TY - JOUR
T1 - Disks around merging binary black holes
T2 - From GW150914 to supermassive black holes
AU - Khan, Abid
AU - Paschalidis, Vasileios
AU - Ruiz, Milton
AU - Shapiro, Stuart L.
N1 - Publisher Copyright:
© 2018 American Physical Society.
PY - 2018/2/23
Y1 - 2018/2/23
N2 - We 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.
AB - We 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.
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U2 - 10.1103/PhysRevD.97.044036
DO - 10.1103/PhysRevD.97.044036
M3 - Article
C2 - 29963650
AN - SCOPUS:85043699108
SN - 2470-0010
VL - 97
JO - Physical Review D
JF - Physical Review D
IS - 4
M1 - 044036
ER -