Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014

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Volume 542 (June 2012)

A&A, 542 (2012) A29

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Table 3

WR- and SN-type ratios deduced from our models, and comparison with previous works and observations.

Notes. Remark: note that even though it seems that the non-rotating models better reproduce the various ratios of the WR subtypes, they are worse at reproducing the WR/O ratio. It is important to fit all these ratios simultaneously.

⁽¹⁾

Considering that the surface He abundance limit between WNL and WNE is 0.1 instead of 10^-5.

⁽²⁾

The maximum He mass ejected allowed to be still considered as a Type Ic SN is 0.4–0.6–0.8 M_⊙ in the low–medium–high SN Ic case, respectively (see Georgy et al. 2009).

⁽³⁾

Assuming that the formation of a BH during the collapse has no influence on the SN explosion.

⁽⁴⁾

Assuming that the formation of a BH during the collapse prevents a bright SN explosion.

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