Table 1
[Mn/Fe] yields for selected thermonuclear (Ia), core collapse (II), and hypernova (HN) models of solar-metallicity progenitors.
| Model name | SN type | Masses | [Mn/Fe] | Ref. |
|
|
||||
| N100 | Ia | near-MCh | 0.33 | (1) |
| N5def | Ia | near-MCh | 0.36 | (2) |
| N150def | Ia | near-MCh | 0.42 | (2) |
| W7 | Ia | near-MCh | 0.15 | (3) |
| W7 | Ia | near-MCh | 0.02 | (4) |
|
|
||||
| 1.1_0.9 | Ia | sub-MCh | –0.15a | (5) |
| 1.06 M⊙ | Ia | sub-MCh | –0.13a | (6) |
|
|
||||
| WW95Bb | II | 11 < M/M⊙ < 40 | –0.15c | (7) |
| LC03Dd | II | 13 < M/M⊙ < 35 | –0.27c | (8) |
| N06 | II+HN | 13 < M/M⊙ < 40 | –0.31c | (9) |
Notes. Only models of near-MCh SNe Ia predict [Mn/Fe] ≥ 0.0.
The given reference is for the explosion model; the respective [Mn/Fe] yields are published here for the first time, assuming that the main sequence progenitor had a solar metallicity (Asplund et al. 2009) and primary C, N, O was converted to 22Ne during core He-burning.
Reference. (1) Seitenzahl et al. (2013); (2) Fink et al. (2013); (3) Iwamoto et al. (1999); (4) Maeda et al. (2010); (5) Pakmor et al. (2012); (6) Ruiter et al. (2013); (7) Woosley & Weaver (1995); (8) Limongi & Chieffi (2003); (9) Nomoto et al. (2006).
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