Volume 614, June 2018
|Number of page(s)||11|
|Section||Stellar structure and evolution|
|Published online||20 June 2018|
Case A and B evolution towards electron capture supernova
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB),
2 Max-Planck-Institut für Astrophysik, Karl Schwarzschild Str. 1, 85741 Garching, Germany
Accepted: 5 March 2018
Context. Most super-asymptotic giant branch (SAGB) stars are expected to end their life as oxygen–neon white dwarfs rather than electron capture supernovae (ECSN). The reason is ascribed to the ability of the second dredge-up to significantly reduce the mass of the He core and of the efficient AGB winds to remove the stellar envelope before the degenerate core reaches the critical mass for the activation of electron capture reactions.
Aims. In this study, we investigate the formation of ECSN through case A and case B mass transfer. In these scenarios, when Roche lobe overflow stops, the primary has become a helium star. With a small envelope left, the second dredge-up is prevented, potentially opening new paths to ECSN.
Methods. We compute binary models using our stellar evolution code BINSTAR. We consider three different secondary masses of 8, 9, and 10 M⊙ and explore the parameter space, varying the companion mass, orbital period, and input physics.
Results. Assuming conservative mass transfer, with our choice of secondary masses all case A systems enter contact either during the main sequence or as a consequence of reversed mass transfer when the secondary overtakes its companion during core helium burning. Case B systems are able to produce ECSN progenitors in a relatively small range of periods (3 ≲ P(d) ≤ 30) and primary masses (10.9 ≤ M∕M⊙≤ 11.5). Changing the companion mass has little impact on the primary’s fate as long as the mass ratio M1∕M2 remains less than 1.4–1.5, above which evolution to contact becomes unavoidable. We also find that allowing for systemic mass loss substantially increases the period interval over which ECSN can occur. This change in the binary physics does not however affect the primary mass range. We finally stress that the formation of ECSN progenitors through case A and B mass transfer is very sensitive to adopted binary and stellar physics.
Conclusions. Close binaries provide additional channels for ECSN but the parameter space is rather constrained likely making ECSN a rare event.
Key words: binaries / close / white dwarfs / supernovae: general
© ESO 2018
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