nbody6++gpu: ready for the gravitational million-body problem

Wang, Long; Spurzem, Rainer; Aarseth, Sverre J.; Nitadori, Keigo; Berczik, Peter; Kouwenhoven, M. B. N.; Naab, Thorsten

doi:10.1093/mnras/stv817

Cited by 242 publications

(207 citation statements)

References 40 publications

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“…The N -body simulations of star clusters in this paper were carried out with NBODY6++GPU (Wang et al 2015(Wang et al , 2016 1 . This code is based on the well-known legacy code NBODY6 and its precursors, developed by S. Aarseth since the 1960s for direct N -body integration of stellar systems (see for an overview Aarseth 1999Aarseth , 2003.…”

Section: Simulation Methodsmentioning

confidence: 99%

“…Later, a GPU-based parallelized version (NBODY6GPU), designed for a desktop or a single computer node with GPU was developed by Nitadori & Aarseth (2012). Wang et al (2015Wang et al ( , 2016 provide a combination of MPI parallelization with the use of many GPUs (using GPU acceleration for every MPI process), with the added feature of OpenMP (or SSE/AVX) used for the neighbour forces. This latest variant, called NBODY6++GPU can be used across multiple GPUaccelerated nodes on supercomputers combining MPI, OpenMP and CUDA-based GPU parallel computing principles.…”

Section: Simulation Methodsmentioning

confidence: 99%

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The dynamical origin of multiple populations in intermediate-age clusters in the Magellanic Clouds

Grijs

Askar

Berczik

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Numerical simulations were carried out to study the origin of multiple stellar populations in the intermediate-age clusters NGC 411 and NGC 1806 in the Magellanic Clouds. We performed NBODY6++ simulations based on two different formation scenarios, an ad hoc formation model where second-generation (SG) stars are formed inside a cluster of first-generation (FG) stars using the gas accumulated from the external intergalactic medium and a minor merger model of unequal mass (M SG /M FG ∼ 5-10%) clusters with an age difference of a few hundred million years. We compared our results such as the radial profile of the SG-to-FG number ratio with observations on the assumption that the SG stars in the observations are composed of cluster members, and confirmed that both the ad hoc formation and merger scenarios reproduce the observed radial trend of the SG-to-FG number ratio which shows less centrally concentrated SG than FG stars. It is difficult to constrain the formation scenario for the multiple populations by only using the spatial distribution of the SG stars. SG stars originating from the merger scenario show a significant velocity anisotropy and rotational features compared to those from the ad hoc formation scenario. Thus, observations aimed at kinematic properties like velocity anisotropy or rotational velocities for SG stars should be obtained to better understand the formation of the multiple populations in these clusters. This is, however, beyond current instrumentation capabilities.

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Section: Simulation Methodsmentioning

confidence: 99%

Section: Simulation Methodsmentioning

confidence: 99%

The dynamical origin of multiple populations in intermediate-age clusters in the Magellanic Clouds

Grijs

Askar

Berczik

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

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“…High-performance computers, more efficient software parallelization, and more modular codes and code environments like AMUSE (amusecode.org, [78]), are pushing the computational limits on star cluster models into new regimes. Great strides have been made recently that may soon open the door to modeling realistic globular clusters with the star-by-star direct N-body method [96] (which is preferred as this requires the least simplifying assumptions of all methods). Realistic open cluster models including 1000s of stars and large populations of multi-planet and multi-stellar systems, evolved for many 100s of Myr, are also on the verge of feasibility and will be completed in the near future.…”

Section: Pos(bash2015)006mentioning

confidence: 99%

Dynamical Processing of Stars and Planets Through Star Clusters

Geller¹

2016

Proceedings of Frank N. Bash Symposium 2015 — PoS(BASH2015)

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Most stars are born in clustered environments that are far denser than the Solar Neighborhood.Yet, star clusters can be hostile locations, where close stellar encounters can be frequent and can have violent consequences, including direct stellar collisions. Such encounters can dramatically alter stellar and planetary systems, and can produce exotic stars that define new pathways in stellar evolution. Understanding how, and to what extent, such "dynamically processing" occurs in star clusters may be critical for our understanding of the architectures of today's observed stellar and planetary systems, as well as the origins of X-ray sources, blue stragglers, sub-subgiants, and other stellar exotica. In this contribution, I discuss the impacts of living in a star cluster on its inhabitants, through a review of observational and theoretical efforts to study these complex systems. Throughout, I assert that binary stars are intimately linked to both the dynamical evolution of star clusters and the effects that stellar encounters within these environments have on their stellar and planetary populations. I conclude that in order to properly interpret our present and future observations of stars and planets, both in star clusters and the field, and particularly if we attempt to use these observations to inform star and planet formation theory, we must first account for the imprint left by stellar encounters within a clustered birth environment.

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“…The long-standing goal of simulating the evolution of a realistic million-body globular cluster (GC) up to twelve-billion years with a direct N -body code was recently achieved by Wang et al (2016) with the nbody6++gpu code (Wang et al 2015). With increasingly more realistic simulations of star clusters, there is also a need to validate and compare results with observations.…”

Section: Introductionmentioning

confidence: 99%

COCOA Code for Creating Mock Observations of Star Cluster Models

Askar

Giersz

Pych

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We introduce and present results from the cocoa (Cluster simulatiOn Comparison with ObservAtions) code that has been developed to create idealized mock photometric observations using results from numerical simulations of star cluster evolution. cocoa is able to present the output of realistic numerical simulations of star clusters carried out using Monte Carlo or N -body codes in a way that is useful for direct comparison with photometric observations. In this paper, we describe the cocoa code and demonstrate its different applications by utilizing globular cluster (GC) models simulated with the mocca (MOnte Carlo Cluster simulAtor) code. cocoa is used to synthetically observe these different GC models with optical telescopes, perform PSF photometry and subsequently produce observed colour magnitude diagrams. We also use cocoa to compare the results from synthetic observations of a cluster model that has the same age and metallicity as the Galactic GC NGC 2808 with observations of the same cluster carried out with a 2.2 meter optical telescope. We find that cocoa can effectively simulate realistic observations and recover photometric data. cocoa has numerous scientific applications that maybe be helpful for both theoreticians and observers that work on star clusters. Plans for further improving and developing the code are also discussed in this paper.

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nbody6++gpu: ready for the gravitational million-body problem

Cited by 242 publications

References 40 publications

The dynamical origin of multiple populations in intermediate-age clusters in the Magellanic Clouds

The dynamical origin of multiple populations in intermediate-age clusters in the Magellanic Clouds

Dynamical Processing of Stars and Planets Through Star Clusters

COCOA Code for Creating Mock Observations of Star Cluster Models

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