Stellar Dynamics of Dense Stellar Systems
| dc.creator | Hut, Piet | |
| dc.date | 1998-04-08 | |
| dc.date.accessioned | 2026-07-07T02:26:34Z | |
| dc.date.available | 2026-07-07T02:26:34Z | |
| dc.description | Stellar dynamics is almost unreasonably well suited for an implementation in terms of special-purpose hardware. Unlike the case of molecular dynamics, stellar dynamics deals exclusively with a long-range force, gravity, which leads to a computational cost scaling as the square of the number of stars involved. While special tricks can lead to a reduction of this cost from $\sim N^2$ to $\sim N\log N$ in the case of very large particle numbers, such tricks are not suitable for all areas within stellar dynamics. When a stellar system is close to equilibrium, and has a very high density, it still pays to compute all interactions on a star by star basis, even for $N=10^5$. Any $cN\log N$ approach would either gloss over the subtle net effects of near-canceling interactions, driving the evolution of such a system, or would carry a prohibitively large coefficient $c$. This paper presents a brief introduction to the stellar dynamics of dense stellar systems, aimed at researchers using special purpose computers in other branches of physics. | |
| dc.description | 10 pages, LaTeX, to appear in the proceedings for the International Symposium on Supercomputing, held in Tokyo, Japan, September 1-3, 1997 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9804089 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9804089 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/12322 | |
| dc.subject | Astrophysics | |
| dc.title | Stellar Dynamics of Dense Stellar Systems | |
| dc.type | text |