On Reflectivity of Quantum Black Hole Horizons. (arXiv:1905.00464v1 [hep-th])
<a href="http://arxiv.org/find/hep-th/1/au:+Oshita_N/0/1/0/all/0/1">Naritaka Oshita</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Wang_Q/0/1/0/all/0/1">Qingwen Wang</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Afshordi_N/0/1/0/all/0/1">Niayesh Afshordi</a>
We study the reflectivity of quantum black hole (BH) horizons using detailed
balance and fluctuation-dissipation theorem, finding a universal flux
reflectivity given by the Boltzmann factor ${mathcal R} = expleft(-{hbar
|omega| over k T_{rm H}}right)$, where $omega$ is frequency in the horizon
frame and $T_{rm H}$ is the Hawking temperature. This implies CP-symmetry (or
$bf{RP}^3$ topology) of the extended BH spacetime. We then briefly discuss
related physical implications: We predict echoes in the ringdown of Kerr BHs,
but they do not exhibit ergoregion instability. The viscosity in the membrane
paradigm is modified to $eta = frac{c^3}{16pi G}tanhleft({hbar |omega|
over 4 k T_{rm H}}right)$, only approaching General Relativistic value at
high frequencies.
We study the reflectivity of quantum black hole (BH) horizons using detailed
balance and fluctuation-dissipation theorem, finding a universal flux
reflectivity given by the Boltzmann factor ${mathcal R} = expleft(-{hbar
|omega| over k T_{rm H}}right)$, where $omega$ is frequency in the horizon
frame and $T_{rm H}$ is the Hawking temperature. This implies CP-symmetry (or
$bf{RP}^3$ topology) of the extended BH spacetime. We then briefly discuss
related physical implications: We predict echoes in the ringdown of Kerr BHs,
but they do not exhibit ergoregion instability. The viscosity in the membrane
paradigm is modified to $eta = frac{c^3}{16pi G}tanhleft({hbar |omega|
over 4 k T_{rm H}}right)$, only approaching General Relativistic value at
high frequencies.
http://arxiv.org/icons/sfx.gif
