Ergosphere-driven winds

Punsly, Brian; Coroniti, F. V.

doi:10.1086/168717

Cited by 105 publications

(116 citation statements)

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“…This temporal evolution is repeated quasiperiodically. Similar cycles of vertical flux accretion/expulsion near black holes was anticipated in Punsly & Coroniti (1990) and is discussed in Chapter 8 of Punsly (2008).…”

Section: The Three-dimensional Resultssupporting

confidence: 64%

“…Type-III field line that is illustrated in Figure 8 was extracted from the jet in Figures 4 and 5. This was the type of vertical field line that had been expected to occur in equatorial accretion flows near black holes in simplified theoretical discussions (Thorne et al 1986;Punsly & Coroniti 1990;Punsly 2008). Surprisingly, this turns out to be the rarest type of field line that we encountered in KDJ.…”

Section: Vertical Field Line Taxonomymentioning

confidence: 63%

“…Consequently, there is a poloidal Poynting (2008) it was shown that the Poynting jet that is driven from the inner edge of the accretion is tantamount to the high accretion rate analog of the "ergospheric disk" jet that was first described in Punsly & Coroniti (1990).…”

Section: The Time Slice T = 9840mmentioning

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 Three-dimensional Resultssupporting

confidence: 64%

Section: Vertical Field Line Taxonomymentioning

confidence: 63%

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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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“…The magnetically driven part of the mechanism is the same as that of Uchida & Shibta [29] and Shibata & Uchida [30]. Punsly & Coroniti (1990) proposed an alternative magnetic force driven mechanism of the relativistic jet formation. They considered the magnetic tension causes the azimuthal velocity to produce the jet due to centrifugal force like the model of non-relativistic jet formation from the accretion disk [31].…”

Section: Resultsmentioning

confidence: 99%

Jet Propulsion Laboratory

2015

Encyclopedia of Astrobiology

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Recent observations of Galactic Black Hole Candidates (BHCs) suggest that those that are superluminal jet sources have more rapid black hole spin rates than otherwise normal BHCs. This provides observational support for models of relativistic jet formation that extract rotational energy of the central black hole. To investigate this mechanism, we have developed a new general relativistic magnetohydrodynamic code in Kerr geometry. Here we report on the first numerical simulation of the formation of a relativistic jet in a rapidly-rotating (a = 0.95) Kerr black hole magnetosphere. We assume that the initial velocity of the disk is zero. We find that the maximum velocity of the jet reaches 0.93c (Lorentz factor, 2.7) and the terminal velocity of the jet is 0.85c (Lorentz factor, 1.9). On the other hand, for a non-rotating (a = 0) Schwarzschild black hole, the maximum jet velocity is less than 0.6c as far as we calculated with the similar condition of the magnetosphere to that of the Kerr black hole case. These numerical results show the importance of the rapidly rotating black hole for the relativistic jet formation clearly.

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“…The first alternative was invented by Punsly and Coroniti [29,30] and elaborated by Punsly (1996). It has also been recently discussed by Li [18].…”

Section: Field Lines Anchored Outside the Horizon Closed At Infinmentioning

confidence: 99%

Magnetic extraction of spin energy from a black hole

Krolik¹

2001

AIP Conference Proceedings

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Abstract.Numerous variations have been proposed on the original suggestion by Blandford and Znajek that magnetic fields could be used to extract rotational energy from black holes. A new categorization of these variations is proposed so that they may be considered in a systematic way. "Black hole spindown" is defined more precisely, distinguishing decrease in the spin parameter a/M from decreases in angular momentum a and rotational kinetic energy, M − M i . Several key physical questions are raised: Can the "stretched horizon" of a black hole communicate with the outside world? Do accretion disks bring any net magnetic flux to the black holes at their centers? Is the magnetic field adjacent to a black hole force-free everywhere?

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Ergosphere-driven winds

Cited by 105 publications

References 0 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

Jet Propulsion Laboratory

Magnetic extraction of spin energy from a black hole

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