A connected component-based method for efficiently integrating multi-scale<i>N</i>-body systems

Jänes, Jürgen; Pelupessy, Inti; Zwart, Simon Portegies

doi:10.1051/0004-6361/201423831

Cited by 15 publications

(13 citation statements)

References 21 publications

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“…To integrate the internal dynamical evolution of star clusters, we used the Huayno code (Pelupessy et al 2012;Jänes et al 2014), which is a class of N-body integrators that implements a variety of kick-drift-kick algorithms through the Hamiltonian splitting strategy of adjustable order (see Portegies Zwart & McMillan 2018;Pelupessy et al 2012;Jänes et al 2014, for detailed descriptions). To integrate the evolution of a Hyades-type star cluster, the Huayno code was implemented within the AMUSE environment, which allowed us to couple the direct N-body integration with the stellar evolution code SeBa (Portegies Zwart & Verbunt 1996;Toonen et al 2012) and the integration along the orbit (see Sect.…”

Section: Star Cluster Setup and Evolutionmentioning

confidence: 99%

“…(1) is ε = 4R virial /N. For the other parameters, we used the default Huayno values such as the type 8 integrator HOLD_DKD (for details, see Pelupessy et al 2012;Jänes et al 2014;Portegies Zwart & McMillan 2018).…”

Section: Star Cluster Setup and Evolutionmentioning

confidence: 99%

“…The quantification of the tidal-tail models we performed relies on the N-body integrator Huayno (Pelupessy et al 2012;Jänes et al 2014), which uses an optimal softening length (as described in Sect. 2.2.1, see Eq.…”

Section: Limitation Of the N-body Integratormentioning

confidence: 99%

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The 800 pc long tidal tails of the Hyades star cluster

Jeřabková

Boffin

Beccari

et al. 2021

A&A

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The tidal tails of stellar clusters provide an important tool for studying the birth conditions of the clusters and their evolution, coupling, and interaction with the Galactic potential. The Gaia satellite, with its high-quality astrometric data, opened this field of study, allowing us to observe large-scale tidal tails. Theoretical models of tidal-tail formation and evolution are available. However, the exact appearance of tidal features as seen in the Gaia catalogue has not yet been studied. Here we present the N-body evolution of a Hyades-like stellar cluster with backward-integrated initial conditions on a realistic 3D orbit in the Milky Way galaxy computed within the AMUSE framework. For the first time, we explore the effect of the initial cluster rotation and the presence of lumps in the Galactic potential on the formation and evolution of tidal tails. For all of our simulations we present Gaia observables and derived parameters in the convergent point (CP) diagram. We show that the tidal tails are not naturally clustered in any coordinate system and that they can span up to 40 km s−1 relative to the cluster centre in proper motions for a cluster age of 600–700 Myr. Models with initial rotation result in significant differences in the cluster mass loss and follow different angular momentum time evolution. Thus the orientation of the tidal tails relative to the motion vector of the cluster and the current cluster angular momentum constrain the initial rotation of the cluster. We highlight the use of the standard CP method in searches for co-moving groups and introduce a new compact CP (CCP) method that accounts for internal kinematics based on an assumed model. Using the CCP method, we are able to recover candidate members of the Hyades tidal tails in the Gaia Data Release 2 and early Data Release 3 (eDR3) reaching a total extent of almost 1 kpc. We confirm the previously noted asymmetry in the detected tidal tails. In the eDR3 data we recovered spatial overdensities in the leading and trailing tails that are kinematically consistent with being epicyclic overdensities and thus would present candidates for the first such detection in an open star cluster. We show that the epicyclic overdensities are able to provide constraints not only on the cluster properties, but also on the Galactic potential. Finally, based on N-body simulations, a close encounter with a massive Galactic lump can explain the observed asymmetry in the tidal tails of the Hyades.

