Evolution of Binary Compact Objects That Merge

  title={Evolution of Binary Compact Objects That Merge},
  author={Hans Albrecht Bethe and G. E. Brown},
  journal={The Astrophysical Journal},
  pages={780 - 789}
Beginning from massive binaries in the Galaxy, we evolve black hole-neutron star (BH-NS) binaries and binary neutron stars, such as the Hulse-Taylor system PSR 1913+16. The new point in our evolution is a quantitative calculation of the accretion of matter by a neutron star in a common-envelope evolution that sends it into a black hole. We calculate the mass of the latter to be ~2.4 M☉. The black hole fate of the first neutron star can only be avoided if the neutron star does not go through… 

Contribution of High-Mass Black Holes to Mergers of Compact Binaries

We consider the merging of compact binaries consisting of a high-mass black hole and a neutron star. From stellar evolutionary calculations that include mass loss, we estimate that a zero-age main

Evolution and merging of binaries with compact objects

The Evolution of Compact Binary Star Systems

The formation and evolution of compact binary stars consisting of white dwarfs, neutron stars, and black holes are reviewed, including their role as progenitors of cosmologically-important thermonuclear SN Ia and AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

Black Hole-Neutron Star Mergers as Central Engines of Gamma-Ray Bursts

Hydrodynamic simulations of the merger of stellar mass black hole-neutron star binaries are compared with mergers of binary neutron stars and the use of a physical nuclear equation of state allows us to include the effects of neutrino emission.

The Evolution of Compact Binary Star Systems

Major uncertainties in the current understanding of properties of NSs and BHs most relevant to the GW studies are discussed, including the treatment of the natal kicks which compact stellar remnants acquire during the core collapse of massive stars and the common envelope phase of binary evolution.

Pre-supernova evolution, compact-object masses, and explosion properties of stripped binary stars

The era of large transient surveys, gravitational-wave observatories, and multi-messenger astronomy has opened up new possibilities for our understanding of the evolution and final fate of massive

Mergers of Neutron Star-Black Hole Binaries with Small Mass Ratios: Nucleosynthesis, Gamma-Ray Bursts, and Electromagnetic Transients

We discuss simulations of the coalescence of black hole-neutron star binary systems with black hole masses between 14 and 20 M☉. The calculations use a three-dimensional smoothed particle


This paper models the orbital inspiral of a neutron star (NS) through the envelope of its giant-branch companion during a common envelope (CE) episode. These CE episodes are necessary to produce

Mergers of Binary Compact Objects

We work out the effects of hypercritical accretion, which transfers mass from the secondary to the primary (older) neutron star (NS) in a binary, showing that such accretion would cause the mass of



The evolution of relativistic binary pulsars

On the galactic and cosmic merger rate of double neutron stars

Previous calculations of the merging rate of double neutron star systems similar to the Hulse-Taylor binary pulsar B1913 + 16 have assumed lifetimes based on the sum of the radio pulsar spin-down age

The Rate of Neutron Star Binary Mergers in the Universe: Minimal Predictions for Gravity Wave Detectors

Of the many sources which gravitational wave observatories might see, merging neutron star binaries are the most predictable. Their waveforms at the observable frequencies are easy to calculate. And

Scenarios for the formation of binary and millisecond pulsars – A critical assessment

The evolution of high-and low-mass X-ray binaries (HMXB and LMXB) into different types of binary radio pulsars, the ‘high-mass binary pulsars’(HMBP) and ‘low-mass binary pulsars’ (LMBP) is discussed.

Supernova Explosions, Black Holes and Nucleon Stars

In the collapse of large stars matter is formed at supranuclear densities. At a density ρ ∼ 3ρ0, where ρ0 is the nuclear matter density, K−‐mesons replace electrons, and go into a Bose condensate.

Presupernova evolution of massive stars.

Population I stars of 15 M/sub sun/ and 25 M/sub sun/ have been evolved from the zero-age main sequence through iron core collapse utilizing a numerical model that incorporates both implicit


The characteristics of many close, evolved binaries can be understood most easily if there exists some agency that can abstract angular momentum or mass, or both, from the precursor system. Close

Neutron Star Population Dynamics. I. Millisecond Pulsars

We study the field millisecond pulsar (MSP) population to infer its intrinsic distribution in spin period and luminosity and to determine its spatial distribution within the Galaxy. Our likelihood

Double-core evolution. II - Two-dimensional hydrodynamic effects

The evolution of a double-core configuration consisting of a 16 M/sub sun/ supergiant and an immersed 1 M/sub sun/ neutron star is investigated with a two-dimensional numerical hydrodynamic