Are you ready to FLY in the universe? A multi-platform \(N\)-body tree code for parallel supercomputers. (English) Zbl 0978.83500
Summary: In the last few years, cosmological simulations of structures and galaxies formations have assumed a fundamental role in the study of the origin, formation and evolution of the universe. These studies improved enormously with the use of supercomputers and parallel systems, allowing more accurate simulations, in comparison with traditional serial systems. The code we describe, called FLY, is a newly written code (using the tree \(N\)-body method), for three-dimensional self-gravitating collisionless systems evolution.
FLY is a fully parallel code based on the tree Barnes-Hut algorithm and periodical boundary conditions are implemented by means of the Ewald summation technique. We use FLY to run simulations of the large scale structure of the universe and of clusters of galaxies, but it could be usefully adopted to run evolutions of systems based on a tree \(N\)-body algorithm. FLY is based on the one-side communication paradigm to share data among the processors, that access to remote private data avoiding any kind of synchronism. The code was originally developed on CRAY T3E system using the logically SHared MEMory access routines (SHMEM) but it runs also on SGI ORIGIN systems and on IBM SP by using the Low-Level Application Programming Interface routines (LAPI).
This new code is the evolution of preliminary codes (WDSH-PT and WD99) for cosmological simulations we implemented in the last years, and it reaches very high performance in all systems where it has been well-tested. This performance allows us today to consider the code FLY among the most powerful parallel codes for tree \(N\)-body simulations. The performance that FLY reaches is discussed and reported, and a comparison with other similar codes is considered. The FLY version 1.1 is freely available on http://www.ct.astro.it/fly/ and it will be maintained and upgraded with new releases.
FLY is a fully parallel code based on the tree Barnes-Hut algorithm and periodical boundary conditions are implemented by means of the Ewald summation technique. We use FLY to run simulations of the large scale structure of the universe and of clusters of galaxies, but it could be usefully adopted to run evolutions of systems based on a tree \(N\)-body algorithm. FLY is based on the one-side communication paradigm to share data among the processors, that access to remote private data avoiding any kind of synchronism. The code was originally developed on CRAY T3E system using the logically SHared MEMory access routines (SHMEM) but it runs also on SGI ORIGIN systems and on IBM SP by using the Low-Level Application Programming Interface routines (LAPI).
This new code is the evolution of preliminary codes (WDSH-PT and WD99) for cosmological simulations we implemented in the last years, and it reaches very high performance in all systems where it has been well-tested. This performance allows us today to consider the code FLY among the most powerful parallel codes for tree \(N\)-body simulations. The performance that FLY reaches is discussed and reported, and a comparison with other similar codes is considered. The FLY version 1.1 is freely available on http://www.ct.astro.it/fly/ and it will be maintained and upgraded with new releases.
MSC:
| 83-08 | Computational methods for problems pertaining to relativity and gravitational theory |
| 83B05 | Observational and experimental questions in relativity and gravitational theory |
| 83C10 | Equations of motion in general relativity and gravitational theory |
References:
| [1] | Antonuccio-Delogu, V.; Becciani, U., (Parallel Scientific Computing — PARA’94 (1994), Springer: Springer Berlin), 17 |
| [2] | Antonuccio-Delogu, V.; Becciani, U.; Pagliaro, A.; Van Kampen, E.; Colafrancesco, S.; Germaná, A.; Gambera, M., MNRAS (2000), submitted; also |
| [3] | Becciani, U.; Antonuccio-Delogu, V.; Gheller, C.; Calori, L.; Buonomo, F.; Imboden, S., IEEE CG&A (2000), submitted; also |
| [4] | Barnes, J., (Hut, P.; McMillan, S., Use of Supercomputers in Stellar Dynamics (1986), Springer: Springer Berlin), 175 |
| [5] | Barnes, J., J. Comput. Phys., 87, 161 (1990) · Zbl 0689.68002 |
| [6] | Barnes, J. E.; Hut, P., Nature, 324, 446 (1986) |
| [7] | Becciani, U.; Antonuccio-Delogu, V.; Pagliaro, A., Comput. Phys. Comm., 99, 1 (1996) · Zbl 0948.70500 |
| [8] | Becciani, U.; Ansaloni, R.; Antonuccio-Delogu, V.; Erbacci, G.; Gambera, M.; Pagliaro, A., Comput. Phys. Comm., 106, 1 (1997) · Zbl 0934.83053 |
| [9] | Becciani, U.; Antonuccio-Delogu, V., J. Comput. Phys., 163, 118 (2000) · Zbl 0968.83050 |
| [10] | Cray MPP Fortran Reference Manual, SR-2504 6.1 (1994), Cray Research Inc. |
| [11] | Dubinski, J., M.Sc. Thesis (1988), University of Toronto |
| [12] | Dubinski, J., New Astronomy, 133, 1 (1996) |
| [13] | Springel, V.; Yoshida, N.; White, S. D.M., New Astronomy (2000), submitted; also |
| [14] | Hernquist, L., ApJ. Suppl., 64, 715 (1987) |
| [15] | Hernquist, L.; Bouchet, F. R.; Suto, Y., ApJ. Suppl., 75, 231 (1991) |
| [16] | Hockney, R. W.; Eastwood, J. W., Computer Simulation Using Particles (1981), Mcgraw-Hill International: Mcgraw-Hill International New York · Zbl 0662.76002 |
| [17] | Geist, A.; Beguelin, A.; Dongarra, J.; Jiang, W.; Manchek, R.; Sunderam, V., PVM 3 User’s Guide and Reference Manual, ORNL/TM-12187 (1994) |
| [18] | Salmon, J., PhD Thesis (1990), California Institute of Technology |
| [19] | Salmon, J.; Warren, M. S., (Proc. of the Eight Conf. on Parallel Processing for Scientific Computing (1997), SIAM) |
This reference list is based on information provided by the publisher or from digital mathematics libraries. Its items are heuristically matched to zbMATH identifiers and may contain data conversion errors. In some cases that data have been complemented/enhanced by data from zbMATH Open. This attempts to reflect the references listed in the original paper as accurately as possible without claiming completeness or a perfect matching.
