Superradiance evolution of black hole shadows revisited

Abstract

Black hole (BH) shadows can be used to probe new physics in the form of ultra-light particles via the phenomenon of superradiant instability. By directly affecting the BH mass and spin, superradiance can lead to a time evolution of the BH shadow, which nonetheless has been argued to be unobservable through Very Long Baseline Interferometry (VLBI) over realistic observation timescales. We revisit the superradiance-induced BH shadow evolution including the competing effects of gas accretion and gravitational wave (GW) emission and, as a first step towards modelling realistic new physics scenarios which predict the existence of multiple ultra-light species, we study the system in the presence of two ultra-light bosons, whose combined effect could help reducing the shadow evolution timescale. We find that accretion and GW emission play a negligible role in our results (justifying previous simplified analyses), and that contrary to our intuition the inclusion of an additional ultra-light boson does not shorten the BH shadow evolution timescale and hence improve detection prospects. However, we point out an important subtlety concerning the observationally meaningful definition of the superradiance-induced BH shadow evolution timescale, which reduces the latter by about an order of magnitude, opening up the possibility of observing the superradiance-induced BH shadow evolution with upcoming VLBI arrays, provided angular resolutions just below the $\mu \mathrm{as}$ level can be reached. As a concrete example, we show that the angular size of the shadow of SgrA${}^{\ast }$ can change by up to $0.6\mu \mathrm{as}$ over a period as short as $16$ years, which further strengthens the scientific case for targeting the shadow of SgrA${}^{\ast }$ with next-generation VLBI arrays.

20 pages, 11 sub-figures arranged in 3 figures. Minor modifications, improved legibility of contour plots, added discussions on backreaction and possibility of processes discussed taking place more than once over the lifetime of the BH. Version accepted for publication in PRD

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