The Long-term Evolution of Main-sequence Binaries in DRAGON Simulations

Shu, Qi; Pang, Xiaoying; Dotti, Francesco Flammini; Kouwenhoven, M. B. N.; Sedda, Manuel Arca; Spurzem, Rainer

doi:10.3847/1538-4365/abcfb8

Cited by 6 publications

(7 citation statements)

References 56 publications

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“…When the cluster dynamically ages, the process of two-body relaxation leads to mass segregation, causing an increase in the binary fraction toward the center of globular clusters (Sollima et al 2007;Milone et al 2012). This trend has also been found in Nbody simulations (Portegies Zwart et al 2004;Shu et al 2021). As a consequence of mass segregation, most massive binaries migrate to the cluster center.…”

Section: Introductionmentioning

confidence: 54%

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Pang,

Wang,

Tang

et al. 2023

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Using membership of 85 open clusters from previous studies based on Gaia Data Release 3 data, we identify binary candidates in the color–magnitude diagram for systems with mass ratio q > 0.4. The binary fraction is corrected for incompleteness at different distances due to the Gaia angular resolution limit. We find a decreasing binary fraction with increasing cluster age, with substantial scatter. For clusters with a total mass >200 M ⊙, the binary fraction is independent of cluster mass. The binary fraction depends strongly on stellar density. Among the four types of cluster environments, the lowest-density filamentary and fractal stellar groups have the highest mean binary fraction: 23.6% and 23.2%, respectively. The mean binary fraction in tidal tail clusters is 20.8% and is lowest in the densest halo-type clusters: 14.8%. We find clear evidence of early disruptions of binary stars in the cluster sample. The radial binary fraction depends strongly on the clustercentric distance across all four types of environments, with the smallest binary fraction within the half-mass radius r h and increasing toward a few r h. Only hints of mass segregation are found in the target clusters. The observed amounts of mass segregation are not significant enough to generate a global effect inside the target clusters. We evaluate the bias of unresolved binary systems (assuming a primary mass of 1 M ⊙) in 1D tangential velocity, which is 0.1–1 km s−1. Further studies are required to characterize the internal star cluster kinematics using Gaia proper motions.

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Section: Introductionmentioning

confidence: 54%

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Pang,

Wang,

Tang

et al. 2023

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“…This is a result of dynamical mass segregation in the star cluster. In the million-particle DRAGON simulations, a color difference of 0.2 mag in CSST N U V − y and 0.1 mag in HST F 330W − F 814W has been observed (Shu et al 2021).…”

Section: Uv Flux Ratiomentioning

confidence: 95%

Investigating the UV-excess in star clusters with $N$-body simulations: predictions for future CSST observations

Pang,

Shu,

Wang

et al. 2022

Preprint

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We study the origin of the UV-excess in star clusters by performing N -body simulations of six clusters with N = 10k and N = 100k (single stars & binary systems) and metallicities of Z = 0.01, 0.001, and 0.0001, using PETAR. All models initially have a 50 percent primordial binary fraction. Using GalevNB we convert the simulated data into synthetic spectra and photometry for the China Space Station Telescope (CSST) and Hubble Space Telescope (HST). From the spectral energy distributions we identify three stellar populations that contribute to the UV-excess: (1) second asymptotic giant branch stars, which contribute to the UV flux at early times; (2) naked helium stars, and (3) white dwarfs, which are long-term contributors to the FUV spectra. Binary stars consisting of a white dwarf and a main-sequence star are cataclysmic variable (CV) candidates. The magnitude distribution of CV candidates is bimodal up to 2 Gyr. The bright CV population is particularly bright inof our model clusters is 1-2 mag redder than the UV-excess globular clusters in M 87 and in the Milky Way. This discrepancy may be induced by helium enrichment in observed clusters. Our simulations are based on simple stellar evolution; we do not include the effects of variations in helium and light elements or multiple stellar * Supported by the research grants from the China Manned Space Project with No. CMS-CSST-2021-A08. ORCID

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“…This is a result of dynamical mass segregation in the star cluster. In the million-particle DRAGON simulations, a color difference of 0.2 mag in CSST NUV − y and 0.1 mag in HST F330W − F814W has been observed (Shu et al 2021).…”

Section: Radial Color Gradientsmentioning

confidence: 95%

Investigating the UV-excess in Star Clusters with N-body Simulations: Predictions for Future CSST Observations*

Pang¹,

Shu²,

Wang³

et al. 2022

Res. Astron. Astrophys.

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We study the origin of the UV-excess in star clusters by performing N-body simulations of six clusters with N = 10 k and N = 100 k (single stars & binary systems) and metallicities of Z = 0.01, 0.001 and 0.0001, using petar. All models initially have a 50% primordial binary fraction. Using GalevNB we convert the simulated data into synthetic spectra and photometry for the China Space Station Telescope (CSST) and Hubble Space Telescope (HST). From the spectral energy distributions we identify three stellar populations that contribute to the UV-excess: (1) second asymptotic giant branch stars, which contribute to the UV flux at early times; (2) naked helium stars and (3) white dwarfs, which are long-term contributors to the FUV spectra. Binary stars consisting of a white dwarf and a main sequence star are cataclysmic variable (CV) candidates. The magnitude distribution of CV candidates is bimodal up to 2 Gyr. The bright CV population is particularly bright in FUV − NUV. The FUV − NUV color of our model clusters is 1–2 mag redder than the UV-excess globular clusters in M87 and in the Milky Way. This discrepancy may be induced by helium enrichment in observed clusters. Our simulations are based on simple stellar evolution; we do not include the effects of variations in helium and light elements or multiple stellar populations. A positive radial color gradient is present in CSST NUV − y for main sequence stars in all models with a color difference of 0.2–0.5 mag, up to 4 half-mass radii. The CSST NUV − g color correlates strongly with HST FUV − NUV for NUV − g > 1 mag, with the linear relation FUV − NUV =(1.09 ± 0.12) × (NUV − g) + (−1.01 ± 0.22). This allows for conversion of future CSST NUV − g colors into HST FUV − NUV colors, which are sensitive to UV-excess features. We find that CSST will be able to detect UV-excess in Galactic/extragalactic star clusters with ages >200 Myr.

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The Long-term Evolution of Main-sequence Binaries in DRAGON Simulations

Cited by 6 publications

References 56 publications

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Investigating the UV-excess in star clusters with $N$-body simulations: predictions for future CSST observations

Investigating the UV-excess in Star Clusters with N-body Simulations: Predictions for Future CSST Observations*

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