Hydrodynamic Instabilities in Close Binary Systems
| dc.creator | Rasio, Frederic A. | |
| dc.date | 1995-12-13 | |
| dc.date.accessioned | 2026-07-07T02:20:36Z | |
| dc.date.available | 2026-07-07T02:20:36Z | |
| dc.description | Equilibrium fluid configurations for close binary systems can become {\em globally unstable\/}. Instabilities arise from the strong tidal interaction between the two components, which tends to make the effective two-body potential governing the orbital motion steeper than $1/r$. As a result, a circular orbit can become unstable to small radial perturbations. The instability can be either secular or dynamical. In both cases it leads to the coalescence and merging of the two components on a timescale generally much shorter than the lifetime of a stable system. Binary coalescence is relevant to a wide variety of astrophysical problems including the formation of blue stragglers, Type~Ia supernovae, the evolution of massive X-ray binaries, and the detection of gravitational waves. | |
| dc.description | uuencoded compressed postscript, 20 pages including figures. To appear in Evolutionary Processes in Binary Stars (NATO ASI), eds. R. Wijers et al. (Dordrecht: Kluwer). Also available from http://ensor.mit.edu/~rasio | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9512089 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9512089 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/10263 | |
| dc.subject | Astrophysics | |
| dc.title | Hydrodynamic Instabilities in Close Binary Systems | |
| dc.type | text |