Decay of massive scalar hair in the background of a black hole with a global monopole

Abstract

The late-time tail behaviors of massive scalar fields are examined analytically in the background of a black hole with a global monopole. It is found that the presence of a solid deficit angle in the background metric makes the massive scalar fields decay faster in the intermediate times. However, the asymptotically late-time tail is not affected and it has the same decay rate of t −5/6 as in the Schwarzschild and nearly extreme Reissner-Nordström backgrounds.

Accretion on Reissner–Nordström–(anti)-de Sitter black hole with global monopole

“…Thus, we note that R is linear and P is quadratic in r, so each term P + R and P − R is quadratic. Therefore, solving these quadratic formulas one can give all four solutions to the original quartic equation (15). The cubic equation (17) can be simplified by making the substitution x = y + a 1 /3.…”

“…Barriola and Vilenkin found the approximate solution of the Einstein equations for the static spherically symmetric black hole with a global monopole [12]. Several other authors have also studied the physical properties of the black holes with global monopoles [14,15,17,16]. In the absence of the electric charge Q and the cosmological constant Λ, Letelier [18] obtained the metric representing the black hole spacetime with a spherical mass M centered at the origin of the system of coordinates, surrounded by a spherical cloud of strings.…”

Absorption and scattering of a black hole with a global monopole in f(R) gravity

“…Black holes are exact solutions of Einstein equations which are determined by mass (M ), electric charge (Q) and angular momentum (J) [1,2] and plays an important role in modern physics. In particular, black hole with a global monopole has been explored extensively by many authors in recent years [3][4][5][6][7] and the metric for this kind of black hole was determined by Barriola and Vilenkin [8]. The global monopoles are topological defects that arise in gauge theories due to the spontaneous symmetry breaking of the original global O(3) symmetry to U (1) [9,10].…”

Dynamical evolution of electromagnetic perturbation in the background of a scalar hairy black hole in Horndeski theory

“…For the massive perturbations, the late-time tails are dominated by the oscillations with inverse power-law form t −(l+3/2) sin µt in the intermediate late time [17][18][19]. However, in the spacetimes with a deficit solid angle ( caused by global monopole [20], cosmic string [21] or tensional brane [22] ), it is found that the late-time tails of perturbations also depend on the symmetry breaking scale.…”