Binary Population Synthesis

Han, Zhanwen; Ge, Hongwei; Chen, Xuefei; Chen, Hailiang

doi:10.1088/1674-4527/20/10/161

Cited by 78 publications

(56 citation statements)

References 124 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is consistent with findings by other studies on isolated binary evolution populations (e.g., Chruślińska et al 2018;Santoliquido et al 2021), which indicated that matching the observed NSNS rate might require higher values for 𝛼 CE and/or smaller SN natal kicks. The NSNS rates could also relatively increase by changes in the mass transfer stability prescriptions (𝜁) and envelope binding energy models (𝜆), which are not explored in our study (see Han et al 2020;Lau et al 2021, and references therein). Future observations and simulations can further constrain this.…”

Section: Comparison With Gw Mergersmentioning

confidence: 86%

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Broekgaarden,

Berger,

Stevenson

et al. 2021

Preprint

View full text Add to dashboard Cite

Making the most of the rapidly increasing population of gravitational-wave detections of black hole (BH) and neutron star (NS) mergers requires comparing observations with population synthesis predictions. In this work we investigate the combined impact from the key uncertainties in population synthesis modelling of the isolated binary evolution channel: the physical processes in massive binary-star evolution and the star formation history as a function of metallicity, 𝑍, and redshift 𝑧, S(𝑍, 𝑧). Considering these uncertainties we create 560 different publicly available model realizations and calculate the rate and distribution characteristics of detectable BHBH, BHNS, and NSNS mergers. We find that our stellar evolution and S(𝑍, 𝑧) variations can impact the predicted intrinsic and detectable merger rates by factors 10 2 -10 4 . We find that BHBH rates are dominantly impacted by S(𝑍, 𝑧) variations, NSNS rates by stellar evolution variations and BHNS rates by both. We then consider the combined impact from all uncertainties considered in this work on the detectable mass distribution shapes (chirp mass, individual masses and mass ratio). We find that the BHNS mass distributions are predominantly impacted by massive binary-star evolution changes. For BHBH and NSNS we find that both uncertainties are important. We also find that the shape of the delay time and birth metallicity distributions are typically dominated by the choice of S(𝑍, 𝑧) for BHBH, BHNS and NSNS. We identify several examples of robust features in the mass distributions predicted by all 560 models, such that we expect more than 95 percent of BHBH detections to contain a BH 8 M and have mass ratios 4. Our work demonstrates that it is essential to consider a wide range of allowed models to study double compact object merger rates and properties. Conversely, larger observed samples could allow us to decipher currently unconstrained stages of stellar and binary evolution.

show abstract

Section: Comparison With Gw Mergersmentioning

confidence: 86%

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Broekgaarden,

Berger,

Stevenson

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Here we describe the terms in this equation, which allows us to highlight the broad range of physics involved and to comment on the key uncertainties. In practice, most modern models rely on some form of population synthesis, where large numbers of stellar binaries are evolved in order to compute the yield, frequently by using simplified recipes to reduce computational cost (Postnov and Yungelson 2014;Han et al 2020).…”

Section: Isolated Binary Evolution With Mass Transfermentioning

confidence: 99%

Rates of compact object coalescences

2022

View full text Add to dashboard Cite

Gravitational-wave detections are enabling measurements of the rate of coalescences of binaries composed of two compact objects—neutron stars and/or black holes. The coalescence rate of binaries containing neutron stars is further constrained by electromagnetic observations, including Galactic radio binary pulsars and short gamma-ray bursts. Meanwhile, increasingly sophisticated models of compact objects merging through a variety of evolutionary channels produce a range of theoretically predicted rates. Rapid improvements in instrument sensitivity, along with plans for new and improved surveys, make this an opportune time to summarise the existing observational and theoretical knowledge of compact-binary coalescence rates.

show abstract

“…The binary fraction of OB stars increases as the spectral type goes to early (Guo et al 2021), and O stars in cluster, associations, and runaways have binary fraction (70%) higher than those in field environment (40%; Chini et al 2012). These observational studies challenge the accepted predominance of the single star evolutionary channel and complicate the exact determination of the evolutionary status and final fates of these stars (Han et al 2020).…”

Section: Introductionmentioning

confidence: 99%

New Massive Contact Twin Binary in a Radio-quiet HII Region Associated with the M17 Complex

Yin,

Chen,

Yao

et al. 2022

Preprint

View full text Add to dashboard Cite

Early-B stars, much less energetic than O stars, may create an H II region that appears as radio-quiet. We report the identification of new early-B stars associated with the radio-quiet H II region G014.645-00.606 in the M17 complex. The ratio-quiet H II region G014.645-00.606 is adjacent to three radio-quiet WISE H II region candidates (Anderson et al. 2014). The ionizing sources of the radio-quiet H II regions are expected to later than B1V, given the sensitivity about 1 − 2 mJy of the MAGPIS 20 cm survey. The stars were first selected if their parallaxes of GAIA EDR3 match that of the 22 GHz H 2 O maser source within the same region. We used the color-magnitude diagram made from the ZTF photometric catalog to select the candidates for massive stars because the intrinsic g − r colors of massive stars change little from B-type to O-type stars. Five stars lie in the areas of the color-magnitude diagram where either reddened massive stars or evolved post-main sequence stars of lower masses are commonly found. Three of the five stars, sources 1, 2, and 3, are located at the cavities of the three IR bubbles, and extended Hα emission is detected around the three IR bubbles. We suggest that sources 1, 2, and 3 are candidates for early-B stars associated with the radio-quiet region G014.645-00.606. Particularly, source 1 is an EW type eclipsing binary with a short period of 0.825 day, while source 2 is an EA type eclipsing binary with a short period of 0.919 day. The physical parameters of the two binary systems have been derived through the PHOEBE model. Source 1 is a twin binary of two stars with T eff ≈ 23, 500 K, and source 2 contains a hotter component (T eff ≈ 20, 100 K) and a cooler one (T eff ≈ 15, 500 K). The O − C values of source 1 show a trend of decline, implying that the period of source is deceasing. Source 1 is likely a contacting early-B twin binary, for which mass transfer might cause its orbit to shrink.

show abstract

Binary Population Synthesis

Cited by 78 publications

References 124 publications

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties

Rates of compact object coalescences

New Massive Contact Twin Binary in a Radio-quiet HII Region Associated with the M17 Complex

Contact Info

Product

Resources

About