Black holes in our Universe are rarely truly isolated, being instead embedded in astrophysical environments such as plasma or dark matter. A particularly intriguing possibility is that light scalar fields form bound states around black holes, producing extended “clouds” known as gravitational atoms. When these clouds become sufficiently compact, the spacetime can no longer be described by a vacuum solution of general relativity. In this regime, one can construct quasistationary, spherically symmetric, self-gravitating scalar gravitational atom configurations. Here, we explore an observationally relevant aspect of these systems by computing their fundamental quasinormal mode. We present a fully relativistic calculation of the axial modes in both the time and frequency domains, finding frequency shifts relative to the vacuum case that depend mostly on the compactness of the gravitational atom. For sufficiently compact configurations, these shifts may be detectable by current or future gravitational wave detectors.
Gravitational atom spectroscopy
Della Rocca, Matteo;Gualtieri, Leonardo;
2026-01-01
Abstract
Black holes in our Universe are rarely truly isolated, being instead embedded in astrophysical environments such as plasma or dark matter. A particularly intriguing possibility is that light scalar fields form bound states around black holes, producing extended “clouds” known as gravitational atoms. When these clouds become sufficiently compact, the spacetime can no longer be described by a vacuum solution of general relativity. In this regime, one can construct quasistationary, spherically symmetric, self-gravitating scalar gravitational atom configurations. Here, we explore an observationally relevant aspect of these systems by computing their fundamental quasinormal mode. We present a fully relativistic calculation of the axial modes in both the time and frequency domains, finding frequency shifts relative to the vacuum case that depend mostly on the compactness of the gravitational atom. For sufficiently compact configurations, these shifts may be detectable by current or future gravitational wave detectors.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
