General relativistic magnetohydrodynamic simulations of monopole magnetospheres of black holes

Komissarov, S. S.

doi:10.1111/j.1365-2966.2004.07738.x

Cited by 145 publications

(165 citation statements)

References 30 publications

(55 reference statements)

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“…When the field attains this "hourglass" topology, the plasma is allowed to accrete freely into the black hole in the radial direction by just sliding along the field lines. Recall that the same situation occurred in the two-dimensional simulation of Komissarov (2004) that was discussed in the previous section.…”

Section: The Two-dimensional Resultsmentioning

confidence: 94%

“…In many respects, the works of Igumenshchev (2008), Komissarov (2004), and Komissarov & McKinney (2007) have crystalized the discussion of the vertical flux near black holes into a simple topological dichotomy: is the astrophysical state an "hourglass" topology (right frame of Igumenshchev (2008). The topology of the right frame, Figure 1(b), is the "hourglass" shape that has a very little vertical flux penetrating the equatorial plane near the event horizon.…”

Section: A Fundamental Topological Issuementioning

confidence: 99%

“…Another line of two-dimensional research was initiated in Komissarov (2004). He explored the l = 1, m = 0, vacuum field solution of Maxwell's equations on a black hole background (known as the Wald solution) after it was filled with a diffuse plasma.…”

Section: A Fundamental Topological Issuementioning

confidence: 99%

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Three-Dimensional Simulations of Vertical Magnetic Flux in the Immediate Vicinity of Black Holes

Punsly

Igumenshchev

Hirose

2009

ApJ

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This article reports on three-dimensional MHD simulations of non-rotating and rapidly rotating black holes and the adjacent black hole accretion disk magnetospheres. A particular emphasis is placed on the vertical magnetic flux that is advected inward from large radii and threads the equatorial plane near the event horizon. In both cases of non-rotating and rotating black holes, the existence of a significant vertical magnetic field in this region is like a switch that creates powerful jets. There are many similarities in the vertical flux dynamics in these two cases in spite of the tremendous enhancement of azimuthal twisting of the field lines and enhancement of the jet power because of an "ergospheric disk" in the Kerr metric. A three-dimensional approach is essential because two-dimensional axisymmetric flows are incapable of revealing the nature of the vertical flux near a black hole. Poloidal field lines from the ergospheric accretion region have been visualized in three dimensions and much of the article is devoted to a formal classification of the different manifestations of the vertical flux in the Kerr case.

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Section: The Two-dimensional Resultsmentioning

confidence: 94%

Section: A Fundamental Topological Issuementioning

confidence: 99%

See 1 more Smart Citation

Three-Dimensional Simulations of Vertical Magnetic Flux in the Immediate Vicinity of Black Holes

Punsly

Igumenshchev

Hirose

2009

ApJ

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“…In particular, it is worth to mention that Refs. [19][20][21][22][23] have recently presented implementations for which detailed tests have been carried out for confirmation of the reliability of their computation, in contrast with the attitude in an early work [17]. They are applied for simulating magnetorotational instability (MRI) of accretion disks and subsequently induced winds and jets around black holes and neutron stars.…”

Section: Introductionmentioning

confidence: 99%

“…In the past decade, numerical implementations for GRMHD simulation in the fixed gravitational field have been extensively developed (e.g., [18,17,[19][20][21][22][23][24]). In particular, it is worth to mention that Refs.…”

Section: Introductionmentioning

confidence: 99%

Magnetohydrodynamics in full general relativity: Formulation and tests

2005

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A new implementation for magnetohydrodynamics (MHD) simulations in full general relativity (involving dynamical spacetimes) is presented. In our implementation, Einstein's evolution equations are evolved by a BSSN formalism, MHD equations by a high-resolution central scheme, and induction equation by a constraint transport method. We perform numerical simulations for standard test problems in relativistic MHD, including special relativistic magnetized shocks, general relativistic magnetized Bondi flow in stationary spacetime, and a longterm evolution for self-gravitating system composed of a neutron star and a magnetized disk in full general relativity. In the final test, we illustrate that our implementation can follow winding-up of the magnetic field lines of magnetized and differentially rotating accretion disks around a compact object until saturation, after which magnetically driven wind and angular momentum transport inside the disk turn on.04.25. Dm, 04.40.Nr, 47.75.+f, 95.30.Qd

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Cosmic black holes - from stellar to supramassive black holes in galaxies

Camenzind¹

2006

Ann. Phys.

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The collapse of massive stars produces the most bizarre objects in the Universe. In the last ten years, astronomers have been successfully searching for real black holes in the Universe. Black hole astrophysics began in the 1960s with the discovery of quasars and other active galactic nuclei (AGN) in distant galaxies. Already in the 1960s it became clear that the most natural explanation for the quasar activity is the release of gravitational energy through accretion of gas onto supermassive black holes. The remnants of this activity have now been found in the centers of about 50 nearby galaxies. BH astrophysics received a new twist in the 1970s with the discovery of the X-ray binary Cygnus X-1. The X-ray emitting compact object was too massive to be explained by a neutron star. Today, about 20 excellent BH candidates are known in XRBs. On the extragalactic scale, more than 100,000 quasars have been found in large galaxy surveys. At the redshift of the most distant ones, the Universe was younger than one billion year. The most enigmatic black hole candidates identified in the last years are the compact objects behind the Gamma-Ray Bursters. The formation of all these types of black holes is accompanied by extensive emission of gravitational waves. The detection of these strong gravity events is one of the biggest challenges for physicists in the near future. Milestones in the history of black hole physicsBlack holes are the most bizarre objects in the Universe. Though they are black by definition (their horizon cannot emit any particles), they become visible in astronomical observations when matter is swallowed by the horizon. Due to the deep gravitational potential near the horizon, most of this radiation is emitted in Xand gamma-rays.Einstein and Schwarzschild. Black holes are the simplest objects one can think of within Einstein's theory of gravity. As Chandrasekhar [9] summarized in 1983, we need for their construction only the concepts of space and time. The source of gravity is ultimately a singularity hidden behind the event horizon. No equation of state for any matter is necessary for their understanding. Shortly after Einstein and Hilbert formulated the field equations for the gravitational field, Schwarzschild found already in 1916 the vacuum solution for nonrotating objects. In this solution, a scaling radius appears, known as the Schwarzschild radiuswhich sets the smallest radius for an object of given mass M . Neutron stars have radii bigger than about 2.5 Schwarzschild radii. Extending the Schwarzschild solution towards radii smaller than R S , opens up the branch of the nonrotating black holes with the Schwarzschild radius as the dimension of the horizon of the black hole. The surface r = R S defines a horizon from which no form of matter can escape to infinity.

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General relativistic magnetohydrodynamic simulations of monopole magnetospheres of black holes

Cited by 145 publications

References 30 publications

Three-Dimensional Simulations of Vertical Magnetic Flux in the Immediate Vicinity of Black Holes

Three-Dimensional Simulations of Vertical Magnetic Flux in the Immediate Vicinity of Black Holes

Magnetohydrodynamics in full general relativity: Formulation and tests

Cosmic black holes - from stellar to supramassive black holes in galaxies

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