Abstract
We study the quantum channel between two localized first-quantized systems that communicate in 3+1 dimensional Schwarzschild spacetime via a quantum field. We analyze the information carrying capacity of direct and black hole-orbiting null geodesics as well as of the timelike contributions that arise because the strong Huygens principle does not hold on the Schwarzschild background. We find, in particular, that the non-direct-null and timelike contributions, which do not possess an analog on Minkowski spacetime, can dominate over the direct null contributions. We cover the cases of both geodesic and accelerated emitters. Technically, we apply tools previously designed for the study of wave propagation in curved spacetimes to a relativistic quantum information communication setup, first for generic spacetimes, and then for the case of Schwarzschild spacetime in particular.
Highlights
Localized first-quantized systems that temporarily couple to a quantum field have been used extensively in a plethora of contexts in quantum field theory in flat and curved spacetimes
Since QL is a subregion of the maximal normal neighborhood, a QL region cannot include points connected by a null geodesic which has orbited around the black hole
The smooth decay is modulated by ripplelike features at certain distances from Alice. These features are caused exactly by null geodesics that orbit around the black hole before arriving at Bob’s detector, as we show in Sec
Summary
Localized first-quantized systems that temporarily couple to a quantum field have been used extensively in a plethora of contexts in quantum field theory in flat and curved spacetimes. There have been a number of recent studies analyzing communication using particle detectors coupling to quantum fields, starting with [21], both in flat spacetime [22,23,24,25,26,27,28,29] and curved [30,31] spacetimes. Among the results, it was shown, for example, that if there are multiple emitters, the choice of their entanglement can help shape their radiation field [29]. Ds2 1⁄4 −fdt þ f−1dr þ r2ðdθ þ sin θdφ2Þ; ð1Þ where f ≔ 1 − 2M=r
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