2017/10/31 by Kazumi Kashiyama, Kenta Hotokezaka, Kohta Murase
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Galaxy #Gamma-ray bursts and supernovae #Jansky #Microwave #Optics #Outflow #Physics #Pulsars and Gravitational Waves Research #Radio galaxy #Stars #Supernova #Synchrotron #astro-ph.HE
paper · pdf · doi:10.1093/mnras/sty1145
published as Mon.Not.Roy.Astron.Soc. 478 (2018) 2281 · 11 pages, 10 figures, accepted for publication in MNRAS
openalex publication_date 2018/05/01 · arxiv created 2018/06/07 · arxiv updated 2018/06/26 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We consider radio emission from a newborn black hole (BH), which is accompanied by a mini-disc with a mass of ≲M⊙. Such a disc can be formed from an outer edge of the progenitor’s envelope, especially for metal-poor massive stars and/or massive stars in close binaries. The disc accretion rate is typically super-Eddington and an ultrafast outflow with a velocity of ∼0.1–0.3c will be launched into the circumstellar medium. The outflow forms a collisionless shock, and electrons are accelerated and emit synchrotron emission in radio bands with a flux of |∼ 1026-30 \rm erg s-1 Hz-1| days to decades after the BH formation. The model predicts not only a fast UV/optical transient but also quasi-simultaneous inverse-Compton X-ray emission approximately a few days after the BH formation, and the discovery of the radio counterpart with coordinated searches will enable us to identify this type of transients. The occurrence rate can be |0.1\hbox--10 \hbox per cent| of the core-collapse supernova rate, which makes them a promising target of dedicated radio observations such as the Jansky VLA Sky Survey.