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HEAD talk, GRRMHD

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by

Aleksander Sądowski

on 7 November 2013

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Transcript of HEAD talk, GRRMHD

Simulating Radiative Accretion Disks in GR
Black holes
Black holes are common
Dark but involved in most energetic phenomena:
AGN
GRBs
X-ray binaries
Accretion extracts
energy from very strong
gravitational field

Modes of accretion
The goal
GRRMHD
Solving radiative transfer
simple for optically thin medium
simple for pure absorptions
demanding for scattering medium
very demanding in GR
Thin disks
moderate Mdot
opt. thick
high/soft state BH binaries
quasars
Super-critical
disks
high Mdot
optically thick
ULX, GRBs
general relativistic radiation magnetohydrodynamics
Status of numerical simulations
thick hot disks (ADAFs) -
GR, 3D, jets, ...
thin and super-critical disk -
(almost ) terra incognita
lowest Mdot
optically thin
ADAF
low/hard state &
quiescent galaxies
Thick disks
solving gas-radiation coupling photon by photon out of reach
approximations: flux limited diffusion, variable Eddington tensor, M1, ...
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
Code development
3D simulations with HARMRAD
improving M1
(multiple angles, frequencies)
subgrid physics
super-critical disks - radiatively driven winds, jets
thin disks - spectra, jets?
thermal stability
state transitions
...
Applications
so far the only global simulations were Newtonian and based on flux-limited diffusion
Radiative energy density (left) and gas density (right)
Averaged structure

Integrated rest mass flux
Energy at infinity flux
Magnetic flux at BH horizon
Accretion rate
Summary
GR
MHD
M1
GRRMHD
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
Future
Full transcript