Disks around merging binary black holes: From GW150914 to supermassive black holes
AffiliationUniv Arizona, Dept Astron, Theoret Astrophys Program
Univ Arizona, Dept Phys, Theoret Astrophys Program
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationDisks around merging binary black holes: From GW150914 to supermassive black holes 2018, 97 (4) Physical Review D
JournalPhysical Review D
Rights© 2018 American Physical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractWe perform magnetohydrodynamic simulations in full general relativity of disk accretion onto nonspinning black hole binaries with mass ratio q = 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.
VersionFinal published version
SponsorsNSF [PHY-1602536, PHY-1662211, PHY-1607449, OCI-1053575]; NASA [NNX13AH44G, 80NSSC17K0070, NNX16AR67G]; Simons foundation; National Science Foundation [OCI 07-25070]; state of Illinois