BIFROST: simulating compact subsystems in star clusters using a hierarchical fourth-order forward symplectic integrator code

Abstract

We present BIFROST, an extended version of the GPU-accelerated hierarchical fourth-order forward symplectic integrator code FROST. BIFROST (BInaries in FROST) can efficiently evolve collisional stellar systems with arbitrary binary fractions up to $f_{\mathrm{bin}}=100\%$ by using secular and regularised integration for binaries, triples, multiple systems or small clusters around black holes within the fourth-order forward integrator framework. Post-Newtonian (PN) terms up to order PN3.5 are included in the equations of motion of compact subsystems with optional three-body and spin-dependent terms. PN1.0 terms for interactions with black holes are computed everywhere in the simulation domain. The code has several merger criteria (gravitational-wave inspirals, tidal disruption events and stellar and compact object collisions) with the addition of relativistic recoil kicks for compact object mergers. We show that for systems with $N$ particles the scaling of the code remains good up to $N_{\mathrm{GPU}}\sim 40\times N/10^6$ GPUs and that the increasing binary fractions up to 100 per cent hardly increase the code running time (less than a factor $\sim 1.5$). We also validate the numerical accuracy of BIFROST by presenting a number of star clusters simulations the most extreme ones including a core collapse and a merger of two intermediate mass black holes with a relativistic recoil kick.

25 pages, 16 figures, accepted for publication in MNRAS

References in corpus (30)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Binary interaction dominates the evolution of massive stars
• The Effect of Pair-Instability Mass Loss on Black Hole Mergers
• Toward Complete Statistics of Massive Binary Stars: Penultimate Results from the Cygnus OB2 Radial Velocity Survey
• Black holes and core expansion in massive star clusters
• Implementing Few-Body Algorithmic Regularization with Post-Newtonian Terms
• PeTar: a high-performance N-body code for modeling massive collisional stellar systems
• N-body simulations of gravitational dynamics
• The core binary fractions of star clusters from realistic simulations
• Algorithmic regularization with velocity-dependent forces
• Binary stars in the Galactic thick disc
• Star Clusters with Primordial Binaries: I. Dynamical Evolution of Isolated Models
• Radii of Young Star Clusters in Nearby Galaxies
• VINE -- A numerical code for simulating astrophysical systems using particles I: Description of the physics and the numerical methods
• A slow-down time-transformed symplectic integrator for solving the few-body problem
• Black hole mergers in compact star clusters and massive black hole formation beyond the mass-gap
• Multiple Stellar Evolution: a population synthesis algorithm to model the stellar, binary, and dynamical evolution of multiple-star systems
• Formation and evolution of young massive clusters in galaxy mergers: the SMUGGLE view
• MSTAR -- a fast parallelised algorithmically regularised integrator with minimum spanning tree coordinates
• Secular and tidal evolution of circumbinary systems
• Signatures of the Many Supermassive Black Hole Mergers in a Cosmologically Forming Massive Early-Type Galaxy
• Algebraic and machine learning approach to hierarchical triple-star stability
• The formation and early evolution of embedded star clusters in spiral galaxies
• FROST: a momentum-conserving CUDA implementation of a hierarchical fourth-order forward symplectic integrator
• The physics of symplectic integrators: perihelion advances and symplectic corrector algorithms
• SpaceHub: A high-performance gravity integration toolkit for few-body problems in astrophysics
• MYRIAD: A new N-body code for simulations of Star Clusters
• A connected component-based method for efficiently integrating multiscale $N$-body systems
• Pairing mechanisms for binary stars
• The impact of Post-Newtonian effects on massive black hole binary evolution at $\sim 1000R_{sch}$ separations

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• Efficiency of black hole formation via collisions in stellar systems: An analysis of data from simulations and observations
• Formation and evolution of binary black holes in $N$-body simulations of star clusters with up to two million stars
• Little Red Dots are Tidal Disruption Events in Runaway-Collapsing Clusters
• Novel Conservative Methods for Adaptive Force Softening in Collisionless and Multi-Species N-Body Simulations
• Evolution of a black hole cluster in full general relativity
• Evolution of eccentric stellar disks around supermassive black holes: the complex disk disruption dynamics and the milliparsec stars
• Mergers all the way down: stellar collisions and kinematics of a dense hierarchically forming massive star cluster in a dwarf starburst
• Structure Formation with Warm White Noise: Effects of Finite Number Density and Velocity Dispersion in Particle and Wave Dark Matter
• Dynamical evolution of the open clusters with different star formation efficiencies and orbital parameters
• DAWN. I. Simulating the formation and early evolution of stellar clusters with Phantom N-Body
• Radiation magnetohydrodynamics simulations of Population III star formation during the Epoch of Reionization
• FROST-CLUSTERS -- III. Metallicity-dependent intermediate mass black hole formation by runaway collisions in dense star clusters