N-Body Simulations of Open, Self-Gravitating Systems
| dc.creator | Huber, Daniel | |
| dc.date | 2001-01-16 | |
| dc.date.accessioned | 2026-07-07T01:57:24Z | |
| dc.date.available | 2026-07-07T01:57:24Z | |
| dc.description | Astrophysical systems differ often in two points from classical thermodynamical systems: 1.) They are open and 2.) gravity is a dominant factor. Both modifies the homogeneous equilibrium structure, known from classical thermodynamics. In order to study the consequence for structure formation in astrophysical systems, we carry out N-body simulations of self-gravitating systems, subjected to an energy-flow. The simulations show that physically realistic, time-dependent boundary conditions can maintain a molecular cloud in a statistically steady state, out of thermodynamic equilibrium. Moreover we perform some simple "gravo-thermal" N-body experiments and compare them with theoretical results. We find negative specific heat in an energy range predicted by Follana and Laliena (1999). | |
| dc.description | 5 pages, 7 figures. To be published in the proceedings of "The Promise of FIRST" symposium, eds. G.L. Pilbratt, J. Cernicharo, A.M. Heras, T. Prusti, R. Harris, ESA SP-460, 2001 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0101265 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0101265 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2373 | |
| dc.subject | Astrophysics | |
| dc.title | N-Body Simulations of Open, Self-Gravitating Systems | |
| dc.type | text |