Studies of the internal dynamics of stellar clusters is conducted primarily through N-Body simulations. A key input into these simulations is the fraction and mass distribution of binary stars. The internal dynamics of stellar clusters is conducted primarily through N-Body simulations. A key input into these simulations is the fraction and mass distribution of binary stars. Currently the N-body input relations are taken from "field" binary stars studies, but to truly understand how clustered environments evolve, binary data from within star clusters is needed, including detailed mass information. The detailed information on binaries masses, primary and secondary, in star clusters has been limited to bright high mass stars that are reachable using decade-long radial velocity surveys. We introduce a new binary detection method, Binary INformation from Open Clusters Using SEDs (BINOCS) that covers the wide mass range needed to improve cluster N-body simulation inputs and comparisons. Using newly-observed multi-wavelength photometric catalogs (0.3 - 8 microns) of the key open clusters with a range of ages, we can show that the BINOCS method determines accurate binary component masses for unresolved cluster binaries through comparison to available RV-based studies. Using this method, we present results on the dynamical evolution of binaries from 0.4 - 2.5 solar masses within nine prototypical clusters, spaning 30 Myr to 7 Gyr, and show how the binary populations evolve, and discover significant variations in the "dynamical age" of a clusters as a function of the stellar mass range studied.
American Astronomical Society Meeting Abstracts #227
- Pub Date:
- January 2016