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NWA 13159
NWA 13159
Found 2019
Chondrite
L6-Melt Breccia
Specimen is a 4.25g slice
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Dramaticaly impacted during its journey in the solar system, this 4.56Ga chondritic rock partialy melted by the event, allows us to actually see the phenomenon, as if we had witnessed
| Northwest Africa 13159 |
| Basic information |
Name: Northwest Africa 13159
This is an OFFICIAL meteorite name.
Abbreviation: NWA 13159
Observed fall: No
Year found: 2019
Country: (Northwest Africa)
Mass: 1393 g
|
Classification
history: |
This is 1 of 44 approved meteorites classified as L6-melt breccia.
|
| Comments: |
Approved 9 Feb 2020 |
| Writeup |
Writeup from MB 109:
Northwest Africa 13159 (NWA 13159)
(Northwest Africa)
Purchased: 2019
Classification: Ordinary chondrite (L6, melt breccia)
History: The meteorite was purchased from a Morrocan dealer at the mineral show in Munich, Germany.
Physical characteristics: Many small dark brownish individuals lacking any fusion crust.
Petrography: The meteorite dominantly consists of partly recrystallized melt rock regions with characteristic FeNi metal and sufide spherules. Few unmelted regions are of L6 type with plagioclase grains about 80 µm in size; no metal or sulfide veins are observed. |
Data from:
MB109
Table 0
Line 0: |
| Place of purchase: |
Munich, Germany |
| Date: |
P 2019 |
| Mass (g): |
1392.5 |
| Pieces: |
many |
| Class: |
L6-melt breccia |
| Shock stage: |
S3 |
| Weathering grade: |
W1 |
| Fayalite (mol%): |
23.4±0.2 (n=11) |
| Ferrosilite (mol%): |
20±0.6 (n=13) |
| Wollastonite (mol%): |
1.7±0.1 (n=13) |
| Classifier: |
A. Greshake, MNB |
| Type spec mass (g): |
23.4 |
| Type spec location: |
MNB |
| Main mass: |
Fabien Kuntz and Ingo Schaefer |
| Comments: |
Submitted by Ansgar Greshake | |
Institutions
and collections |
MNB: Museum für Naturkunde, Invalidenstraße 43, D-10115 Berlin, Germany (institutional address; updated 24 Dec 2011)
Kuntz: Fabien Kuntz, France; Website (private address) |
Chondrites are stony (non-metallic) meteorites that have not been modified due to melting or differentiation of the parent body. They are formed when various types of dust and small grains that were present in the early solar system accreted to form primitive asteroids.
Chondrites were formed by the accretion of particles of dust and grit present in the primitive Solar System which gave rise to asteroids over 4,550 million years ago. These asteroid parent bodies of chondrites are (or were) small to medium sized asteroids that were never part of any body large enough to undergo melting and planetary differentiation. Dating using 206Pb/204Pb gives an estimated age of 4,566.6 ± 1.0 Ma years, matching ages for other chronometers. Another indication of their age is the fact that the abundance of non-volatile elements in chondrites is similar to that found in the atmosphere of the Sun and other stars in our galaxy. Although chondritic asteroids never became hot enough to melt based upon internal temperatures, many of them reached high enough temperatures that they experienced significant thermal metamorphism in their interiors. The source of the heat was most likely energy coming from the decay of short-lived radioisotopes (half-lives less than a few million years) that were present in the newly formed solar system, especially 26Al and 60Fe, although heating may have been caused by impacts onto the asteroids as well. Many chondritic asteroids also contained significant amounts of water, possibly due to the accretion of ice along with rocky material. As a result, many chondrites contain hydrous minerals, such as clays, that formed when the water interacted with the rock on the asteroid in a process known as aqueous alteration. In addition, all chondritic asteroids were affected by impact and shock processes due to collisions with other asteroids. These events caused a variety of effects, ranging from simple compaction to brecciation, veining, localized melting, and formation of high-pressure minerals. The net result of these secondary thermal, aqueous, and shock processes is that only a few known chondrites preserve in pristine form the original dust, chondrules, and inclusions from which they formed.
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