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Slowly balding black holes | | Maxim Lyutikov
; Jonathan C. McKinney
; | | Date: |
3 Sep 2011 | | Abstract: | The "no hair" theorem, a key result in General Relativity, states that an
isolated black hole is defined by only three parameters: mass, angular
momentum, and electric charge; this asymptotic state is reached on a
light-crossing time scale. We find that the "no hair" theorem is not formally
applicable for black holes formed from collapse of a rotating neutron star.
Rotating neutron stars can self-produce particles via vacuum breakdown forming
a highly conducting plasma magnetosphere such that magnetic field lines are
effectively "frozen-in" the star both before and during collapse. In the limit
of no resistivity, this introduces a topological constraint which prohibits the
magnetic field from sliding off the newly-formed event horizon. As a result,
during collapse of a neutron star into a black hole, the latter conserves the
number of magnetic flux tubes $N_B = e Phi_infty /(pi c hbar)$, where
$Phi_infty approx 2 pi^2 B_{NS} R_{NS}^3 /(P_{
m NS} c)$ is the initial
magnetic flux through the hemispheres of the progenitor and out to infinity. We
test this theoretical result via three-dimensional general relativistic plasma
simulations of rotating black holes that start with a neutron star dipole
magnetic field with no currents initially present outside the event horizon.
The black hole’s magnetosphere subsequently relaxes to the split monopole
magnetic field geometry with self-generated currents outside the event horizon.
The dissipation of the resulting equatorial current sheet leads to a slow loss
of the anchored flux tubes, a process that balds the black hole on long
resistive time scales rather than the short light-crossing time scales expected
from the vacuum "no-hair" theorem. | | Source: | arXiv, 1109.0584 | | Services: | Forum | Review | PDF | Favorites | |
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