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Original
1952
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Similar

C. Deffayet, X. Gao, D. A. Steer and G. Zahariade, “From k-essence to generalised Galileons”, Phys. Rev. D 84
Original
2011
Cited alongside, same era.
G. Gubitosi and E. V. Linder, “Purely Kinetic Coupled Gravity”, Phys. Lett. B 703
Original
2011
Cited alongside, same era.
T. Kobayashi, M. Yamaguchi and J. ’i. Yokoyama, “Generalized G-inflation: Inflation with the most general second-order field equations”, Prog. Theor. Phys. 126
Original
2011
Cited alongside, same era.
C. Charmousis, E. J. Copeland, A. Padilla and P. M. Saffin, “Self-tuning and the derivation of a class of scalar-tensor theories”, Phys. Rev. D 85
Original
2012
Cited alongside, same era.
E. J. Copeland, A. Padilla and P. M. Saffin, “The cosmology of the Fab-Four”, JCAP 1212

Then

E. V. Linder, “How Fabulous Is Fab 5 Cosmology?”, JCAP 1312
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2013
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C. de Rham, “Massive Gravity”, Living Rev. Rel. 17
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2014
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M. Zumalacárregui and J. García-Bellido, “Transforming gravity: from derivative couplings to matter to second-order scalar-tensor theories beyond the Horndeski Lagrangian”, Phys. Rev. D 89
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2014
Later among the works it cites.
X. Gao, “Unifying framework for scalar-tensor theories of gravity”, Phys. Rev. D 90
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2014
Later among the works it cites.
X. Gao, “Hamiltonian analysis of spatially covariant gravity”, Phys. Rev. D 90
Original

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2015

Horndeski theories self-tuning to a de Sitter vacuum

Martin-Moruno, Prado, Nunes, Nelson J., Lobo, Francisco S. N.

Understand

We consider Horndeski cosmological models able to screen the vacuum energy coming from any field theory assuming that after this screening the space should be in a de Sitter vacuum with a particular value of the cosmological constant specified by the theory of gravity itself.

The most general scalar-tensor cosmological models without higher than second order derivatives in the field equations that have a spatially flat de Sitter critical point for any kind of material content or vacuum energy are, therefore, presented.
These models could allow us to understand the current accelerated expansion of the universe as the result of a dynamical evolution towards a de Sitter attractor.