On the Neutron Star-Black Hole Binaries Produced by Binary-driven-Hypernovae

TL;DR

This paper explores the formation of neutron star-black hole binaries through binary-driven hypernovae, highlighting their unique evolution, high bound retention rate, and potential significance for gravitational wave sources.

Contribution

It introduces a new class of NS-BH binaries formed via BdHNe, differing from traditional models by accounting for hypercritical accretion and non-instantaneous mass ejection effects.

Findings

Nearly 100% of these binaries remain bound after explosion.

They may significantly contribute to the gravitational wave merger rate.

These systems could produce a new class of ultrashort GRBs.

Abstract

Binary-driven-hypernovae (BdHNe) within the induced gravitational collapse (IGC) paradigm have been introduced to explain energetic ($E_{\rm iso}\gtrsim 10^{52}$~erg), long gamma-ray bursts (GRBs) associated with type Ic supernovae (SNe). The progenitor is a tight binary composed of a carbon-oxygen (CO) core and a neutron star (NS) companion, a subclass of the newly proposed "ultra-stripped" binaries. The CO-NS short-period orbit causes the NS to accrete appriciable matter from the SN ejecta when the CO core collapses, ultimately causing it to collapse to a black hole (BH) and producing a GRB. These tight binaries evolve through the SN explosion very differently than compact binaries studied in population synthesis calculations. First, the hypercritical accretion onto the NS companion alters both the mass and momentum of the binary. Second, because the explosion timescale is on par with the orbital period, the mass ejection can not be assumed to be instantaneous. This dramatically affects the post-SN fate of the binary. Finally, the bow shock created as the accreting NS plows through the SN ejecta transfers angular momentum, braking the orbit. These systems remain bound even if a large fraction of the binary mass is lost in the explosion (well above the canonical 50\% limit), and even large kicks are unlikely to unbind the system. Indeed, BdHNe produce a new family of NS-BH binaries unaccounted for in current population synthesis analyses and, although they may be rare, the fact that nearly 100\% remain bound implies they may play an important role in the compact merger rate, important for gravitational waves (GWs) that, in turn, can produce a new class of ultrashort GRBs.