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Summary
| Description | A Tinsley-Wallerstein diagram shows the iron abundance, [Fe/H], on the x-axis and the abundance of alpha process elements, [alpha/fe], on the y-axis. It helps to assess which population of the Milky Way a stars belongs to: (a) thin disk / low-alpha sequence stars with [alpha/Fe] ≳ 0.2, (b) thick disk / high-alpha sequence stars with [alpha/Fe] ≲ 0.2, or (c) stars that have likely not been born at the same time as the disk, like metal poor stars with [Fe/H] ≲ -1.0, or accreted stars with lower iron and alpha-abundances than the stellar disk). The data from Wallerstein (1962) is shown as red circles on top of the 2020 public data from the large scale stellar spectroscopic surveys APOGEE (DR16) and GALAH (DR3). |
| Source | Made from data of Wallerstein (1962),APOGEE DR16 and GALAH+DR3 |
| Author | GingerLemon |
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 05:18, 9 March 2021 | | 1,890 × 980 (220 KB) | GingerLemon | {{Information |Description= |Source={{own}} |Date= |Author= GingerLemon |Permission= |other_versions= }} |
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