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Updated: Mar 28, 2026

Setting Limits on Supersymmetry Using Simplified Models

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Published on: November 15, 2013

Neutron-Star-Black-Hole Binaries Produced by Binary-Driven Hypernovae.

Chris L Fryer¹, F G Oliveira^2,3,4, J A Rueda^2,3,4,5

¹CCS-2, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA.

Physical Review Letters

|December 20, 2015

Summary

This summary is machine-generated.

Binary-driven hypernovae (BdHNe) create neutron-star black-hole binaries from collapsing stars. These systems remain bound after supernovae, potentially explaining gravitational waves and ultrashort gamma-ray bursts.

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Area of Science:

Astrophysics
Stellar Evolution
High-Energy Astrophysics

Background:

Energetic long gamma-ray bursts (GRBs) and Type Ic supernovae are linked to binary-driven hypernovae (BdHNe).
BdHNe originate from tight binaries of carbon-oxygen (CO) cores and neutron-star (NS) companions, a type of ultrastripped binary.
The NS companion accretes matter during CO core collapse, leading to black hole (BH) formation and GRB emission.

Purpose of the Study:

To investigate the unique binary evolution during supernovae explosions.
To understand the formation and fate of neutron-star black-hole (NS-BH) binaries in the BdHNe scenario.
To assess the contribution of these systems to compact merger rates and gravitational wave events.

Main Methods:

Analysis of binary evolution under hypercritical accretion during supernova explosions.
Modeling the impact of non-instantaneous mass ejection on binary dynamics.
Investigating the role of bow shock interactions in angular momentum transfer and orbital braking.

Main Results:

The hypercritical accretion and non-instantaneous mass ejection significantly alter binary evolution compared to standard compact binary models.
Bow shock formation during accretion brakes the orbit, ensuring binary systems remain bound even with substantial mass loss.
BdHNe produce a novel class of NS-BH binaries not accounted for in current population synthesis.

Conclusions:

BdHNe provide a plausible mechanism for producing energetic GRBs and associated Type Ic supernovae.
The high binding fraction of resulting NS-BH binaries suggests they are significant contributors to the compact merger rate.
These systems may be progenitors of gravitational wave events and a new class of ultrashort GRBs.