Multi-physics simulations using a hierarchical interchangeable software interface

Zwart, Simon F. Portegies; McMillan, Stephen L. W.; Elteren, A. van; Pelupessy, F. I.; Vries, Nathan de

doi:10.1016/j.cpc.2012.09.024

Cited by 174 publications

(38 citation statements)

References 35 publications

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“…To simulate the evolution of star clusters on solar-like orbits, we make use of the Barnes & Hut Tree code (BHTREE; Barnes & Hut 1986) made available through the Astrophysical Multipurpose Software Environment (AMUSE; Portegies Zwart et al 2013;Pelupessy et al 2013;Portegies Zwart & McMillan 2018). Clusters were initialized as Plummer models with masses and half-mass radii of either 510 M and 0.5 pc or 804 M and 3 pc.…”

Section: Simulationsmentioning

confidence: 99%

Searching for solar siblings in APOGEE and Gaia DR2 with N-body simulations

Webb

Price-Jones

Bovy

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We make use of APOGEE and Gaia data to identify stars that are consistent with being born in the same star cluster as the Sun. We limit our analysis to stars that match solar abundances within their uncertainties, as they could have formed from the same Giant Molecular Cloud (GMC) as the Sun. We constrain the range of orbital actions that solar siblings can have with a suite of simulations of solar birth clusters evolved in static and time-dependent tidal fields. In the static tidal field, which contains a bulge, disk, and halo, simulated solar siblings all have 5.8 < J R < 7.4 km s −1 kpc, 1848 < L z < 1868 km s −1 kpc, and 0.27 < J z < 0.49 km s −1 kpc. Given the actions of stars in APOGEE and Gaia , we find one star (Solar Sibling 1) that meets these criteria and shares chemistry with the Sun. Incorporating the effects of a bar and spiral arms increases the range of possible J R and L z for cluster escapers, extending the candidate list to 203 stars. Adding GMCs to the potential can eject solar siblings out of the plane of the disk and increase their J z , resulting in a final candidate list of 550 stars. The entire suite of simulations indicate that solar siblings should have J R < 116 km s −1 kpc, 353 < L z < 2110 km s −1 kpc, and J z < 0.8 km s −1 kpc. Given these criteria, it is most likely that the Sun's birth cluster has reached dissolution and is not the commonly cited open cluster M67.

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Section: Simulationsmentioning

confidence: 99%

Searching for solar siblings in APOGEE and Gaia DR2 with N-body simulations

Webb

Price-Jones

Bovy

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The latter case, which we will refer to as 'isolated' binary evolution, includes interacting systems that undergo mass transfer in the inner binary, and systems in which the tertiary star becomes unbound from the inner binary due to a SNe event but with the inner binary remaining bound, and possibly merging at a later time. Both codes, SecularMultiple and BSE, are implemented within the AMUSE framework (Portegies Zwart et al 2013;Pelupessy et al 2013).…”

Section: Methodsmentioning

confidence: 99%

Double Neutron Star Mergers from Hierarchical Triple-star Systems

Hamers

Thompson

2019

ApJ

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The isolated binary evolution model for merging neutron stars (NSs) involves processes such as mass transfer, common-envelope evolution, and natal kicks, all of which are poorly understood. Also, the predicted NS-NS merger rates are typically lower than the rates inferred from the LIGO GW170817 event. Here, we investigate merger rates of NS and black hole (BH)-NS binaries in hierarchical triple-star systems. In such systems, the tertiary can induce Lidov-Kozai (LK) oscillations in the inner binary, accelerating its coalescence, and potentially enhancing compact object merger rates. However, since compact objects originate from massive stars, the prior evolution should also be taken into account. Natal kicks, in particular, could significantly reduce the rates by unbinding the tertiary before it can affect the inner binary through LK evolution. We carry out simulations of massive triples taking into account stellar evolution starting from the main sequence, secular and tidal evolution, and the effects of supernovae. For large NS birth kicks (σ k = 265 km s −1 ), we find that the triple NS-NS merger rate (several hundred Gpc −3 yr −1 ) is lower by a factor of ∼ 2 − 3 than the binary rate, but for no kicks (σ k = 0 km s −1 ), the triple rate (several thousand Gpc −3 yr −1 ) is comparable to the binary rate. Our results indicate that a significant fraction of NS-NS mergers could originate from triples if a substantial portion of the NS population is born with low kick velocities, as indicated by other work. However, uncertainties and open questions remain because of our simplifying assumption of dynamical decoupling after inner binary interaction has been triggered.

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“…Our numerical algorithm is implemented within the AMUSE framework (Portegies Zwart et al 2013;Pelupessy et al 2013), and is similar to that used for quadruple-star systems by Hamers (2018a), in this case simplifying to the case of three stars. For completeness, we give a brief summary of the most important ingredients of the algorithm, and the assumptions made.…”

Section: Numerical Approach and Simulation Setupmentioning

confidence: 99%

The Impact of White Dwarf Natal Kicks and Stellar Flybys on the Rates of Type Ia Supernovae in Triple-star Systems

Hamers

Thompson

2019

ApJ

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Type Ia supernovae (SNe Ia) could arise from mergers of carbon-oxygen white dwarfs (WDs) triggered by Lidov-Kozai (LK) oscillations in hierarchical triple-star systems. However, predicted merger rates are several orders of magnitude lower than the observed SNe Ia rate. The low predicted rates can be attributed in part to the fact that many potential WD-merger progenitor systems, with high mutual orbital inclination, merge or interact before the WD stage. Recently, evidence was found for the existence of natal kicks imparted on WDs with a typical magnitude of 0.75 km s −1 . In triples, kicks change the mutual inclination and in general increase the outer orbit eccentricity, bringing the triple into an active LK regime at late stages and avoiding the issue of pre-WD merger or interaction. Stars passing by the triple can result in similar effects. However, both processes can also disrupt the triple. In this paper, we quantitatively investigate the impact of WD kicks and flybys on the rate of WD mergers using detailed simulations. We find that WD kicks and flybys combine to increase the predicted WD merger rates by a factor of ∼ 2.5, resulting in a time-integrated rate of ≈ 1.1 × 10 −4 M −1 . Despite the significant boost, the predicted rates are still more than one order of magnitude below the observed rate of ∼ 10 −3 M −1 . However, many systematic uncertainties still remain in our calculations, in particular the potential contributions from tighter triples, dynamically unstable systems, unbound systems due to WD kicks, and quadruple systems.

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Multi-physics simulations using a hierarchical interchangeable software interface

Cited by 174 publications

References 35 publications

Searching for solar siblings in APOGEE and Gaia DR2 with N-body simulations

Searching for solar siblings in APOGEE and Gaia DR2 with N-body simulations

Double Neutron Star Mergers from Hierarchical Triple-star Systems

The Impact of White Dwarf Natal Kicks and Stellar Flybys on the Rates of Type Ia Supernovae in Triple-star Systems

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