2018/01/31 by Abid Khan, Vasileios Paschalidis, Milton Ruiz +1
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Astrophysical Phenomena and Observations #Astrophysics #Binary black hole #Binary number #Black hole (networking) #Classical mechanics #Galaxy #General relativity #Gravitational wave #High-pressure geophysics and materials #LIGO #Observable #Physics #Pulsars and Gravitational Waves Research #Scaling #Supermassive black hole #astro-ph.GA #astro-ph.HE #astro-ph.SR #gr-qc
paper · pdf · doi:10.1103/physrevd.97.044036
published as Phys. Rev. D 97, 044036 (2018) · 14 pages, 6 figures, 5 tables, added discussion and references, matches published version
openalex publication_date 2018/02/23 · arxiv created 2018/02/24 · arxiv updated 2018/02/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
= 29/36. We survey different disk models which differ in their scale height, total size and magnetic field to quantify the robustness of previous simulations on the initial disk model. Scaling our simulations to LIGO GW150914 we find that such systems could explain possible gravitational wave and electromagnetic counterparts such as the Fermi GBM hard x-ray signal reported 0.4 s after GW150915 ended. Scaling our simulations to supermassive binary black holes, we find that observable flow properties such as accretion rate periodicities, the emergence of jets throughout inspiral, merger and postmerger, disk temperatures, thermal frequencies, and the time delay between merger and the boost in jet outflows that we reported in earlier studies display only modest dependence on the initial disk model we consider here.