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HEAD talk, GRRMHD
Transcript of HEAD talk, GRRMHD
Black holes are common
Dark but involved in most energetic phenomena:
energy from very strong
Modes of accretion
Solving radiative transfer
simple for optically thin medium
simple for pure absorptions
demanding for scattering medium
very demanding in GR
high/soft state BH binaries
general relativistic radiation magnetohydrodynamics
Status of numerical simulations
thick hot disks (ADAFs) -
GR, 3D, jets, ...
thin and super-critical disk -
(almost ) terra incognita
low/hard state &
solving gas-radiation coupling photon by photon out of reach
approximations: flux limited diffusion, variable Eddington tensor, M1, ...
Aleksander Sądowski, CfA
in collaboration with:
R. Narayan, A. Tchekhovskoy, J. McKinney
There is a frame where flux vanishes
reasonable, local, simple in GR
far from being perfect
(En. density & Flux)
GRRMHD, 2D, Mdot=100, KORAL
3D simulations with HARMRAD
(multiple angles, frequencies)
super-critical disks - radiatively driven winds, jets
thin disks - spectra, jets?
so far the only global simulations were Newtonian and based on flux-limited diffusion
Radiative energy density (left) and gas density (right)
Integrated rest mass flux
Energy at infinity flux
Magnetic flux at BH horizon
first ever GRRMHD simulations of radiation dominated BH accretion disk
high accretion rate, slim disk branch
jet as efficient as for RIAFs
strong outflows of mass for spinning BHs