Shadowing-based reliability decay in softened n-body simulations

被引:8
作者
Hayes, WB [1 ]
机构
[1] Univ Toronto, Dept Comp Sci, Toronto, ON M5S 3G4, Canada
关键词
methods : n-body simulations;
D O I
10.1086/375263
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
A shadow of a numerical solution to a chaotic system is an exact solution to the equations of motion that remains close to the numerical solution for a long time. In a collisionless n-body system, we know that particle motion is governed by the global potential rather than by interparticle interactions. As a result, the trajectory of each individual particle in the system is independently shadowable. It is thus meaningful to measure the number of particles that have shadowable trajectories as a function of time. We find that the number of shadowable particles decays exponentially with time as e(-mut) and that for epsilon is an element of [similar to0.2, 1] (in units of the local mean interparticle separation (n) over bar), there is an explicit relationship among the decay constant mu, the time step h of the leapfrog integrator, the softening epsilon, and the number of particles N in the simulation. Thus, given N and epsilon, it is possible to precompute the time step h necessary to achieve a desired fraction of shadowable particles after a given length of simulation time. We demonstrate that a large fraction of particles remain shadowable over similar to100 crossing times even if particles travel up to about 1/3 of the softening length per time step. However, a sharp decrease in the number of shadowable particles occurs if the time step increases to allow particles to travel farther than the softening length in 1 time step or if the softening is decreased below similar to0.2 (n) over bar.
引用
收藏
页码:L59 / L62
页数:4
相关论文
共 12 条
[1]   Simulations of structure formation in the universe [J].
Bertschinger, E .
ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, 1998, 36 :599-654
[2]  
Binney J., 2008, Galactic Dynamics
[3]  
CLARKE DA, 1997, 12 KINGST M COMP AST, V123
[4]   OBSTRUCTIONS TO SHADOWING WHEN A LYAPUNOV EXPONENT FLUCTUATES ABOUT ZERO [J].
DAWSON, S ;
GREBOGI, C ;
SAUER, T ;
YORKE, JA .
PHYSICAL REVIEW LETTERS, 1994, 73 (14) :1927-1930
[5]   ON THE EXPONENTIAL INSTABILITY OF N-BODY SYSTEMS [J].
GOODMAN, J ;
HEGGIE, DC ;
HUT, P .
ASTROPHYSICAL JOURNAL, 1993, 415 (02) :715-733
[6]  
HAYES W, 1995, THESIS U TORONTO
[7]   Shadowing high-dimensional hamiltonian systems:: The gravitational N-body problem -: art. no. 054104 [J].
Hayes, WB .
PHYSICAL REVIEW LETTERS, 2003, 90 (05) :4
[8]  
HEGGIE DC, 1986, USE SUPERCOMPUTERS S, P33
[9]   DISCRETENESS NOISE VERSUS FORCE ERRORS IN N-BODY SIMULATIONS [J].
HERNQUIST, L ;
HUT, P ;
MAKINO, J .
ASTROPHYSICAL JOURNAL, 1993, 402 (02) :L85-L88
[10]   ON THE RELIABILITY OF GRAVITATIONAL N-BODY INTEGRATIONS [J].
QUINLAN, GD ;
TREMAINE, S .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1992, 259 (03) :505-518