2017/11/07 by Shigeo S. Kimura, Kohta Murase, Peter Mészáros · 7 citations
Physics and Astronomy · #Accretion (finance) #Astrophysical Phenomena and Observations #Binary black hole #Binary number #Black hole (networking) #Ejecta #Gamma-ray bursts and supernovae #Light curve #Primary (astronomy) #Pulsars and Gravitational Waves Research #Spectral line #Transient (computer programming) #astro-ph.HE
paper · pdf · doi:10.3847/1538-4357/aa988b
published in The Astrophysical Journal 851(1), 53 (IOP Publishing) · 9 pages, 3 figures, accepted for publication in ApJ, arXiv:1702.07337v2 was split into two papers according to referee's suggestion. This is Paper II. See also arXiv:1702.07337v3 for Paper I
arxiv created 2017/11/07 · openalex created_date 2017/11/10 · openalex publication_date 2017/12/10 · arxiv updated 2017/12/18 · openalex updated_date 2026/08/05
Abstract We discuss the electromagnetic radiation from newborn binary black holes (BBHs). As a consequence of the evolution of massive stellar binaries, a binary consisting of a primary black hole (BH) and a secondary Wolf–Rayet star is expected as a BBH progenitor system. We investigate optical transients from the birth of BBHs powered by the Bondi–Hoyle–Lyttleton accretion onto the primary BH, which occur ∼1–10 Gyr earlier than gravitational-wave signals at the BH–BH merger. When the secondary massive star collapses into a BH, it may eject a fraction of its outer material and may form a disk around the primary BH and induces a powerful disk wind. These primary-induced winds can lead to optical transients with a kinetic energy of ∼10 47 –3 × 10 48 erg, an ejecta velocity of 10 8 –10 9 cm s −1 , a duration of a few days, and an absolute magnitude ranging from about −11 to −14. The light curves and late-time spectra of these transients are distinctive from those of ordinary supernovae, and detection of this type of transient is possible by future optical transient surveys if the event rate of this transient is comparable to the merger rate of BBHs. This paper focuses on the emissions from disk-driven transients induced by the primary BH, different from Paper I, which focuses on wind-driven transients from the tidally locked secondary massive star.