Effective field theory approach to modified gravity including Horndeski theory and Hořava–Lifshitz gravity
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Publication:5252779
DOI10.1142/S0218271814430081zbMath1314.83057arXiv1409.1984OpenAlexW3102879326MaRDI QIDQ5252779
Ryotaro Kase, Shinji Tsujikawa
Publication date: 3 June 2015
Published in: International Journal of Modern Physics D (Search for Journal in Brave)
Full work available at URL: https://arxiv.org/abs/1409.1984
Relativistic cosmology (83F05) Relativistic gravitational theories other than Einstein's, including asymmetric field theories (83D05) Equations of motion in general relativity and gravitational theory (83C10)
Related Items (15)
Effective field theory of dark energy: a review ⋮ Stability of scalar perturbations in scalar-torsion f(T,ϕ) gravity theories in the presence of a matter fluid ⋮ Scalar fields near compact objects: resummation versus UV completion ⋮ Weakly-coupled stealth solution in scordatura degenerate theory ⋮ The effective field theory of nonsingular cosmology ⋮ Cosmology of Extended Proca-Nuevo ⋮ White dwarf mass-radius relation in theories beyond general relativity ⋮ Probing modified gravity with integrated Sachs-Wolfe CMB and galaxy cross-correlations ⋮ Disformal symmetry in the Universe: mimetic gravity and beyond ⋮ FLRW cosmology with Horava-Lifshitz gravity: impacts of equations of state ⋮ Testing theories of gravity and supergravity with inflation and observations of the cosmic microwave background ⋮ The role of the tachyonic instability in Horndeski gravity ⋮ Tackling non-linearities with the effective field theory of dark energy and modified gravity ⋮ On the stability conditions for theories of modified gravity in the presence of matter fields ⋮ Effective description of higher-order scalar-tensor theories
Cites Work
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- Hořava–Lifshitz cosmology: a review
- Canonical Variables for General Relativity
- Mach's Principle and a Relativistic Theory of Gravitation
- The cosmological constant problem
- 4D gravity on a brane in 5D Minkowski space
- \(k\)-inflation
- Perturbations in \(k\)-inflation
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