Possible Signatures of Ejecta-Companion Interaction in iPTF 13bvn

Abstract

We investigate the possible effects of the supernova ejecta hitting the companion star in iPTF 13bvn, focusing on the observable features when it becomes visible. iPTF 13bvn is a type Ib supernova that may become the first case that its progenitor is identified as a binary by near future observations. According to calculations by Bersten et al. (2014), the progenitor should have a mass $\approx 3.5M_{\odot }$ to reproduce the supernova light curve, and such compact stars could only be produced via binary evolution. This is one of the reasons that we expect the progenitor to be a binary, but it should be confirmed by observing the remaining companion after the supernova. Their evolutionary calculations suggest that the companion star will be an overluminous OB star at the moment of supernova. With a combination of hydrodynamical and evolutionary simulations, we find that the secondary star will be heated by the supernova ejecta and expand to have larger luminosities and lower surface effective temperatures. The star will look rather like a red super giant, and this should be taken into account when searching for the companion star in the supernova ejecta in future observations.

few corrections made, published in ApJ

References in corpus (5)

• Modules for Experiments in Stellar Astrophysics (MESA)
• iPTF13bvn: The First Evidence of a Binary Progenitor for a Type Ib Supernova
• Possible binary progenitors for the type Ib supernova iPTF13bvn
• Optical observations of the fast declining type Ib supernova iPTF13bvn
• The Outcome of Supernovae in Massive Binaries; Removed Mass, and its Separation Dependence

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• Formation Scenario of the Progenitor of iPTF13bvn Revisited
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