Abstract

Contributed Talk - Splinter MassiveStars

Tuesday, 10 September 2024, 14:00   (S23)

Interacting supernovae from wide massive binaries

A. Ercolino (1), H. Jin (1), N. Langer (1,2), L. Dessart (3)
(1) Argelander Institut für Astronomie, Universität Bonn, (2) Max-Planck Institut für Radioastronomie, (3) Institut d’Astrophysique de Paris CNRS-Sorbonne Université

The light curves and spectra of many Type I and Type II supernovae (SNe) are heavily influenced by the progenitors properties and the interaction of the SN ejecta with circumstellar material (CSM) surrounding the progenitor star. The observed diversity hints at the fact that many progenitors have undergone some level of stripping and CSM pollution shortly before the explosion. The presence of a binary companion and the onset of stable or unstable mass transfer offers a mechanism which can give rise to this diversity. In this talk, we present a set of detailed massive evolutionary models in which the donor star, a Red Supergiant (RSG) is in a wide orbit around a main-sequence companion, and undergoes stable mass transfer or common envelope evolution in the later stages of evolution, up until the moment of core collapse. Their resulting SN types range from Type IIP to H-deficient IIb and H-free Ib. In some models, the material lost during the pre-SN transfer may form a dense CSM which surrounds the system by the time of core collapse which can give rise to significant interaction effects in the SN light-curve and spectra. If the mass transfer turns unstable, the progenitor may show significant variability in the last few thousand years prior to core collapse, and the following SN will likely exhibit strong interaction effects. We also address and discuss some significant features of RSGs that may impact our results, from the presence of pulsations and extended atmospheres, to the initial eccentricity of the orbit.