Healthy theories beyond Horndeski

By F. Vernizzi. 2016

451 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/65f90571096b67f96eb824fb513d5044269bf284

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Citations in the corpus

Cosmological tests of modified gravity (2015, methodology): “The Lagrangian that leads to second order equations of motion can be expressed in terms of the geometric scalars introduced above as [82, 92]”
hi_class: Horndeski in the Cosmic Linear Anisotropy Solving System (2016, background): “These models always contain higher derivatives in the equations of motion, even though that cancel once all the constraints are solved, leaving second-order equations for the propagating degrees of freedom [39, 40] (see also [41–43]).”
Extended scalar-tensor theories of gravity (2016, unknown): “In the literature, the unitary gauge is frequently used to study extended theories of Horndeski [4, 5, 21].”
Degenerate higher derivative theories beyond Horndeski: evading the Ostrogradski instability (2015, methodology): “1) also includes the extension beyond Horndeski introduced in [14], which can be written as L 4 = F4(φ,X)ǫ μνρ σ ǫ ′′′φμφμ′φνν′φρρ′ .”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “It includes as members the beyond Horndeski class [141, 142, 143] and the even more general class called degenerate higher-order scalar-tensor (DHOST) theories [140].”
Generic instabilities of nonsingular cosmologies in Horndeski theory: A no-go theorem (2016, methodology): “The resultant gradient instability is cured by the introduction of higher order spatial derivatives arising in the effective field theory approach [29] or in theories beyond Horndeski [30, 40, 41].”
Effective description of higher-order scalar-tensor theories (2017, methodology): “e, the introduction of a larger class of models, often called \beyond Horndeski" theories, showed that the absence of an extra scalar mode is compatible with third order Euler-Lagrange equations [17,24].3 These \beyond Horndeski" theories give a nonzero H, but L and the Aare still vanishin”
Gravitational wave decay into dark energy (2018, methodology): “e possible: !ˇˇfrom the coupling HM2 Pl ij@ iˇ@ jˇand ! ˇfrom the coupling HM2 Pl ˇ_ _2 ij . Here H is a dimensionless time-dependent function measuring the beyond Horndeski character of the theory [24,25]. It is dened in eq. (47) and for the theory (70) above is given by H = 2Xf ;X=f. We have stud”
Degenerate higher order scalar-tensor theories beyond Horndeski and disformal transformations (2016, background): “Within these degenerate higher order scalar tensor (DHOST) theories, we recovered, as particular cases, the (quadratic) Horndeski Lagrangian L4 as well as its extension L bH 4 introduced in [5, 6] (see section II for an explicit definition of these Lagrangians).”
Effective field theory of dark energy: A review (2019, methodology): “It captures for example the physics at linear cosmological scales of theories such as f(R)-gravity [97, 98], Horndeski [34, 36], GLPV theories [37, 80], low-energy Hořava gravity [49] and more, as illustrated in Table 1.”
Testing modified gravity at cosmological distances with LISA standard sirens (2019, background): “ot necessary in order to avoid dangerous Ostrogradsky instabilities [80,81]. This aspect, noticed in [82] using transformations of the metric, led initially to the so called beyond Horndeski theories [83]. Subsequently, it was realised that higher order eld equations are actually harmless provided t”