Built on

C. Deffayet, S. Deser, and G. Esposito-Farese, “Generalized Galileons: All scalar models whose curved background extensions maintain second-order field equations and stress-tensors,” Phys.Rev
Original
1967
Earlier work this paper cites.
G. W. Horndeski, “Second-order scalar-tensor field equations in a four-dimensional space,” International Journal of Theoretical Physics
1974
Earlier work this paper cites.
C. A. Kolassis, N. O. Santos, and D. Tsoubelis, “Energy conditions for an imperfect fluid,” Classical and Quantum Gravity
1988
Earlier work this paper cites.
A. A. Starobinsky, “Future and origin of our universe: Modern view,” Grav.Cosmol
2000
Earlier work this paper cites.
R. Caldwell, “A Phantom menace?,” Phys.Lett
2002
Earlier work this paper cites.
R. R. Caldwell, M. Kamionkowski, and N. N. Weinberg, “Phantom energy and cosmic doomsday,” Phys.Rev.Lett
2003
Earlier work this paper cites.
S. M. Carroll, M. Hoffman, and M. Trodden, “Can the dark energy equation - of - state parameter w be less than -1?,” Phys.Rev
2003
Earlier work this paper cites.
Cambridge University Press, 2005
V. Mukhanov, Physical foundations of cosmology · 2005
Earlier work this paper cites.
S. Dubovsky, T. Gregoire, A. Nicolis, and R. Rattazzi, “Null energy condition and superluminal propagation,” JHEP
2006
Earlier work this paper cites.

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Then

T. Kobayashi, M. Yamaguchi, and J. Yokoyama, “Generalized G-inflation: Inflation with the most general second-order field equations,” Prog.Theor.Phys
Original
2011
Later among the works it cites.
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2011
Later among the works it cites.
D. A. Easson, I. Sawicki, and A. Vikman, “G-Bounce,” JCAP
Original
2011
Later among the works it cites.
O. Pujolas, I. Sawicki, and A. Vikman, “The Imperfect Fluid behind Kinetic Gravity Braiding,” JHEP
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Later among the works it cites.
Supernova Cosmology Project
Original

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2012

Hidden Negative Energies in Strongly Accelerated Universes

Sawicki, Ignacy, Vikman, Alexander

Understand

We point out that theories of cosmological acceleration which have equation of state, w, such that 1+w is small but positive may still secretly violate the null energy condition.

This violation implies the existence of observers for whom the background has infinitely negative energy densities, despite the fact that the perturbations are free of ghosts and gradient instabilities.

Built on

C. Deffayet, S. Deser, and G. Esposito-Farese, “Generalized Galileons: All scalar models whose curved background extensions maintain second-order field equations and stress-tensors,” Phys.Rev
Original
1967
Earlier work this paper cites.
G. W. Horndeski, “Second-order scalar-tensor field equations in a four-dimensional space,” International Journal of Theoretical Physics
1974
Earlier work this paper cites.
C. A. Kolassis, N. O. Santos, and D. Tsoubelis, “Energy conditions for an imperfect fluid,” Classical and Quantum Gravity
1988
Earlier work this paper cites.
A. A. Starobinsky, “Future and origin of our universe: Modern view,” Grav.Cosmol
2000
Earlier work this paper cites.
R. Caldwell, “A Phantom menace?,” Phys.Lett
2002
Earlier work this paper cites.
R. R. Caldwell, M. Kamionkowski, and N. N. Weinberg, “Phantom energy and cosmic doomsday,” Phys.Rev.Lett
2003
Earlier work this paper cites.
S. M. Carroll, M. Hoffman, and M. Trodden, “Can the dark energy equation - of - state parameter w be less than -1?,” Phys.Rev
2003
Earlier work this paper cites.
Cambridge University Press, 2005
V. Mukhanov, Physical foundations of cosmology · 2005
Earlier work this paper cites.
S. Dubovsky, T. Gregoire, A. Nicolis, and R. Rattazzi, “Null energy condition and superluminal propagation,” JHEP
2006
Earlier work this paper cites.