English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We have used our new technique for fully numerical evolutions of orbitingblack-hole binaries without excision to model the last orbit and merger of anequal-mass black-hole system. We track the trajectories of the individualapparent horizons and find that the binary completed approximately one and athird orbits before forming a common horizon. Upon calculating the completegravitational radiation waveform, horizon mass, and spin, we find that thebinary radiated 3.2% of its mass and 24% of its angular momentum. The earlypart of the waveform, after a relatively short initial burst of spuriousradiation, is oscillatory with increasing amplitude and frequency, as expectedfrom orbital motion. The waveform then transitions to a typical `plunge'waveform; i.e. a rapid rise in amplitude followed by quasinormal ringing. Theplunge part of the waveform is remarkably similar to the waveform from thepreviously studied `ISCO' configuration. We anticipate that the plungewaveform, when starting from quasicircular orbits, has a generic shape that isessentially independent of the initial separation of the binary.Comment: 5 pages, 5 figures, revtex

Last orbit of binary black holes