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Table 1

Summary of progenitor and ejecta properties.

Model Mi Mf L Teff R R95 Menv Mr Me Ekin V 99,H V 99,He V 99,Ni H He 56Ni0 XH,s
[M] [M] [L] [K] [R] [R] [M] [M] [M] [B] [km s−1] [km s−1] [km s−1] [M] [M] [M]
H_R5 16 4.13 9.8(4) 4.6(4) 5.0 0.87 0.0 1.55 2.58 1.26 1.75(3) 6.36(3) 0.00 1.42 0.061 0.0
H_R61 16 4.46 61.1 0.80 5.0(−4) 1.60 2.86 1.23 1.19(4) 3.87(3) 5.92(3) 4.10(−3) 1.51 0.059 0.062
H_R152 16 4.57 7.4(4) 7.7(3) 152.2 0.77 1.1(−3) 1.60 2.97 1.22 1.22(4) 3.59(3) 5.74(3) 3.72(−3) 1.50 0.049 0.059
H_R228 16 4.57 1.0(5) 6.8(3) 228.4 0.76 2.2(−3) 1.70 2.87 1.27 1.26(4) 3.64(3) 5.95(3) 4.09(−3) 1.51 0.059 0.066
H_R385 16 4.67 1.0(5) 5.3(3) 385.3 0.75 1.2(−2) 1.70 2.97 1.21 1.23(4) 3.60(3) 5.82(3) 8.38(−3) 1.53 0.049 0.12
H_R601 16 5.14 1.2(5) 4.3(3) 601.5 0.77 0.10 1.65 3.49 1.20 8.78(3) 3.85(3) 4.53(3) 5.17(−2) 1.70 0.058 0.38

He_R11 12 2.67 11.0 3.4 0.0 0.98 1.02 5.00(3) 0.0 0.93 0.0 0.0
He_R173 12 2.73 3.0(4) 5.8(3) 173.0 5.2 0.074 1.04 0.97 5.00(3) 0.0 0.99 0.0 0.0

Notes. Mi and Mf are the initial and final mass; R is the final surface radius; R95 corresponds to the radius that contains 95% of the star mass in the progenitor model; Menv is the mass of the tenuous envelope (corresponding to envelope material with a mass density lower than 10−5 g cm−3); Mr is the remnant mass; Me and Ekin are the ejecta mass and kinetic energy. The following three columns give the ejecta velocity that bounds 99% of the corresponding species total mass. The integration is done inwards in velocity space for H and He, and outwards for 56Ni. The next three columns give the total mass of H, He, and 56Ni initially (56Ni0). The last column gives the surface mass fraction of H. All models were evolved all the way to iron core collapse except models He_R11 and He_R173 for which the progenitor evolution was stopped at the onset of core neon burning. Model He_R11 is the same as He_R173 except that it was trimmed of the extended low-density envelope prior to explosion (it is used for the comparative study of shock behaviour presented in Sect. 4). All H-rich models are characterised by a low level of mixing. The H-deficient models He_R173 and He_R11 have no 56Ni. H-rich models stem from the explosion of the primary in a binary system originally composed of a 16.0 and a 14.0 M component. The H-deficient models result from the evolution of 2.8 M star on the zero age He main sequence; this star would have had a mass of ~12 M on the zero age H main sequence. Model H_R385 went through Case B mass transfer, and all other models through Case BB mass transfer.

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