General Relativistic Simulations of Early Jet Formation in a Rapidly Rotating Black Hole Magnetosphere

2000 ◽  
Vol 536 (2) ◽  
pp. 668-674 ◽  
Author(s):  
Shinji Koide ◽  
David L. Meier ◽  
Kazunari Shibata ◽  
Takahiro Kudoh
Keyword(s):  
Black Hole ◽  
Jet Formation ◽  
Rotating Black Hole ◽  
General Relativistic

scholarly journals General Relativistic Simulation of Jet Formation from Magnetized Accretion Disk

1997 ◽  
Vol 163 ◽  
pp. 667-671
Author(s):  
Shinji Koide ◽  
Kazunari Shibata ◽  
Takahiro Kudoh
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Accretion Disk ◽  
Galactic Nuclei ◽  
Lorentz Factor ◽  
Numerical Code ◽  
Jet Formation ◽  
Relativistic Jet ◽  
Relativistic Regime ◽  
General Relativistic

AbstractRecently, superluminal motions are observed not only from active galactic nuclei but also in our Galaxy. These phenomena are explained as relativistic jets propagating almost toward us with Lorentz factor more than 2. For the formation of such a relativistic jet, magnetically driven mechanism around a black hole is most promising. We have extended the 2.5D Newtonian MHD jet model (Shibata & Uchida 1986) to general relativistic regime. For this purpose, we have developed a general relativistic magnetohydrodynamic (GRMHD) numerical code and applied it to the simulation of the magnetized accretion disk around a black hole. We have found the formation of magnetically driven jets with 86 percent of light velocity (i.e. Lorentz factor ~ 2.0).

scholarly journals General Relativistic Magnetohydrodynamic Simulations of Collapsars: Rotating Black Hole Cases

2004 ◽  
Vol 615 (1) ◽  
pp. 389-401 ◽  
Author(s):  
Yosuke Mizuno ◽  
Shoichi Yamada ◽  
Shinji Koide ◽  
Kazunari Shibata
Keyword(s):  
Black Hole ◽  
Rotating Black Hole ◽  
General Relativistic ◽  
Magnetohydrodynamic Simulations

scholarly journals QUASI-PERIODIC OSCILLATIONS AND FREQUENCIES IN AN ACCRETION DISK AND COMPARISON WITH THE NUMERICAL RESULTS FROM NON-ROTATING BLACK HOLE COMPUTED BY THE GRH CODE

2007 ◽  
Vol 22 (02) ◽  
pp. 141-157 ◽  
Author(s):  
ORHAN DONMEZ
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Numerical Results ◽  
Pressure Gradients ◽  
Periodic Oscillations ◽  
Rotating Black Hole ◽  
Accretion Flows ◽  
Numerical Result ◽  
General Relativistic ◽  
Physical Phenomena

The shocked wave created on the accretion disk after different physical phenomena (accretion flows with pressure gradients, star-disk interaction etc.) may be responsible observed Quasi Periodic Oscillations (QPOs) in X-ray binaries. We present the set of characteristics frequencies associated with accretion disk around the rotating and non-rotating black holes for one particle case. These persistent frequencies are results of the rotating pattern in an accretion disk. We compare the frequency's from two different numerical results for fluid flow around the non-rotating black hole with one particle case. The numerical results are taken from Refs. 1 and 2 using fully general relativistic hydrodynamical code with non-selfgravitating disk. While the first numerical result has a relativistic tori around the black hole, the second one includes one-armed spiral shock wave produced from star-disk interaction. Some physical modes presented in the QPOs can be excited in numerical simulation of relativistic tori and spiral waves on the accretion disk. The results of these different dynamical structures on the accretion disk responsible for QPOs are discussed in detail.

scholarly journals Numerical Simulation of Relativistic Jet Formation in Black Hole Magnetosphere

1998 ◽  
Vol 188 ◽  
pp. 415-416 ◽  
Author(s):  
Shinji Koide ◽  
Kazunari Shibata ◽  
Takahiro Kudoh
Keyword(s):  
Black Hole ◽  
Galactic Nuclei ◽  
Apparent Velocity ◽  
Jet Formation ◽  
Radio Jets ◽  
Relativistic Jet ◽  
Superluminal Motion ◽  
Protostellar Jets ◽  
General Relativistic ◽  
Magnetic Mechanism

The radio jets ejected from active galactic nuclei (AGNs) sometimes show proper motions with apparent velocity exceeding the speed of light. This phenomenon, called superluminal motion, is explained as relativistic jets propagating in a direction almost toward us, and has been thought to be ejected from the close vicinity of hypothetical supermassive black holes powering AGNs (Rees 1996). The magnetic mechanism has been proposed not only for AGN jets (Lovelace 1976; Blandford & Payne 1983) but also for protostellar jets (Pudritz & Norman 1986; Uchida & Shibata 1985; Shibata & Uchida 1986), although no one has yet performed nonsteady general relativistic magnetohydrodynamic (GRMHD) numerical simulations on the formation of jets from the accretion disk around a black hole.

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