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We investigate a scenario where quantum correlations affect the gravitational field.
Vacuum expectation value of the stress tensor in an arbitrary curved background: The covariant point-separation method
S. M. Christensen · 1976
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Effective-potential approach to graviton production in the early universe
J. B. Hartle · 1977
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The back reaction effect in particle creation in curved spacetime
Robert M. Wald · 1977
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Cosmology for grand unified theories with radiatively induced symmetry breaking
Andreas Albrecht and Paul J. Steinhardt · 1982
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Effects of quantum fields on singularities and particle horizons in the early universe
Paul Anderson · 1983
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Nicholas David Birrell and Paul Charles William Davies · 1984
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A single atomic particle forever floating at rest in free space: New value for electron radius
Hans Dehmelt · 1988
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Charles H. Bennett, Gilles Brassard, Claude Crépeau, Richard Jozsa, Asher Peres, and William K. Wootters · 1993
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Roger Penrose · 1996
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T. D. Ladd, F. Jelezko, R. Laflamme, Y. Nakamura, C. Monroe, and J. L. O’Brien · 2010
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Observer-dependent entanglement
Paul M Alsing and Ivette Fuentes · 2012
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Angelo Bassi, Kinjalk Lochan, Seema Satin, Tejinder P. Singh, and Hendrik Ulbricht · 2013
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Secure quantum key distribution
Hoi-Kwong Lo, Marcos Curty, and Kiyoshi Tamaki · 2014
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Spacetime effects on satellite-based quantum communications
David Edward Bruschi, Timothy C. Ralph, Ivette Fuentes, Thomas Jennewein, and Mohsen Razavi · 2014
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In this paper we will use the natural convention c = ℏ = k B = 1 c=\hbar=k_{B}=1 and we use Einstein’s summation convention. The metric has signature ( − , + , + , + ) (-,+,+,+)
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We note that in 2 + 1 2+1 dimensions there are contributions to Einstein’s tensor that do not decay in time i.e., those for which | 𝐱 | ∼ t |\mathbf{x}|\sim t
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Experimental satellite quantum communications
Giuseppe Vallone, Davide Bacco, Daniele Dequal, Simone Gaiarin, Vincenza Luceri, Giuseppe Bianco, and Paolo Villoresi · 2015
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