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Seres meteorite, Serres, Serres Prefecture, Macedonia Department, Greece

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Latitude & Longitude (WGS84): 41° 2' 59'' North , 23° 34' 0'' East
Latitude & Longitude (decimal): 41.05000,23.56667
Köppen climate type:Cfb : Temperate oceanic climate
Non-native locality type:Meteorite

Ordinary chondrite, black (H4)
Fell, June 1818; 8.5 kg

Historical details of the recovery of Seres are vague. The history of our chemical and mineralogical understanding of Seres is somewhat more complete. In 1832 Berzelius recognized four separate phases in Seres (chromite, olivine, meteoritic iron, and troilite), but only olivine and meteoritic iron were mineralogically described essentially as we would describe them today. The olivine (Fa17) and orthopyroxene ('bronzite') are characteristic of the H-chondrite geochemical group. Mineralogically the meteorite consists primarily of dominant olivine and somewhat lesser amounts of low-Ca pyroxene along with minor amounts of Fe-Ni metal (kamacite and taenite), troilite, and other silicates. Accessory chromite and other minor opaques are also reported. Troilite, often polycrystalline, is found in fine-grained kamacite-troilite aggregates which have sometimes drawn detailed attention. Silica-bearing chondrules and clasts have also drawn similar attention.

Seres is often described as a gas-poor meteorite and has an unusually short 0.64 Ma cosmic ray exposure (CRE) age.

The H (relatively high in total iron) chondrites are the second largest group of witnessed ordinary chondrite falls (nearly 40% of well-classified falls). The H4 petrologic type represents less than 20 % of the H chondrites. Seres is the 20th most massive of 51 recognized falls now classified exactly as 'H4' chondrites (May 2017).

The main mass has been kept at the Naturhistorisches Museum in Wiens (Vienna).

What's in a name? The Seres meteorite has also been referred to as the 'Macedonia' and the 'Serrai' meteorite. The current English transcription for both the city and the prefecture is 'Serres'. However, to avoid confusion official meteorite 'names' (labels) which have been in currency for a century or two are almost never abandoned.

Mineral List

10 valid minerals.

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Berzelius, J.J. (1832) Undersökning af en vid Bohumiliz i Böhmen funnen jernmassa. Handl. Svenska Vetenskaps-Akad. 106-119.
Wood, J.A. (1958) Silicate Meteorite Structures and the Origin of Meteorites: Dissertation, Ph.D: Massachusetts Institute of Technology. 172 pages. (June 1958).
Mason, B. (1963) Olivine Composition in Chondrites: Geochimica et Cosmochimica Acta 27(9): 1011-1023. (Sept 1963).
Heymann, D. & Anders, E. (1967) Meteorites with short cosmic-ray exposure ages, as determined from their Al 26 content: Geochimica et Cosmochimica Acta 31(10): 1793-1809. (Oct1967) .
Wood, J. A. (1967) Chondrites: Their metallic minerals, thermal histories, and parent planets. Icarus 6 (1):1-49.
Ramdohr, P. (1973). The Opaque Minerals in Stony Meteorites. Elsevier Publishing Company: Amsterdam; London: New York. 245 pages.
Sears. D.W. & Sears, H. (1977) Sketches in the history of Meteoritics 2: The Early chemical and mineralogical work: Meteoritics 12(1): 27-46. (March 1977)
Graham, A.L., Bevan, A.W.R. & Hutchison, B. (1985) Catalogue of Meteorites (4/e). University of Arizona Press: Tucson.
Brigham, C.A. et al. (1986) Silica-bearing chondrules and clasts in ordinary chondrites. Geochimica et Cosmochimica Acta 50(8): 1573-1836. (Aug 1986).
Britt, D. T. & Pieters, C. M. (1991) Black ordinary chondrites - an analysis of abundance and fall frequency: Meteoritics 26(4): 279-285. (Dec 1991).
Graf, Th. & Marti K. (1995) Collisional history of H chondrites. J. Geophys. Res. (Planets) 100: 21247–21263. (Oct 1995).
Grady, M.M. (2000). Catalogue of Meteorites (5/e). Cambridge University Press: Cambridge; New York; Oakleigh; Madrid; Cape Town. 689 pages.
Hezel, D.C. et al. (2006) Origin of SiO2-rich components in ordinary chondrites. Geochimica et Cosmochimica Acta 70(6): 1548-1564. (March 2006).

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