2006/04/04 by N. Ivanova, C. O. Heinke, F. A. Rasio +3 · 145 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Brown dwarf #Circumbinary planet #Cluster (spacecraft) #Common envelope #Gamma-ray bursts and supernovae #Globular cluster #Star cluster #Stellar evolution #Supernova #White dwarf #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2006.10876.x
published in Monthly Notices of the Royal Astronomical Society 372(3), 1043-1059 (Oxford University Press) · 17 pages (MNRAS style), 18 figures, submitted to MNRAS (the version with full resolution figures is available at http://www.cita.utoronto.ca/~nata/lit.html)
arxiv created 2006/04/04 · openalex publication_date 2006/09/29 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In this paper, the first of a series, we study the stellar dynamical and evolutionary processes leading to the formation of compact binaries containing white dwarfs (WDs) in dense globular clusters (GCs). We examine the processes leading to the creation of X-ray binaries such as cataclysmic variables (CVs) and AM CVn systems. Using numerical simulations, we identify the dominant formation channels and we predict the expected numbers and characteristics of detectable systems, emphasizing how the cluster sources differ from the field population. We explore the dependence of formation rates on cluster properties and we explain in particular why the distribution of CVs has only a weak dependence on cluster density. We also discuss the frequency of dwarf nova outbursts in GCs and their connection with moderately strong WD magnetic fields. We examine the rates of Type Ia supernovae (SNe Ia) via both single and double degenerate channels in clusters and we argue that those rates may contribute to the total SN Ia rate in elliptical galaxies. Considering coalescing WD binaries, we discuss possible constraints on the common envelope evolution of their progenitors and we derive theoretical expectations for gravitational wave detection by Laser Interferometer Space Antenna (LISA).