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Article overview
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Characterization of the production of intense Alfv'en pulses : GRMHD simulation of black hole accretion disks | | Akira Mizuta
; Toshikazu Ebisuzaki
; Toshiki Tajima
; Shigehiro Nagataki
; | | Date: |
27 Jul 2017 | | Abstract: | The episodic dynamics of the magnetic eruption of a spinning black hole (BH)
accretion disks and its associated intense shapeup of their jets is studied via
three-dimensional general-relativistic magnetohydrodynamics (GRMHD). The
embedded magnetic fields in the disk get amplified by the magnetorotational
instability (MRI) so large as to cause an eruption of magnetic field
(recconection) and large chunks of matter episodically accrete toward the roots
of the jets upon such an event. We also find that the eruption events produce
intensive Alfv’en pulses, which propagate through the jets. After the
eruption, the disk backs to the weakly magnetic states. Such disk activities
cause short time variabilities in mass accretion rate at the event horizon as
well as electric-magnetic luminosity inside the jet. Since the dimensionless
strength parameter $a_0=eE/m_e omega_{
m A}c$ of these Alfv’en wave pulses
is extremely high $sim 10^{10}$ for the $10^8$ solar masses central black hole
and $10$\% Eddington accretion rate accretion flow, the bow wake acceleration
model proposed by Ebisuzaki & Tajima (2014) certainly works to accelerate the
ultra-high energy cosmic rays and electrons which finally emit gamma-rays.
Since our GRMHD model has universality in its spatial and temporary scales, it
is applicable to a wide range of astrophysical objects ranging from those of
AGN (which is the primary target of this research), to micro-quasars, and down
to young stellar objects. Properties such as time variabilities of blazar
gamma-ray flares and spectrum observed by {it Fermi} Gamma-ray Observatory are
well explained by linear acceleration of electrons by the bow wake. | | Source: | arXiv, 1707.8799 | | Services: | Forum | Review | PDF | Favorites | |
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