MLAPM - a C code for cosmological simulations
We present a computer code written in C that is designed to simulate structure formation from collisionless matter. The code is purely grid-based and uses a recursively refined Cartesian grid to solve Poisson's equation for the potential, rather than obtaining the potential from a Green's...
| Main Authors: | , , |
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| Format: | Journal article |
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2001
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| _version_ | 1826264947996229632 |
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| author | Knebe, A Green, A Binney, J |
| author_facet | Knebe, A Green, A Binney, J |
| author_sort | Knebe, A |
| collection | OXFORD |
| description | We present a computer code written in C that is designed to simulate structure formation from collisionless matter. The code is purely grid-based and uses a recursively refined Cartesian grid to solve Poisson's equation for the potential, rather than obtaining the potential from a Green's function. Refinements can have arbitrary shapes and in practice closely follow the complex morphology of the density field that evolves. The timestep shortens by a factor two with each successive refinement. It is argued that an appropriate choice of softening length is of great importance and that the softening should be at all points an appropriate multiple of the local inter-particle separation. Unlike tree and P3M codes, multigrid codes automatically satisfy this requirement. We show that at early times and low densities in cosmological simulations, the softening needs to be significantly smaller relative to the inter-particle separation than in virialized regions. Tests of the ability of the code's Poisson solver to recover the gravitational fields of both virialized halos and Zel'dovich waves are presented, as are tests of the code's ability to reproduce analytic solutions for plane-wave evolution. The times required to conduct a LCDM cosmological simulation for various configurations are compared with the times required to complete the same simulation with the ART, AP3M and GADGET codes. The power spectra, halo mass functions and halo-halo correlation functions of simulations conducted with different codes are compared. |
| first_indexed | 2024-03-06T20:15:58Z |
| format | Journal article |
| id | oxford-uuid:2c27ec31-a193-4914-97ea-2db4d7e8eb90 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T20:15:58Z |
| publishDate | 2001 |
| record_format | dspace |
| spelling | oxford-uuid:2c27ec31-a193-4914-97ea-2db4d7e8eb902022-03-26T12:35:16ZMLAPM - a C code for cosmological simulationsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:2c27ec31-a193-4914-97ea-2db4d7e8eb90Symplectic Elements at Oxford2001Knebe, AGreen, ABinney, JWe present a computer code written in C that is designed to simulate structure formation from collisionless matter. The code is purely grid-based and uses a recursively refined Cartesian grid to solve Poisson's equation for the potential, rather than obtaining the potential from a Green's function. Refinements can have arbitrary shapes and in practice closely follow the complex morphology of the density field that evolves. The timestep shortens by a factor two with each successive refinement. It is argued that an appropriate choice of softening length is of great importance and that the softening should be at all points an appropriate multiple of the local inter-particle separation. Unlike tree and P3M codes, multigrid codes automatically satisfy this requirement. We show that at early times and low densities in cosmological simulations, the softening needs to be significantly smaller relative to the inter-particle separation than in virialized regions. Tests of the ability of the code's Poisson solver to recover the gravitational fields of both virialized halos and Zel'dovich waves are presented, as are tests of the code's ability to reproduce analytic solutions for plane-wave evolution. The times required to conduct a LCDM cosmological simulation for various configurations are compared with the times required to complete the same simulation with the ART, AP3M and GADGET codes. The power spectra, halo mass functions and halo-halo correlation functions of simulations conducted with different codes are compared. |
| spellingShingle | Knebe, A Green, A Binney, J MLAPM - a C code for cosmological simulations |
| title | MLAPM - a C code for cosmological simulations |
| title_full | MLAPM - a C code for cosmological simulations |
| title_fullStr | MLAPM - a C code for cosmological simulations |
| title_full_unstemmed | MLAPM - a C code for cosmological simulations |
| title_short | MLAPM - a C code for cosmological simulations |
| title_sort | mlapm a c code for cosmological simulations |
| work_keys_str_mv | AT knebea mlapmaccodeforcosmologicalsimulations AT greena mlapmaccodeforcosmologicalsimulations AT binneyj mlapmaccodeforcosmologicalsimulations |