| Model . | Initial state . | Mini|${}(\, \mathrm{M}_\odot )$| . | Mf|${}(\, \mathrm{M}_\odot )$| . | MHe, f|${}(\, \mathrm{M}_\odot )$| . | Z (Z⊙) . | Code up to Ne burning . | 3D initial conditions . | PPM scheme . | Axis treatment . | Nucleon correlations . | Weak magnetism . | ga, s . |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| z9.6 | H ZAMS | 9.6 | 9.6 | 1.38 | 0 | kepler | No | CW84 | Coarsening | No | no | 0 |
| s11.8 | H ZAMS | 11.8 | 10.4 | 2.45 | 1 | kepler | Yes | CS08 | Coarsening | Yes | no | −0.05 |
| z12 | H ZAMS | 12.0 | 12.0 | 2.49 | 0 | kepler | Yes | CW84 | Coarsening | Yes | no | −0.05 |
| s12.5 | H ZAMS | 12.5 | 9.78 | 3.17 | 1 | kepler | Yes | CW84 | Coarsening | Yes | no | 0 |
| he2.8 | He ZAMS | 2.8 | 1.49 | 1.49 | 1 | bec | No | CW84 | Coarsening | No | no | 0 |
| he3.0 | He ZAMS | 3.0 | 3.00 | 3.00 | 1 | kepler | Yes | CS08 | Fourier filter | Yes | yes | −0.05 |
| he3.5 | He ZAMS | 3.5 | 2.39 | 2.39 | 1 | bec | No | CS08 | Fourier filter | Yes | no | −0.05 |
| Model . | Initial state . | Mini|${}(\, \mathrm{M}_\odot )$| . | Mf|${}(\, \mathrm{M}_\odot )$| . | MHe, f|${}(\, \mathrm{M}_\odot )$| . | Z (Z⊙) . | Code up to Ne burning . | 3D initial conditions . | PPM scheme . | Axis treatment . | Nucleon correlations . | Weak magnetism . | ga, s . |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| z9.6 | H ZAMS | 9.6 | 9.6 | 1.38 | 0 | kepler | No | CW84 | Coarsening | No | no | 0 |
| s11.8 | H ZAMS | 11.8 | 10.4 | 2.45 | 1 | kepler | Yes | CS08 | Coarsening | Yes | no | −0.05 |
| z12 | H ZAMS | 12.0 | 12.0 | 2.49 | 0 | kepler | Yes | CW84 | Coarsening | Yes | no | −0.05 |
| s12.5 | H ZAMS | 12.5 | 9.78 | 3.17 | 1 | kepler | Yes | CW84 | Coarsening | Yes | no | 0 |
| he2.8 | He ZAMS | 2.8 | 1.49 | 1.49 | 1 | bec | No | CW84 | Coarsening | No | no | 0 |
| he3.0 | He ZAMS | 3.0 | 3.00 | 3.00 | 1 | kepler | Yes | CS08 | Fourier filter | Yes | yes | −0.05 |
| he3.5 | He ZAMS | 3.5 | 2.39 | 2.39 | 1 | bec | No | CS08 | Fourier filter | Yes | no | −0.05 |
Notes: Mini is the initial mass of the stellar evolution model. For the single-star progenitors, this is the ZAMS mass; for the helium star (binary) models, it is the initial helium star mass. Mf and MHe, f are the progenitor mass and the helium (core) mass at the pre-supernova stage; these are identical for the stripped-envelope models. Z is the initial metallicity. CW84 refers to the original PPM reconstruction of Colella & Woodward (1984), and CS08 refers to the sixth-order extremum-preserving method of Colella & Sekora (2008). ga, s is the strangeness contribution to the axial coupling constant for neutral currents. Tauris et al. (2015).
| Model . | Initial state . | Mini|${}(\, \mathrm{M}_\odot )$| . | Mf|${}(\, \mathrm{M}_\odot )$| . | MHe, f|${}(\, \mathrm{M}_\odot )$| . | Z (Z⊙) . | Code up to Ne burning . | 3D initial conditions . | PPM scheme . | Axis treatment . | Nucleon correlations . | Weak magnetism . | ga, s . |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| z9.6 | H ZAMS | 9.6 | 9.6 | 1.38 | 0 | kepler | No | CW84 | Coarsening | No | no | 0 |
| s11.8 | H ZAMS | 11.8 | 10.4 | 2.45 | 1 | kepler | Yes | CS08 | Coarsening | Yes | no | −0.05 |
| z12 | H ZAMS | 12.0 | 12.0 | 2.49 | 0 | kepler | Yes | CW84 | Coarsening | Yes | no | −0.05 |
| s12.5 | H ZAMS | 12.5 | 9.78 | 3.17 | 1 | kepler | Yes | CW84 | Coarsening | Yes | no | 0 |
| he2.8 | He ZAMS | 2.8 | 1.49 | 1.49 | 1 | bec | No | CW84 | Coarsening | No | no | 0 |
| he3.0 | He ZAMS | 3.0 | 3.00 | 3.00 | 1 | kepler | Yes | CS08 | Fourier filter | Yes | yes | −0.05 |
| he3.5 | He ZAMS | 3.5 | 2.39 | 2.39 | 1 | bec | No | CS08 | Fourier filter | Yes | no | −0.05 |
| Model . | Initial state . | Mini|${}(\, \mathrm{M}_\odot )$| . | Mf|${}(\, \mathrm{M}_\odot )$| . | MHe, f|${}(\, \mathrm{M}_\odot )$| . | Z (Z⊙) . | Code up to Ne burning . | 3D initial conditions . | PPM scheme . | Axis treatment . | Nucleon correlations . | Weak magnetism . | ga, s . |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| z9.6 | H ZAMS | 9.6 | 9.6 | 1.38 | 0 | kepler | No | CW84 | Coarsening | No | no | 0 |
| s11.8 | H ZAMS | 11.8 | 10.4 | 2.45 | 1 | kepler | Yes | CS08 | Coarsening | Yes | no | −0.05 |
| z12 | H ZAMS | 12.0 | 12.0 | 2.49 | 0 | kepler | Yes | CW84 | Coarsening | Yes | no | −0.05 |
| s12.5 | H ZAMS | 12.5 | 9.78 | 3.17 | 1 | kepler | Yes | CW84 | Coarsening | Yes | no | 0 |
| he2.8 | He ZAMS | 2.8 | 1.49 | 1.49 | 1 | bec | No | CW84 | Coarsening | No | no | 0 |
| he3.0 | He ZAMS | 3.0 | 3.00 | 3.00 | 1 | kepler | Yes | CS08 | Fourier filter | Yes | yes | −0.05 |
| he3.5 | He ZAMS | 3.5 | 2.39 | 2.39 | 1 | bec | No | CS08 | Fourier filter | Yes | no | −0.05 |
Notes: Mini is the initial mass of the stellar evolution model. For the single-star progenitors, this is the ZAMS mass; for the helium star (binary) models, it is the initial helium star mass. Mf and MHe, f are the progenitor mass and the helium (core) mass at the pre-supernova stage; these are identical for the stripped-envelope models. Z is the initial metallicity. CW84 refers to the original PPM reconstruction of Colella & Woodward (1984), and CS08 refers to the sixth-order extremum-preserving method of Colella & Sekora (2008). ga, s is the strangeness contribution to the axial coupling constant for neutral currents. Tauris et al. (2015).
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
