GRMHD Simulations of Accretion Disk and Jets around Black Holes
GRMHD Simulations of Accretion Disk and Jets around Black Holes
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Accretion flow around a massive object is ubiquitous in astrophysics which is often accompanied by outflows and jets ejected at relativistic speeds. The mechanism of accretion flows is mainly governed by the interaction of a non-Maxwellian plasma with a relativistic gravitational field, a strong electromagnetic field, and possibly a strong radiation field as well. The plasma is generally treated as a fluid and thus general relativistic magnetohydrodynamic (GRMHD) equations are solved, which include magnetic field and radiation.
Accretion flow around a massive object is ubiquitous in astrophysics which is often accompanied by outflows and jets ejected at relativistic speeds. The mechanism of accretion flows is mainly governed by the interaction of a non-Maxwellian plasma with a relativistic gravitational field, a strong electromagnetic field, and possibly a strong radiation field as well. The plasma is generally treated as a fluid and thus general relativistic magnetohydrodynamic (GRMHD) equations are solved, which include magnetic field and radiation.
Left Panel: Top - Artist diagram of accretion disk accreting matter from a companion star Bottom- EHT image of M87
Right panel: NASA image of accretion disk
Simulations
Simulations
Evolution of a magnetized torus of plasma around a black hole from time t=0 to t=1000 in units of rg/c .
(Color plots represent density while the white lines represent magnetic field lines)
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