Table 1
Summary of properties of the heracles simulations and their initial conditions.
Model | t rise | Δtmax | L bol,max | f drop |
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R ⋆ | M ejecta | E kin | H ρ | n ρ | Ṁ | M ext | τ ext | |
[d] | [d] | [erg s-1] | [erg] | [R⊙] | [M⊙] | [erg] | [R⋆] | [M⊙ yr-1] | [M⊙] | |||||
|
||||||||||||||
r1w1 | 0.018 | 0.062 | 7.38(44) | 146.2 | 6.65(48) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 1(–6) | 2.75(–3) | 160 | |
r1w2 | 0.019 | 0.068 | 6.71(44) | 130.4 | 6.68(48) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 1(–5) | 2.79(–3) | 160 | |
r1w3 | 0.025 | 0.15 | 3.30(44) | 57.4 | 6.66(48) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 1(–4) | 3.05(–3) | 160 | |
r1w4 | 0.186 | 5.11 | 6.53(43) | 5.61 | 8.67(48) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 1(–3) | 5.59(–3) | 169 | |
r1w1h | 0.30 | 0.755 | 4.16(44) | 11.98 | 2.10(49) | 501 | 12.52 | 1.35(51) | 0.3 | 12 | 1(–6) | 1.62(–1) | 4780 | |
r1w5h | 0.21 | 1.03 | 1.79(44) | 8.72 | 1.10(49) | 501 | 12.52 | 1.35(51) | 0.1 | ... | 3(–3) | 3.57(–2) | 1600 | |
r1w5r | 0.53 | 2.36 | 6.25(43) | 1.74 | 9.48(48) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 5(–3) | 1.02(–2) | 353 | |
r1w6 | 1.94 | 7.00 | 5.24(43) | 2.02 | 1.99(49) | 501 | 12.52 | 1.35(51) | 0.01 | ... | 1(–2) | 3.04(–2) | 246 | |
r2w1 | 0.081 | 0.179 | 8.03(44) | 84.91 | 1.44(49) | 1107 | 12.57 | 1.24(51) | 0.01 | ... | 1(–6) | 6.14(–2) | 956 |
Notes. It takes trise for the recorded luminosity to rise from 5 × 108 L⊙ to Lbol,max. The parameter Δtmax is the time during which Lbol remains above a tenth of Lbol,max; fdrop is the factor by which Lbol decreases in one day after the time of maximum; gives the time integrated bolometric luminosity from first detection until 15 d later; R⋆ is the progenitor radius, which corresponds to the RSG surface in the mesa model; Mejecta and Ekin are the ejecta mass and kinetic energy (without the atmosphere/wind material); Hρ is the atmospheric scale height in the intermediate region between R⋆ and the base of the wind; and nρ is the exponent of the power law joining this atmosphere and the base of the wind. The next column gives the wind mass loss rate within 2−5 × 1014 cm; beyond this radius the wind mass loss rate is always set to 10-6 M⊙ yr-1. The subscript “ext” refers to the external material located beyond R⋆. Its optical depth is below unity before shock breakout (because of its low original temperature, typically below the RSG effective temperature of ~3000 K). Here, we give its optical depth for post-shock breakout conditions, i.e., when H and He are fully ionized (κ = 0.34 cm2 g-1). Numbers in parenthesis represent powers of ten.
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