Massive star evolution: luminous blue variables as unexpected supernova progenitors

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Table 1

Properties of the SN progenitors from rotating models at solar metalicity, which have an LBV spectrum and explode as SN II-b / II-n.

M_ini

M_prog.^a

Age^a

L_⋆^a

T_⋆^a^b

T_eff^c

R_⋆^a^b

R_phot^c

Ṁ^a

v_∞

M_V

B − V

He (surface)

(M_⊙)

(Myr)

(10⁵ L_⊙)

(K)

(R_⊙)

(M_⊙ yr^-1)

(km s^-1)

(mag)

(mass fraction)

20.0

7.1

10.5

1.9

20 355

19 540

35.3

38.1

1.2 × 10^-5

272

−6.8

−0.14

0.74

25.0

9.6

8.6

3.2

25 790

20 000

28.4

47.0

4.6 × 10^-5

326

−7.2

−0.11

0.92

Notes.

^(a)

From Ekström et al. (2012).

^(b)

Defined here as the temperature (radius) of the last layer of the stellar envelope.

^(c)

Defined here as the temperature (radius) of the layer where the Rosseland optical depth is equal to 2/3.

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