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Table 1

Summary of properties of the heracles simulations and their initial conditions.

Model t rise Δtmax L bol,max f drop R M ejecta E kin H ρ n ρ 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 × 108L  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 10-6M 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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