Gravitational N-Body Simulations

By S. Aarseth. 2003

661 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a9d1ed5f0c54fb9d17eb87f998ae30d30bce2199

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Citations in the corpus

A sub-parsec resolution simulation of the Milky Way: global structure of the interstellar medium and properties of molecular clouds (2013, methodology): “his is not the case in dense systems where star-star interactions are c 0000 RAS, MNRAS 000, 000–000 4 Renaudetal. dedicated numerical techniques in the context of molecular clouds and star clusters (Aarseth 2003), the integration of the galactic scale eﬀects in such simulations has started out only”
Stellar Remnants in Galactic Nuclei: Mass Segregation (2006, background): “They are described in detail in Aarseth (1999, 2003).”
Stellar collisions during binary–binary and binary–single star interactions (2004, methodology): “For the sake of simplicity, we have chosen not to implement the appropriate technique for detecting collisions with regularization (see section 9.8 of Aarseth 2003).”
Young Massive Star Clusters (2010, methodology): “A.3 N-body methods N -body codes incorporate detailed descriptions of stellar dynamics at all levels, using direct integration of the individual (Newtonian) stellar equations of motion for all stars (Aarseth 2003, Heggie & Hut 2003).”
Merging black holes in young star clusters (2019, background): “NBODY6++GPU and MOBSE are perfectly integrated: they update stellar parameters and trajectories simultaneously during the computation.”
The stellar and sub-stellar IMF of simple and composite populations (2011, background): “8.2 in Aarseth 2003 for a related concept).”
On the variation of the initial mass function (2000, methodology): “C odes The dynam icalevolution ofthe clusters studied here is calculated using N body6 (Aarseth 1999; Aarseth 2000),which includes state-of-the artstellarevolution (Hurley,Pols& Tout2000),a standard G alactic tidal eld (Terlevich 1987),and additionalroutines for initiating the binary-rich…”
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “…these diffuse low-mass clusters constitute a low fraction of the total mass of the MW GC system and also because these clusters straddle the boundary between GCs and open clusters, the latter of which are well known to be better suited for direct N-body modeling (e.g., Aarseth 2003, for a review).”
IMPLEMENTING FEW-BODY ALGORITHMIC REGULARIZATION WITH POST-NEWTONIAN TERMS (2007, methodology): “More details about the thus-far mentioned methods can be found in the book by Aarseth (2003).”
The dragon simulations: globular cluster evolution with a million stars (2016, methodology): “ 2014) stars. Employment of new hardware and software signiﬁcantly improved the performance of the simulation programs. Essential was the series of NBODY codes developed by Aarseth and collaborators (Aarseth 2003; Nitadori & Aarseth 2012; Wang et al. 2015) combined with the specialpurpose hardwa”
Rapid Eccentricity Oscillations and the Mergers of Compact Objects in Hierarchical Triples (2013, background): “In general, roundoff error in N-body dynamical simulations can be avoided with some variation of algorithmic regularization (see, e.g., Mikkola & Tanikawa 1999; Aarseth 2003).”
Toward Understanding Massive Star Formation (2007, background): “Also, the timescales for the N-body dynamics are short enough for the whole process to occur on or before the ZAMS (van Albada 1968, Aarseth 2003).”
The effects of fly‐bys on planetary systems (2010, methodology): “A complete description of the physics included and algorithms used in NBODY6 can be found in Aarseth (2003).”
Tidal tails of star clusters (2009, methodology): “ives us an idea of the maximum importance of a wide range of realistic tidal inﬂuences on star clusters and their tidal tails. All computations were performed with the collisional N-body code NBODY4 (Aarseth 1999, 2003) on the GRAPE-6A supercomputers at the AIfA (Fukushige, Makino & Kawai 2005).”