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Section: Star Cluster Setup and Evolutionmentioning

confidence: 99%

Section: Star Cluster Setup and Evolutionmentioning

confidence: 99%

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The 800 pc long tidal tails of the Hyades star cluster

Jeřabková

Boffin

Beccari

et al. 2021

A&A

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“…The force calculation in Nemesis is implemented in multiple bridge operations (Fujii et al 2007;Portegies Zwart & McMillan 2018). These bridges integrate the equations of motion of the individual components (particles and the subsystems) via a second-order Verlet kick-drift-kick method (see Hut et al 1995;Jänes et al 2014).…”

Section: Integrating the Systemmentioning

confidence: 99%

Survivability of planetary systems in young and dense star clusters

Elteren

Zwart

Pelupessy

et al. 2019

A&A

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Aims. We perform a simulation using the Astrophysical Multipurpose Software Environment of the Orion Trapezium star cluster in which the evolution of the stars and the dynamics of planetary systems are taken into account. Methods. The initial conditions from earlier simulations were selected in which the size and mass distributions of the observed circumstellar disks in this cluster are satisfactorily reproduced. Four, five, or size planets per star were introduced in orbit around the 500 solar-like stars with a maximum orbital separation of 400 au.Results. Our study focuses on the production of free-floating planets. A total of 357 become unbound from a total of 2522 planets in the initial conditions of the simulation. Of these, 281 leave the cluster within the crossing timescale of the star cluster; the others remain bound to the cluster as free-floating intra-cluster planets. Five of these free-floating intra-cluster planets are captured at a later time by another star.Conclusions. The two main mechanisms by which planets are lost from their host star, ejection upon a strong encounter with another star or internal planetary scattering, drive the evaporation independent of planet mass of orbital separation at birth. The effect of small perturbations due to slow changes in the cluster potential are important for the evolution of planetary systems. In addition, the probability of a star to lose a planet is independent of the planet mass and independent of its initial orbital separation. As a consequence, the mass distribution of free-floating planets is indistinguishable from the mass distribution of planets bound to their host star.Article number, page 3 of 17

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“…We subsequently performed several direct N-body simulations to verify this result. For these we adopted the connected-component symplectic integrator Huayno (Jänes, Pelupessy & Portegies Zwart 2014) within the AMUSE (Portegies Zwart & McMillan 2017) framework. The mild kicks expected due to an interaction with an Oort cloud binary and a massive planet, either passing through or bound to the Oort cloud, are insufficient to explain the observed velocity of 'Oumuamua .…”

Section: Dynamical Ejection From the Sun's Oort Cloudmentioning

confidence: 99%

The origin of interstellar asteroidal objects like 1I/2017 U1 ‘Oumuamua

Zwart

Torres

Pelupessy

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

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We study the origin of the interstellar object 1I/2017 U1 'Oumuamua by juxtaposing estimates based on the observations with simulations. We speculate that objects like 'Oumuamua are formed in the debris disc as left over from the star and planet formation process, and subsequently liberated. The liberation process is mediated either by interaction with other stars in the parental star-cluster, by resonant interactions within the planetesimal disc or by the relatively sudden mass loss when the host star becomes a compact object. Integrating 'Oumuamua backward in time in the Galactic potential together with stars from the Gaia-TGAS catalogue we find that about 1.3 Myr ago 'Oumuamua passed the nearby star HIP 17288 within a mean distance of 1.3 pc. By comparing nearby observed L-dwarfs with simulations of the Galaxy we conclude that the kinematics of 'Oumuamua is consistent with relatively young objects of 1.1-1.7 Gyr. We just met 'Oumuamua by chance, and with a derived mean Galactic density of ∼ 3 × 10 5 similarly sized objects within 100 au from the Sun or ∼ 10 14 per cubic parsec we expect about 2 to 12 such visitors per year within 1 au from the Sun.

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A connected component-based method for efficiently integrating multi-scaleN-body systems

Cited by 15 publications

References 21 publications

The 800 pc long tidal tails of the Hyades star cluster

The 800 pc long tidal tails of the Hyades star cluster

Survivability of planetary systems in young and dense star clusters

The origin of interstellar asteroidal objects like 1I/2017 U1 ‘Oumuamua

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