76Fs20-21Wo4.3-4.5; Fe/Mn = 55-58; n=2), and olivine that is mainly magnesian (Fo71-74; n=16; Fo66; n=1; Fe/Mn = 74-119). Minor components are rhyolitic mesostasis (SiO2 = 70%, K2O = 4%), Fe-Mg armalcolite (n=2) with 0.17% ZrO2, FeNi-metal (Ni = 4.4-5.9%, Co = 0.28±0.56%, n=5) and is in some cases associated with minor troilite and schreibersite (P = 12.6%, Ni = 10.6-14%, Co = 0.24-0.36%; n=2). Bulk composition (INAA, R. Korotev, WUSL): Na2O = 0.56, FeO = 5.8 (both in %), Ni = 475, Sr = 800, Sm = 7.3, and Th = 2.5 (all in ppm). Overall, indistinguishable from Dhofar 1627.

Classification: lunar (feldspathic breccia).

Specimens: Type specimen, ASU; TS and INAA samples at WUSL.


Randy Says…

It's relatively rich in incompatibles elements for a feldspathic lunar meteorite and overall similar in composition to soils from Apollo 16.


More Information

Meteoritical Bulletin Database

Dhofar 1627 | 1980


Schematic Map of the Find Locations of the Dhofar Lunar Meteorites


Korotev R. L. (2012) Lunar meteorites from Oman. Meteoritics & Planetary Science 47, 1365–1402. doi: 10.1111/j.1945-5100.2012.01393.x

Korotev R. L. (2017) Update (2012–2017) on lunar meteorites from Oman. Meteoritics & Planetary Science 52, 1251-1256.
All Korotev data on Omanian lunar meteorites.

Korotev R. L. (2013) Siderophile elements in brecciated lunar meteorites (abstract). In 44th Lunar and Planetary Science Conference, abstract no. 1028.

Korotev R. L., Irving A. J., and Bunch T. E. (2012) Keeping Up With the Lunar Meteorites — 2012 (abstract). In Lunar and Planetary Science XLIII, abstract no. 1152, 43rd Lunar and Planetary Science Conference.

Korotev R. L. and Irving A. J. (2015) Keeping up with the lunar meteorites 2015. 46th Lunar and Planetary Science Conference, abstract no. 1942.



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Prepared by
: Randy L. Korotev
Department of Earth and Planetary Sciences
Washington University in St. Louis

Please don't contact me about the meteorite you think you've found until you read this and this.


Last revised: 13-June-2017