Open Access
Table A.2.
SNcc yield models used in this work via the abunfit package (see below for references).
Category | Name | Ref. | Remarks |
---|---|---|---|
SNcc | |||
Input | Ro10_0 | a,b | Zinit = 0 Z⊙, M ∈ [8, 50] M⊙ |
Ro10_2E-6 | a,b | Zinit = 0.0001 Z⊙, M ∈ [8, 50] M⊙ | |
Ro10_2E-4 | a,b | Zinit = 0.01 Z⊙, M ∈ [8, 50] M⊙ | |
Ro10_2E-3 | a,b | Zinit = 0.1 Z⊙, M ∈ [8, 50] M⊙ | |
Ro10_2E-2 | a,b | Zinit = 1 Z⊙, M ∈ [8, 50] M⊙ | |
Nomoto | No13_SNcc_0 | c | Core-collapse Zinit = 0 Z⊙, M ∈ [11, 140] M⊙ |
No13_SNcc_0.001 | c | Core-collapse Zinit = 0.05 Z⊙, M ∈ [11, 40] M⊙ | |
No13_SNcc_0.004 | c | Core-collapse Zinit = 0.2 Z⊙, M ∈ [11, 40] M⊙ | |
No13_SNcc_0.008 | c | Core-collapse Zinit = 0.4 Z⊙, M ∈ [11, 40] M⊙ | |
No13_SNcc_0.02 | c | Core-collapse Zinit = 1 Z⊙, M ∈ [11, 40] M⊙ | |
No13_SNcc_0.05 | c | Core-collapse Zinit = 2.5 Z⊙, M ∈ [11, 40] M⊙ | |
No13_PISNe_0 | c | Pair-instability SNeZinit = 0 Z⊙, M ∈ [140, 300] M⊙ | |
No13_SNe_0 | c | Core-collapse M ∈ [11, 140] M⊙ and pair-instability M ∈ [140, 300] M⊙, Zinit = 0 Z⊙ | |
No13_HNe_0 | c | Hyper-novae Zinit = 0 Z⊙ Z⊙, M ∈ [20, 140] M⊙ | |
No13_HNe_0.001 | c | Hyper-novae Zinit = 0.05 Z⊙, M ∈ [20, 40] M⊙ | |
No13_HNe_0.004 | c | Hyper-novae Zinit = 0.2 Z⊙, M ∈ [20, 40] M⊙ | |
No13_HNe_0.008 | c | Hyper-novae Zinit = 0.4 Z⊙, M ∈ [20, 40] M⊙ | |
No13_HNe_0.02 | c | Hyper-novae Zinit = 1 Z⊙, M ∈ [20, 40] M⊙ | |
No13_HNe_0.05 | c | Hyper-novae Zinit = 2.5 Z⊙, M ∈ [20, 40] M⊙ | |
Massive | He0210_SNcc_0 | d,e | Core-collapse Zinit = 0 Z⊙, M ∈ [10, 100] M⊙ |
He0210_PISNe_0 | d,e | Pair-instability SNeZinit = 0 Z⊙, M ∈ [140, 260] M⊙ | |
He0210_SNe_0 | d,e | Core-collapse M ∈ [10, 100] M⊙ and pair-instability, M ∈ [140, 260] M⊙, Zinit = 0 Z⊙ | |
Neutrino | Su16_N20 | f | Incl. neutrino transport, calibrated for a Nomoto & Hashimoto (1988) progenitor to explode as SN1987A, Zinit = 1 Z⊙, M ∈ [12, 120] M⊙ |
Su16_W18 | f | Incl. neutrino transport, calibrated for a Utrobin et al. (2015) progenitor to explode as SN1987A, Zinit = 1 Z⊙, M ∈ [12, 120] M⊙ |
Notes. Models used in our input cosmological simulations are given in bold.
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