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Table 2

Properties of the core-collapse SN progenitor models at solar metallicity.

Mini Mprog.a Agea L⋆a T⋆a,b Teff R⋆ Rphot Ṁa υ∞ β Sp. Type SN Type
(M⊙) (M⊙) (Myr) (L⊙) (K) (K) (R⊙) (R⊙) (M⊙   yr-1) (km   s-1)
non-rotating models
9 8.8 30.3 39 401 3480 3480 547.49 547.49 9.7 × 10-7 − − K − M  I IIP
12 11.3 17.8 46 259 3556 3556 567.94 567.94 1.3 × 10-6 − − K − M  I IIP
15 13.25 12.5 79 999 3571 3571 740.91 740.91 3.2 × 10-6 − − K − M  I IIP
20 8.8 8.7 152 291 3741 3741 931.42 931.42 2.0 × 10-5 − − K − M  I IIL/b
23 7.6 7.6 195 030 4410 4410 758.29 758.29 4.4 × 10-5 − − K − M  I IIL/b
25 8.2 7.09 2.4E+05 27 116 26 330 22.20 23.49 9.7 × 10-6 694 1.0 WN11h/LBV IIL/b
32 10.9 5.81 3.7E+05 45 790 40 480 9.65 12.32 2.9 × 10-5 1200 1.0 WN7–8o Ib
40 12.7 4.97 4.8E+05 48 183 40 006 9.99 14.4 4.2 × 10-5 1291 1.0 WN7–8o Ib
50 16.53 4.34 7.4E+05 235 060 161 200 0.52 1.10 1.2 × 10-5 5000 1.0 WO1–3 Ib
60 12.4 3.97 4.8E+05 225 077 164 600 0.46 0.85 1.5 × 10-5 5000 1.0 WO1–3 Ic
85 18.5 3.40 9.0E+05 236 900 166 900 0.56 1.13 2.2 × 10-5 5000 1.0 WO1–3 Ic
120 30.7 3.00 1.8E+06 167 700 145 100 1.59 2.11 3.1 × 10-5 5000 1.0 WO1–3 Ib
rotating models, initial υrot/υcrit = 0.4
9 8.5 35.5 42 802 3528 3528 555.08 555.08 1.1 × 10-6 − − K − M  I IIP
12 10.22 20.7 72 652 3550 3550 714.24 714.24 2.7 × 10-6 − − K − M  I IIP
15 11.07 15.0 121 442 3623 3623 886.73 886.73 6.5× 10-6 − − K − M  I IIP
16.5 12.14 13.0 126 610 3645 3645 894.92 894.92 7.0× 10-6 − − K − M  I IIP
18 6.32 11.7 153 052 5382 5382 451.20 451.20 1.7× 10-5 − − G1Ia+ IIL/b
20 7.1 10.4 1.9E+05 20 355 19 540 35.30 38.11 1.2× 10-5 272 1.0 LBV IIL/b
25 9.6 8.60 3.2E+05 24 625 20 000 31.1 46.96 4.6× 10-5 326 1.0 LBV Ib
28 10.8 7.92 3.5E+05 28 882 26 823 23.68 26.26 2.6× 10-5 415 1.0 WN10-11 Ib
32 10.1 7.22 3.4E+05 181 500 154 100 0.58 0.81 1.2× 10-5 5000 1.0 WO1 Ic
40 12.2 6.17 4.4E+05 211 700 161 100 0.49 0.85 1.4× 10-5 5000 1.0 WO1–2 Ic
60 18.9 4.86 8.6E+05 247 100 174 500 0.48 1.01 2.0× 10-5 5000 1.0 WO1–3 Ic
85 26.2 4.06 1.3E+06 266 700 168 400 0.54 1.34 2.8× 10-5 5000 1.0 WO1–3 Ib
120 18.9 3.55 8.6E+05 252 800 174 500 0.48 1.01 2.0× 10-5 5000 1.0 WO1 Ic

Notes. From left to right, the columns correspond to the initial mass on the main sequence (Mini), the SN progenitor mass (Mprog.), and the age, bolometric luminosity (L⋆), temperature at the hydrostatic surface (T⋆), effective temperature (Teff), radius of the hydrostatic surface (R⋆), photospheric radius (Rphot), mass-loss rate (Ṁ), wind terminal velocity (υ∞), steepness of the velocity law (β), and spectral type at the pre-SN stage. The last column corresponds to the SN type as computed by Georgy et al. (2012). Spectral types in italic were not obtained via classification of the spectra, and thus are tentative.

(a)

From Ekström et al. (2012), except for the non-rotating 23 and 50 M⊙ and the rotating 18 and 28 M⊙ models, which were computed for this work.

(b)

This is defined here as the temperature computed by the Geneva code without the correction due to optical-depth effects of the stellar wind.

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