Does circumventing the curvature singularity of the Kerr black hole affects
    the timescale of the scalar cloud formation around it? By definition, the
    scalar cloud, forms a gravitational atom with hydrogen-like bound states, lying
    on the threshold of a massive scalar field’s superradiant instability regime
    (time-growing quasi-bound states) and beyond (time-decaying quasi-bound
    states). By taking a novel type of rotating hollow regular black hole proposed
    by Simpson and Visser which unlike its standard rivals has an asymptotically
    Minkowski core, we address this question. The metric has a minimal extension
    relative to the standard Kerr, originating from a single regularization
    parameter $\ell$, with length dimension. We show with the inclusion of the
    regularization length scale $\ell$ into the Kerr spacetime, without affecting
    the standard superradiant instability regime, the timescale of scalar cloud
    formation gets shorter. Since the scalar cloud after its formation, via energy
    dissipation, can play the role of a continuum source for gravitational waves,
    such a reduction in the instability growth time improves the phenomenological
    detection prospects of new physics because the shorter the time, the more
    astrophysically important.

    Source link


    Leave A Reply