binary_c-python: A Python-based stellar population
synthesis tool and interface to binary_c

Hendriks, D. D.; Izzard, Robert G.

doi:10.21105/joss.04642

Cited by 7 publications

(2 citation statements)

References 14 publications

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“…Stars with a convective surface (red, orange, and purple) harbour equilibrium tides, while stars with a radiative zone around a conv ectiv e core (orange and yellow) harbour dynamical tides. computation, output management, and data storage is performed with the BINARY C-PYTHON software package (Hendriks & Izzard 2023 ).…”

Section: Implementation In Binary Cmentioning

confidence: 99%

Detailed equilibrium and dynamical tides: impact on circularization and synchronization in open clusters

Mirouh,

Hendriks,

Dykes

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Binary stars evolve into chemically-peculiar objects and are a major driver of the Galactic enrichment of heavy elements. During their evolution they undergo interactions, including tides, that circularize orbits and synchronize stellar spins, impacting both individual systems and stellar populations. Using Zahn’s tidal theory and mesa main-sequence model grids, we derive the governing parameters λlm and E2, and implement them in the new mint library of the stellar population code binary_c. Our mint equilibrium tides are 2 to 5 times more efficient than the ubiquitous bse prescriptions while the radiative-tide efficiency drops sharply with increasing age. We also implement precise initial distributions based on bias-corrected observations. We assess the impact of tides and initial orbital-parameter distributions on circularization and synchronization in eight open clusters, comparing synthetic populations and observations through a bootstrapping method. We find that changing the tidal prescription yields no statistically-significant improvement as both calculations typically lie within 0.5σ. The initial distribution, especially the primordial concentration of systems at log10(P/d) ≈ 0.8, e ≈ 0.05 dominates the statistics even when artificially increasing tidal strength. This confirms the inefficiency of tides on the main sequence and shows that constraining tidal-efficiency parameters using the e − log10(P/d) distribution alone is difficult or impossible. Orbital synchronization carries a more striking age-dependent signature of tidal interactions. In M35 we find twice as many synchronized rotators in our mint calculation as with bse. This measure of tidal efficiency is verifiable with combined measurements of orbital parameters and stellar spins.

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Section: Implementation In Binary Cmentioning

confidence: 99%

Detailed equilibrium and dynamical tides: impact on circularization and synchronization in open clusters

Mirouh,

Hendriks,

Dykes

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…libcdict has been used for the last year in the binary_c single-and binary-star population nucleosynthesis framework (Izzard et al, 2004(Izzard et al, , 2006(Izzard et al, , 2009(Izzard et al, , 2018. Recent works (Hendriks & Izzard, 2023b;Izzard & Jermyn, 2023;Mirouh et al, 2023;Yates et al, 2023) compute the evolution of millions of singleand binary-stellar systems in only a few hours using its binary_c-python Python frontend (Hendriks & Izzard, 2023a). We provide libcdict as open-source code on Gitlab subject to the GPL3.…”

Section: Statement Of Needmentioning

confidence: 99%

libcdict: fast dictionaries in C

Izzard,

Hendriks,

Nemergut

2023

JOSS

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A common requirement in science is to store and share large sets of simulation data in an efficient, nested, flexible and human-readable way. Such datasets contain number counts and distributions, i.e. histograms and maps, of arbitrary dimension and variable type, e.g. floatingpoint number, integer or character string. Modern high-level programming languages like Perl and Python have associated arrays, knowns as dictionaries or hashes, respectively, to fulfil this storage need. Low-level languages used more commonly for fast computational simulations, such as C and Fortran, lack this functionality. We present a libcdict, a C dictionary library, to solve this problem. Libcdict provides C and Fortran application programming interfaces (APIs) to native dictionaries, called cdicts, and functions for cdict to load and save these as JSON and hence for easy interpretation in other software and languages like Perl, Python and R.

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Anomalously low-mass core-He-burning star in NGC 6819 as a post-common-envelope phase product

Matteuzzi,

Hendriks,

Izzard

et al. 2024

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Precise masses of red giant stars enable a robust inference of their ages, but there are cases where these age estimates are very precise but also very inaccurate. Examples are core-helium-burning (CHeB) stars that have lost more mass than predicted by standard single-star evolutionary models. Members of star clusters in the Kepler database represent a unique opportunity to identify such stars because they combine exquisite asteroseismic constraints with independent age information (members of a star cluster share a similar age and chemical composition). We focus on the single metal-rich (Z ≈ Z⊙) Li-rich low-mass CHeB star KIC4937011, which is a member of the open cluster NGC 6819 (turn-off mass of ≈1.6 M⊙, i.e. an age of ≈2.4 Gyr). This star has a lower mass by ≈1 M⊙ than expected for its age and metallicity, which might be explained by binary interactions or mass loss along the red giant branch (RGB). To infer formation scenarios for this object, we performed a Bayesian analysis by combining the binary stellar evolutionary framework BINARY_C V2.2.3 with the dynamic nested-sampling approach contained in the DYNESTY V2.1.1 package. We find that this star probably is the result of a common-envelope evolution (CEE) phase during the RGB stage of the primary star in which the low-mass (< 0.71 M⊙) main-sequence companion does not survive. The mass of the primary star at the zero-age main sequence is in the range [1.46, 1.71] M⊙, with a log-orbital period in the range [0.06, 2.4] log10(days). During the CEE phase, ≈1 M⊙ of material is ejected from the system, and the final star reaches the CHeB stage after helium flashes as if it were a single star with a mass of ≈0.7 M⊙, which is what we observe today. Although the proposed scenario is consistent with photometric and spectroscopic observations, a quantitative comparison with detailed stellar evolution calculations is needed to quantify the systematic skewness of the radius, luminosity, and effective temperature distributions towards higher values than observations.

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binary_c-python: A Python-based stellar population synthesis tool and interface to binary_c

Abstract: We present the software package binary_c-python which provides a convenient and easy-touse interface to the binary_c (

Cited by 7 publications

References 14 publications

Detailed equilibrium and dynamical tides: impact on circularization and synchronization in open clusters

Detailed equilibrium and dynamical tides: impact on circularization and synchronization in open clusters

libcdict: fast dictionaries in C

Anomalously low-mass core-He-burning star in NGC 6819 as a post-common-envelope phase product

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