Massive Scalar Field Evolution in the Dyadosphere Spacetime of Charged Black Hole

AbstractWe study massive scalar field perturbation on Kerr black holes in dynamical Chern–Simons gravity by performing a $$(2+1)$$ ( 2 + 1 ) -dimensional simulation. Object pictures of the wave dynamics in time domain are obtained. The tachyonic instability is found to always occur for any nonzero black hole spin and any scalar field mass as long as the coupling constant exceeds a critical value. The presence of the mass term suppresses or even quench the instability. The quantitative dependence of the onset of the tachyonic instability on the coupling constant, the scalar field mass and the black hole spin is given numerically.

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ENTROPY OF SCALAR FIELD NEAR A SCHWARZSCHILD BLACK HOLE HORIZON

International Journal of Modern Physics A ◽

10.1142/s0217751x06033805 ◽

2006 ◽

Vol 21 (30) ◽

pp. 6183-6190 ◽

Cited By ~ 3

Author(s):

M. R. SETARE

Keyword(s):

Black Hole ◽

Scalar Field ◽

Spherical Shell ◽

Polarization Effect ◽

Vacuum Polarization ◽

Mixed Boundary Condition ◽

Mixed Boundary ◽

Massive Scalar ◽

Schwarzschild Black Hole ◽

Massive Scalar Field

In this paper we compute the correction to the entropy of Schwarzschild black hole due to the vacuum polarization effect of massive scalar field. The Schwarzschild black hole is supposed to be confined in spherical shell. The scalar field obeying mixed boundary condition on the spherical shell.

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Massive scalar field quasinormal modes of a Schwarzschild black hole surrounded by quintessence

Open Physics ◽

10.2478/s11534-008-0056-7 ◽

2008 ◽

Vol 6 (2) ◽

Cited By ~ 8

Author(s):

Chunrui Ma ◽

Yuanxing Gui ◽

Wei Wang ◽

Fujun Wang

Keyword(s):

Black Hole ◽

Scalar Field ◽

Quasinormal Modes ◽

Massless Scalar ◽

Massless Scalar Field ◽

Massive Scalar ◽

Schwarzschild Black Hole ◽

Third Order ◽

Massive Scalar Field ◽

Absolute Value

AbstractWe present the quasinormal frequencies of the massive scalar field in the background of a Schwarzchild black hole surrounded by quintessence with the third-order WKB method. The mass of the scalar field u plays an important role in studying the quasinormal frequencies, the real part of the frequencies increases linearly as mass of the field u increases, while the imaginary part in absolute value decreases linearly which leads to damping more slowly than the massless scalar field. The frequencies have a limited value, so it is easier to detect the quasinormal modes. Moreover, owing to the presence of the quintessence, the massive scalar field damps more slowly.

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A new spin on black hole hair

International Journal of Modern Physics D ◽

10.1142/s0218271814420140 ◽

2014 ◽

Vol 23 (12) ◽

pp. 1442014 ◽

Cited By ~ 71

Author(s):

Carlos A. R. Herdeiro ◽

Eugen Radu

Keyword(s):

Black Holes ◽

General Relativity ◽

Black Hole ◽

Scalar Field ◽

Massive Scalar ◽

Massive Scalar Field ◽

Hairy Black Holes ◽

Scalar Hair

We show that scalar hair can be added to rotating, vacuum black holes (BHs) of general relativity. These hairy black holes (HBHs) clarify a lingering question concerning gravitational solitons: Whether a BH can be added at the centre of a boson star (BS), as it typically can for other solitons. We argue that it can, but only if it is spinning. The existence of such HBHs is related to the Kerr superradiant instability triggered by a massive scalar field. This connection leads to the following conjecture: a (hairless) BH, which is afflicted by the superradiant instability of a given field, must allow hairy generalizations with that field.

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