We present a proof-of-concept on how massive stellar triples can lead to sequential binary black hole mergers and GW emission observable by current-day GW facilities. We outline their formation, and explore these events in the context the pair-instability gap. We find that binary black-hole mergers in the pair-instability mass gap can be of triple origin and therefore are not exclusively formed in dense dynamical environments. We propose that the progenitor of GW170729 is a low-metallicity field triple. We support the premise that GW190521 could not have been formed in the field.
I am an assistant professor in computational and theoretical astrophysics
at the Anton Pannekoek Institute of the University of Amsterdam.
I'm also a member of GRAPPA and a chair of
the LISA working package on stellar-mass sources.
I'm interested in the formation and evolution of stellar systems, such as binaries and triples.
How do they evolve? And how do they end their lives? What are the properties of the
energetic and transient phenomena they produce - both in electromagnetic and in
gravitational wave radiation?
toonen [at] uva.nl
s.toonen [at] bham.ac.uk will be deactivated soon
Science Park 904
1098 XH Amsterdam