http://arxiv.org/abs/1701.07444
The detection of gravitational waves from black hole (BH) mergers provides an inroad toward probing the interior of astrophysical BHs. The general-relativistic description of a BH’s interior is that of empty spacetime with a (possibly) super-dense core. Recently, however, the hypothesis that the BH interior does not exist has been gaining traction, as it provides a means for resolving the BH information-loss problem. Here, we propose a simple method for answering the question: Does the BH interior exist and, if so, does it contain some distribution of matter or is it mostly empty? Our proposal is premised on the idea that, similar to the case of relativistic, ultra-compact stars, any BH-like object whose interior has some matter distribution should support fluid modes in addition to the conventional and universally present spacetime modes. In particular, the Coriolis-induced Rossby (r-) modes, whose spectrum is mostly insensitive to the composition of the interior matter, should be a universal feature of a BH-like object. In fact, the characteristic properties of these modes are determined by only the object’s mass and speed of rotation. The r-modes oscillate at a lower frequency, decay at a slower rate and produce weaker gravitational waves than do those of the spacetime class. Hence, they imprint a model-independent signature of a non-empty interior in the gravitational-wave spectrum resulting from a BH merger.
R. Brustein and A. Medved
Fri, 27 Jan 17
31/54
Comments: 21 pages, 1 figure
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