Slowly-rotating curved acoustic black holes: Quasinormal modes, Hawking-Unruh radiation and quasibound states

TL;DR

This paper studies sound wave behavior in a new class of slowly-rotating acoustic black holes, analyzing quasinormal modes, Hawking-Unruh radiation, and quasibound states to better understand black hole physics through analog models.

Contribution

It introduces a novel metric for slowly-rotating acoustic black holes and investigates their quasinormal modes, radiation, and bound states, linking analog models to astrophysical black holes.

Findings

Derived perturbative solutions for sound waves in curved acoustic black holes.

Analyzed quasinormal mode frequencies and their implications.

Explored Hawking-Unruh radiation and quasibound states in the model.

Abstract

Astrophysical black holes are generally surrounded by accretion disks, galactic matter and the omnipresent cosmic microwave background radiation, thus allowing for the concurrent propagation of both gravitational and sound waves. Recently, acoustic black holes were embedded in Schwarzschild spacetime allowing for the coexistence of event and acoustic horizons. Here, we obtain a class of perturbative solutions to the field equations of the relativistic Gross-Pitaevskii and Yang-Mills theories, which describe sound waves propagating on a curved slowly-rotating acoustic black hole, akin to Lense-Thirring spacetime. We investigate the quasinormal mode frequencies, Hawking-Unruh radiation, and quasibound states. Our novel metric mimics the gravitational field of astrophysical compact objects in the limiting case of slow rotation, and therefore could, in principle, shed more light into the underlying classical and quantum physics of black holes through analog acoustic probes.