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Neutron Star Binaries in Open Clusters
Published online by Cambridge University Press: 12 April 2016
Extract
We use N-body simulations of open clusters to examine the evolutionary history of binaries containing neutron stars. The model includes consistent treatment of all the relevant processes (Aarseth 1996):
• Synthetic stellar evolution
– mass and radius as a function of time (Eggleton et al. 1989)
• Accurate treatment of close encounters
– Perturbations of binaries and stable multiple systems - Exchange reactions (involving triple and binary-binary interactions) - Collisions → blue stragglers
• Binary evolution (primordial and dynamically formed)
– Tidal interactions (Mardling & Aarseth 1996) - Stable mass transfer - Common envelope evolution - Magnetic braking - Gravitational radiation - Mergers (including blue stragglers)
• Mass loss
– Stellar winds - Supernovae - Evaporation of stars from the cluster
• Neutron star formation
– Supernovae with kick velocities of Lyne & Lorimer (1994), Drukier (1996) - Accretion-induced collapse
- Type
- Part 7 Binary Systems
- Information
- International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 541 - 542
- Copyright
- Copyright © Astronomical Society of the Pacific 1996
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