Journal ArticleDOI
The evolution of massive close binaries: V: Systems containing primaries with masses between 10M ⊙ and 15M ⊙
J. P. De Greve,C. De Loore +1 more
TLDR
In this article, the final state of binary systems with initial massesM1i=10M to 15M was derived from the mass of their C/O-cores, and the possibility of a second stage of mass transfer towards the secondary was considered.Abstract:
The final state of the primaries of binary systems with initial massesM1i=10M⊙ to 15M⊙ is derived from the mass of their C/O-cores. The possibility of a second stage of mass transfer towards the secondary is considered. It turns out that the critical mass for the bifurcation is about 14M⊙: stars with larger masses in this range are the progenitors of neutron stars, while the lower mass stars are the ancestors of white dwarfs.read more
Citations
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Ultra-stripped supernovae: progenitors and fate
TL;DR: In this article, a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe) was presented, in which the binary parameter space leading to electron capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, was examined and the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic.
Journal ArticleDOI
A New Class of High-Mass X-Ray Binaries: Implications for Core Collapse and Neutron Star Recoil
TL;DR: In this article, the authors investigate a class of high-mass X-ray binaries (HMXBs) with long orbital periods (Porb > 30 days) and low eccentricities (e 0.2) and develop a self-consistent phenomenological picture wherein the neutron stars born in the observed wide HMXBs receive only a small kick (50 km s-1).
Journal ArticleDOI
The Galactic Population of Low- and Intermediate-Mass X-Ray Binaries
TL;DR: In this paper, the formation probability of low and intermediate-mass X-ray binaries (L/IMXBs) with initial donor masses of 1.5-4 M was studied.
Journal ArticleDOI
A Comprehensive Study of Neutron Star Retention in Globular Clusters
TL;DR: In this article, a population study of the formation and evolution of massive binary systems was conducted, and the authors used a Monte Carlo approach to generate and evolve an ensemble of massive primordial binaries.
Journal ArticleDOI
Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations I: Black Hole - Neutron Star Mergers
Floor S. Broekgaarden,Edo Berger,Coenraad J. Neijssel,Coenraad J. Neijssel,Alejandro Vigna-Gómez,Debatri Chattopadhyay,S. P. Stevenson,Martyna Chruslinska,Stephen Justham,Selma E. de Mink,Selma E. de Mink,Selma E. de Mink,Ilya Mandel,Ilya Mandel +13 more
TL;DR: In this paper, the authors present binary population synthesis of isolated BHNS systems in order to predict their merger rate and characteristics for ground-based GW observatories, and explore key uncertainties in their assumptions about massive binary star evolution (e.g., mass transfer, common-envelope evolution, supernovae).
References
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Journal ArticleDOI
Evolutionary Processes in Close Binary Systems
TL;DR: According to as mentioned in this paper, 50% o f the main-sequence stars are binary and 60% of the early-type stars are double with mass ratio larger than 0.2.
Journal ArticleDOI
Evolution of massive close binaries and formation of neutron stars and black holes
TL;DR: In this article, the influence of UFI-neutrino emission on the evolution of close binaries was investigated, assuming both the Ledoux and Schwarzschild stability criteria for semiconvection.
Journal ArticleDOI
A calculation of a white dwarf supernova
Carl J. Hansen,J. C. Wheeler +1 more
TL;DR: In this article, a hydrodynamic calculation of a 1.42M⊙ white dwarf supernova is described, where the collapse is initiated by electron capture and the subsequent nuclear detonation of C12 at high densities is sufficient to disperse all the material of the star.
Journal ArticleDOI
Evolution of Massive Close Binaries. I: The X-Ray Binary Stage
C. De Loore,J. P. De Greve +1 more
TL;DR: In this article, the evolution of binary systems consisting of a 20M⊙ primary and secondaries of respectively 14, 10, 8 and 6M ⊙ was computed from the Main Sequence stage through the X-ray phase, until the second mass transfer phase.