Ultra-stripped supernovae and double neutron star systems
Thomas Tauris
TL;DR
This paper discusses the evolution of close binary systems leading to ultra-stripped supernovae and their role in forming double neutron star systems, highlighting the limited ejecta mass and small neutron star kicks involved.
Contribution
It provides theoretical predictions for double neutron star systems resulting from ultra-stripped supernovae, based on Case BB Roche-lobe overflow, and compares them with observations.
Findings
Ultra-stripped supernovae have very limited ejecta mass.
Small neutron star kicks are likely in these systems.
Predictions align with some observed double neutron star systems.
Abstract
The evolution of close-orbit progenitor binaries of double neutron star (DNS) systems leads to supernova (SN) explosions of ultra-stripped stars. The amount of SN ejecta mass is very limited from such, more or less, naked metal cores with envelope masses of only 0.01-0.2 Msun. The combination of little SN ejecta mass and the associated possibility of small NS kicks is quite important for the characteristics of the resulting DNS systems left behind. Here, we discuss theoretical predictions for DNS systems, based on Case BB Roche-lobe overflow prior to ultra-stripped SNe, and briefly compare with observations.
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