Abstract
Galactic globular clusters are old, dense star systems typically containing 104–106 stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution that leads to relativistic binaries, and current and possible future observational evidence for this population. Our discussion of globular cluster evolution will focus on the processes that boost the production of tight binary systems and the subsequent interaction of these binaries that can alter the properties of both bodies and can lead to exotic objects. Direct N-body integrations and Fokker-Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.
Highlights
For the purposes of this review, relativistic binaries are systems containing two stellar mass degenerate or collapsed objects that are in close orbits
The dynamical approximations employed coupled with an imperfect understanding of stellar and binary evolution make it impossible to compare the results of these simulations directly to observations
A neutron star binary, for instance, can imply a binary composed of two neutron stars or a binary where a neutron star is paired with any type of secondary depending on the authors preference
Summary
For the purposes of this review, relativistic binaries are systems containing two stellar mass degenerate or collapsed objects that are in close orbits. These models can be compared with the observable members of the population of relativistic binaries in order to try and constrain the entire population. A shorter and more observationally focused review of compact objects in globular clusters can be found in Maccarone and Knigge [306]
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have