The origin of type Ib supernovae

Astronomy and Astrophysics – Astronomy

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Mass Ratios, Oxygen, Stellar Mass Ejection, Supernovae, Mass Distribution, Nickel Isotopes, Stellar Rotation

Scientific paper

A recent estimate of the oxygen mass in the type Ib supernova SN 1984L, approximately 1 solar mass, supports the hypothesis that SN Ib and SN II-b have common progenitors (stars with 15-25 solar masses), which assumes that SN Ib progenitors are binaries and that those of SN II-P are singles or wide binaries. However, observations show that Ni-56 mass in SN Ib is twice that in SN II-P. This paradox is resolved if it is considered that pre-SN Ib, as close binaries, can rotate faster than pre-SN II-P. This rotation is capable of increasing the mass of Ni-56 ejecta in SN Ib either via the effect of rotation on the dynamics of the explosion or via the formation of the more massive silicon mantle due to more effective mixing induced by the rotation at the O-burning stage. One of the consequences of the rapid rotation of pre-SN IB might be the axial symmetry of the distribution of the presupernova's chemical composition, which might produce nonsphericity of Ni-56 ejecta. It is shown that SN Ib and SN II-L cannot have common progenitors if the diversity of SN Ib is exhausted by the observational sample.

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