Displacement of X-ray binaries: constraints on the natal kicks

Zuo, Zhao-Yu

doi:10.1051/0004-6361/201424604

Cited by 10 publications

(8 citation statements)

References 49 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It has been widely accepted that the neutron stars get large natal kicks when they form via core-collapse SNe (e.g., Cordes et al 1993;Lyne & Lorimer 1994;Wang et al 2006;Zuo 2015). However, the magnitudes of natal kicks imparted to BHs is still a matter of debate.…”

Section: Natal Kick Distribution For Bhsmentioning

confidence: 99%

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

Chatterjee

Rodriguez

Rasio

2017

ApJ

127

145

View full text Add to dashboard Cite

Recent N-body simulations predict that large numbers of stellar black holes (BHs) could at present remain bound to globular clusters (GCs), and merging BH-BH binaries are produced dynamically in significant numbers. We systematically vary "standard" assumptions made by numerical simulations related to, e.g., BH formation, stellar winds, binary properties of high-mass stars, and IMF within existing uncertainties, and study the effects on the evolution of the structural properties of GCs, and the BHs in GCs. We find that variations in initial assumptions can set otherwise identical initial clusters on completely different evolutionary paths, significantly affecting their present observable properties, or even affecting the cluster's very survival to the present. However, these changes usually do not affect the numbers or properties of local BH-BH mergers. The only exception is that variations in the assumed winds and IMF can change the masses and numbers of local BH-BH mergers, respectively. All other variations (e.g., in initial binary properties and binary fraction) leave the masses and numbers of locally merging BH-BH binaries largely unchanged. This is in contrast to binary population synthesis models for the field, where results are very sensitive to many uncertain parameters in the initial binary properties and binary stellar-evolution physics. Weak winds are required for producing GW150914-like mergers from GCs at low redshifts. LVT151012 can be produced in GCs modeled both with strong and weak winds. GW151226 is lower-mass than typical mergers from GCs modeled with weak winds, but is similar to mergers from GCs modeled with strong winds.

show abstract

Section: Natal Kick Distribution For Bhsmentioning

confidence: 99%

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

Chatterjee

Rodriguez

Rasio

2017

ApJ

127

145

View full text Add to dashboard Cite

show abstract

“…Also, whether or not black holes that are formed in core-collapse supernova receive a kick is still under debate (e.g. Gualandris et al, 2005;Repetto and Nelemans, 2015;Repetto et al, 2012;Wong et al, 2014;Zuo, 2015).…”

Section: Supernova Explosionsmentioning

confidence: 99%

The evolution of hierarchical triple star-systems

2016

View full text Add to dashboard Cite

Field stars are frequently formed in pairs, and many of these binaries are part of triples or even higher-order systems. Even though, the principles of single stellar evolution and binary evolution, have been accepted for a long time, the long-term evolution of stellar triples is poorly understood. The presence of a third star in an orbit around a binary system can significantly alter the evolution of those stars and the binary system. The rich dynamical behaviour in three-body systems can give rise to Lidov-Kozai cycles, in which the eccentricity of the inner orbit and the inclination between the inner and outer orbit vary periodically. In turn, this can lead to an enhancement of tidal effects (tidal friction), gravitational-wave emission and stellar interactions such as mass transfer and collisions. The lack of a self-consistent treatment of triple evolution, including both three-body dynamics as well as stellar evolution, hinders the systematic study and general understanding of the long-term evolution of triple systems. In this paper, we aim to address some of these hiatus, by discussing the dominant physical processes of hierarchical triple evolution, and presenting heuristic recipes for these processes. To improve our understanding on hierarchical stellar triples, these descriptions are implemented in a public source code TrES, which combines three-body dynamics (based on the secular approach) with stellar evolution and their mutual influences. Note that modelling through a phase of stable mass transfer in an eccentric orbit is currently not implemented in TrES, but can be implemented with the appropriate methodology at a later stage.

show abstract

“…current position and its birth location. At the same time, the SN kick affects the binary's orbit, and a correlation should exist between binary parameters and the distance an HMXB travels from its birth site (Zuo & Li 2010;Zuo 2015). These models use traditional BPS to reproduce general characteristics of the HMXB population, such as the observation that HMXBs with higher X-ray luminosities tend to be found closer to star forming regions than systems with lower X-ray luminosities (Kaaret et al 2004).…”

Section: A New Approach In Bpsmentioning

confidence: 99%

“…Sepinsky et al (2005) demonstrated that the distance traveled by a population of HMXBs depends on the binary physics assumed. Later, Zuo & Li (2010) and Zuo (2015) went further by correlating this travel distance with orbital period and X-ray luminosity. A more in-depth study of HMXB travel distances, including either the formation of individual systems or spatially resolved SFHs, is lacking; however, it is the next step in modeling X-ray binary populations given the increasing availability of spatially resolved SFHs.…”

Section: Introductionmentioning

confidence: 96%

dart_board: Binary Population Synthesis with Markov Chain Monte Carlo

Andrews,

Zezas,

Fragos

2017

Preprint

View full text Add to dashboard Cite

By employing Monte Carlo random sampling, traditional binary population synthesis (BPS) offers a substantial improvement in efficiency over brute force, grid-based studies. Even so, BPS models typically require a large number of simulation realizations, a computationally expensive endeavor, to generate statistically robust results. Recent advances in statistical methods have led us to revisit the traditional approach to BPS. In this work we describe our publicly available code dart board which combines rapid binary evolution codes, typically used in traditional BPS, with modern Markov chain Monte Carlo methods. dart board takes a novel approach that treats the initial binary parameters and the supernova kick vector as model parameters. This formulation has several advantages, including the ability to model either populations of systems or individual binaries, the natural inclusion of observational uncertainties, and the flexible addition of new constraints which are problematic to include using traditional BPS. After testing our code with mock systems, we demonstrate the flexibility of dart board by applying it to three examples: (i) a generic population of high mass X-ray binaries (HMXBs), (ii) the population of HMXBs in the Large Magellanic Cloud (LMC) in which the spatially resolved star formation history is used as a prior, and (iii) one particular HMXB in the LMC, Swift J0513.4−6547, in which we include observations of the system's component masses and orbital period. Although this work focuses on HMXBs, dart board can be applied to a variety of stellar binaries including the recent detections by gravitational wave observatories of merging compact object binaries.

show abstract

Displacement of X-ray binaries: constraints on the natal kicks

Cited by 10 publications

References 49 publications

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

Binary Black Holes in Dense Star Clusters: Exploring the Theoretical Uncertainties

The evolution of hierarchical triple star-systems

dart_board: Binary Population Synthesis with Markov Chain Monte Carlo

Contact Info

Product

Resources

About