Breit-Wigner resonances and the quasinormal modes of anti-de Sitter black holes

Understand

The purpose of this short communication is to show that the theory of Breit-Wigner resonances can be used as an efficient numerical tool to compute black hole quasinormal modes.

• For illustration we focus on the Schwarzschild anti-de Sitter (SAdS) spacetime.
• The resonance method is better suited to small SAdS black holes than the traditional series expansion method, allowing us to confirm that the damping timescale of small SAdS black holes for scalar and gravitational fields is proportional to r_+^(-2l-2), where r_+ is the horizon radius.
• The proportionality coefficients are in good agreement with analytic calculations.