The formation of the stripped envelope type II b Supernova progenitors: Rotation, Metallicity and Overshooting

TL;DR

This paper investigates how rotation, metallicity, overshooting, and orbital period influence the formation of Type IIb supernova progenitors, emphasizing binary interactions and physical parameters' roles in progenitor characteristics.

Contribution

It provides a detailed analysis of the effects of physical factors and binary parameters on the formation and properties of Type IIb supernova progenitors, highlighting the importance of initial orbital period.

Findings

Binary systems are the main channel for Type IIb progenitors below 20 M_sun.

Progenitor type depends on initial orbital period, affecting supergiant classification.

Low metallicity leads to smaller hydrogen envelopes and radii.

Abstract

Type IIb supernovae are believed to originate from core-collapse progenitors having kept only a very thin hydrogen envelope. We aim to explore how some physical factors, such as rotation, metallicity, overshooting, and the initial orbital period in binaries, significantly affect the Roche lobe overflow and the formation of type IIb supernovae. It is found that binaries are the main channel that capable of producing type typeIIb supernovae progenitors in the mass range for initial masses below 20 $M_{\odot}$. The formation of type IIb supernova progenitors is extremely sensitive to the initial orbital period. A less massive hydrogen indicates smaller radius and a higher effective temperatures, and vice versa. Binary systems with initial periods between 300 and 720 days produce type IIb progenitors that are a red supergiant. Those with an initial period between 50 and 300 days produce yellow supergiant progenitors and those with initial periods shorter than 50 days, blue supergiant progenitors. Both rapid rotation and larger overshooting can enlarge the carbon-oxygen core mass and lead to higher core temperature and lower central density at the pre-collapse phase. They are also beneficial to surface nitrogen enrichment but restrict the efficiency of the first dredge-up. SN IIb progenitors with low metallicity have smaller hydrogen envelope masses and radii than the high metallicity counterparts. Ultra-stripped binary models have systematically higher core mass fraction $\rm ^{12}C$ left, which has important influence on the compactness of type IIb progenitors.