Paragenetic Mode 1 : Stellar atmosphere condensates
Return to the list of paragentic modesDescription
The earliest phase of mineral formation know, stellar minerals are identified by their extreme isotopic anomalies as pre-solar grains, some individual stellar moissanite (SiC) grains have been dated to around 7 billion years old.
Stage
Minerals
Click on a button to filter by elements. Green = must include. Black = must exclude. Mineral names listed in bold are exclusively known from this paragenetic mode.
| Element | Count | Percent |
|---|
| H | Hydrogen | 1 | 4.55% |
| C | Carbon | 4 | 18.18% |
| N | Nitrogen | 1 | 4.55% |
| O | Oxygen | 10 | 45.45% |
| Mg | Magnesium | 4 | 18.18% |
| Al | Aluminium | 3 | 13.64% |
| Si | Silicon | 4 | 18.18% |
| P | Phosphorus | 1 | 4.55% |
| S | Sulfur | 2 | 9.09% |
| Ca | Calcium | 2 | 9.09% |
| Ti | Titanium | 2 | 9.09% |
| V | Vanadium | 1 | 4.55% |
| Cr | Chromium | 2 | 9.09% |
| Fe | Iron | 7 | 31.82% |
| Ni | Nickel | 2 | 9.09% |
| Ru | Ruthenium | 2 | 9.09% |
| Os | Osmium | 1 | 4.55% |
| Ir | Iridium | 2 | 9.09% |
References
Hazen, Robert M., Morrison, Shaunna M. (2022) On the paragenetic modes of minerals: A mineral evolution perspective. American Mineralogist, 107 (7) 1262-1287 doi:10.2138/am-2022-8099
