Evolution of binary stars and the effect of tides on binary populations

By J. Hurley, C. Tout, O. Pols. 2002

1,440 citations recorded by the source corpus.

We present a rapid binary-evolution algorithm that enables modelling of even the most complex binary systems. In addition to all aspects of single-star evolution, features such as mass transfer, mass accretion, common-envelope evolution, collisions, supernova kicks and angular momentum loss mechanisms are included. In particular, circularization and synchronization of the orbit by tidal interactions are calculated for convective, radiative and degenerate damping mechanisms. We use this algorithm to study the formation and evolution of various binary systems. We also investigate the effect that tidal friction has on the outcome of binary evolution. Using the rapid binary code, we generate a series of large binary populations and evaluate the formation rate of interesting individual species and events. By comparing the results for populations with and without tidal friction, we quantify the hitherto ignored systematic effect of tides and show that modelling of tidal evolution in binary systems is necessary in order to draw accurate conclusions from population synthesis work. Tidal synchronism is important but, because orbits generally circularize before Roche lobe overflow, the outcome of the interactions of systems with the same semilatus rectum is almost independent of eccentricity. It is not necessary to include a distribution of eccentricities in population synthesis of interacting binaries; however, the initial separations should be distributed according to the observed distribution of semilatera recta rather than periods or semimajor axes.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bf6972006e039ce4258feb010df516d66cdc3f89

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In Astronomy and Astrophysics

1. Michela Mapelli
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Citations in the corpus

• COSMIC Variance in Binary Population Synthesis (2019, methodology): “As a fiducial model for critical mass ratios, we choose the standard model reported in Hurley et al. (2002) which does not differentiate between models for degenerate and non-degenerate accretors.”
• Detached white dwarf main-sequence star binaries (2004, methodology): “The code uses the single star evolution formulae derived by Hurley et al. (2000) and follows the main steps of the binary evolution scheme outlined by Hurley et al. (2002).”
• MERGING BLACK HOLE BINARIES IN GALACTIC NUCLEI: IMPLICATIONS FOR ADVANCED-LIGO DETECTIONS (2016, methodology): “These authors used the stellar evolution code BSE (Hurley et al. 2002, 2007) improved with the stellar remnant prescription from Kiel and Hurley (2009) and Chatterjee et al. (2010).”
• The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “Our BHBs were generated by evolving isolated stellar binaries with a new version of the BSE code (Hurley et al. 2002), which includes up-to-date recipes for stellar evolution and stellar winds (Vink et al. 2011; Chen et al. 2015).”
• The effect of the metallicity-specific star formation history on double compact object mergers (2019, background): “We evaluate dynamical instability by comparing the radial response of the Roche lobe to mass transfer dlog (RL)/dlog (m) against the response of the stellar radius to mass transfer dlog (R∗)/dlog (m) (Paczyński & Sienkiewicz 1972; Hjellming & Webbink 1987; Soberman, Phinney & van den Heuvel 1997).”
• Merging black holes in young star clusters (2019, methodology): “In its original version, NBODY6++GPU is coupled with the population synthesis code BSE (Hurley et al. 2000, 2002).”
• Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, background): “…computational efficiency is a set of simplifications; for example, stellar structure is not generally evolved directly, but relies on a set of models such as those provided by Hurley et al. (2000, 2002), which in turn rely on one original grid of non-rotating stellar models (Pols et al. 1998).”
• Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, methodology): “(12) For the CE phase we adopted the same formalism used by Hurley et al. (2002) and described in detail in Ivanova et al. (2013).”
• Compact binaries in star clusters – I. Black hole binaries inside globular clusters (2009, methodology): “Stellar evolution is calculated for all stars in the cluster and thus our simulations represent a complete star cluster populations synthesis study based on the stellar evolution tracks of Hurley et al. (2000, 2002).”
• X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, methodology): “More recently, Zuo & Li (2011) studied the evolution of XRB populations in late type galaxies, using a modified version of the BSE population synthesis code (Hurley et al. 2002).”
• Intermediate - mass black holes (2003, background): “…simulations (Portegies & Zwart 2002) do not include primordial binaries, because of computational limitations (although progress is being made; see Hurley, Tout, and Pols 2002; Hurley and Shara 2002; Hut et al. 2003; Aarseth 2003), but further investigation is underway to determine the regimes of…”
• THE DYNAMICAL EVOLUTION OF STELLAR BLACK HOLES IN GLOBULAR CLUSTERS (2014, background): “Stars and binaries are evolved according to the stellar evolution fitting formulae and interacting binary evolution calculations of SSE and BSE (Hurley et al. 2000, Hurley et al. 2002).”
• Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, methodology): “Approximately one-third of these close binaries will probably merge, particularly those with smaller mass ratios and/or shorter separations (Hurley et al. 2002; Belczynski et al. 2008, §11).”
• Theoretical uncertainties of the Type Ia supernova rate (2014, methodology): “Because the core masses are determined without taking overshooting during previous evolution phases into account, a fiis made to take overshooting into consideration, based on the core masses calculated by Hurley et al. (2002) during the early-AGB (E-AGB).”