TreePM: A code for cosmological N-body simulations

By J. Bagla. 1999

We describe the TreePM method for carrying out large N-Body simulations to study formation and evolution of the large scale structure in the Universe. This method is a combination of Barnes and Hut tree code and Particle-Mesh code. It combines the automatic inclusion of periodic boundary conditions of PM simulations with the high resolution of tree codes. This is done by splitting the gravitational force into a short range and a long range component. We describe the splitting of force between these two parts. We outline the key differences between TreePM and some other N-Body methods.

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Citations in the corpus

The Cosmological simulation code GADGET-2 (2005, unknown): “GADGET-2 ’s mathematical implementation of this so-called TreePM method (Xu, 1995; Bode et al., 2000; Bagla, 2002) is similar to that of Bagla & Ray (2003).”
FastPM: a new scheme for fast simulations of dark matter and haloes (2016, background): “…is calculated separately, a Gaussian function Wg(k) = exp[−(krs)2] is often added to apodize the long range force and suppress grid anisotropy, rs being the smoothing scale of long range force (typical slightly larger than the force mesh cell sizes) (Bagla 2002; Springel 2005; Habib et al. 2013).”
Simulating galaxy formation with the IllustrisTNG model (2017, methodology): “The Tree-PM scheme is a synthesis of the particle-mesh method and the tree algorithm (Xu 1995; Bode, Ostriker & Xu 2000; Bagla 2002), where the gravitational potential is explicitly split in Fourier space into a long-range and a short-range part.”
Comparing AMR and SPH Cosmological Simulations. I. Dark Matter and Adiabatic Simulations (2003, unknown): “GADGET’s mathematical implementation of this so-called TreePM method (Xu 1995; Bode et al. 2000; Bagla 2002) is similar to that of Bagla & Ray (2003).”