An overview of f(R) theories
ABSTRACT A brief introduction to theories of the gravitational field with a Lagrangian
that is a function of the scalar curvature is given. The emphasis will be
placed in formal developments, while comparison to observation will be
discussed in the chapter by S. Jor\'as in this volume.
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ABSTRACT: The field equations following from a Lagrangian L(R) will be deduced and solved for special cases. If L is a non-linear function of the curvature scalar, then these equations are of fourth order in the metric. In the introduction we present the history of these equations beginning with the paper of H. Weyl from 1918, who first discussed them as alternative to Einstein's theory. In the third part, we give details about the cosmic no hair theorem, i.e., the details how within fourth order gravity with L= R + R^2 the inflationary phase of cosmic evolution turns out to be a transient attractor. Finally, the Bicknell theorem, i.e. the conformal relation from fourth order gravity to scalar-tensor theory, will be shortly presented.03/2006;
Physical review D: Particles and fields 06/1996; 53(10):5597-5608.
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ABSTRACT: Several authors have argued that self-consistent f(R) gravity models distinct from the cold dark matter model with a cosmological constant (LambdaCDM) are almost ruled out. Confronting such claims, we present a particular two-parameter f(R) model that (a) is cosmologically viable and distinguishable from LambdaCDM, (b) is compatible with the existence of relativistic stars, (c) is free of singularities of the Ricci scalar during the cosmological evolution, and (d) allows the addition of high-curvature corrections that could be relevant for inflation.Physical Review Letters 07/2009; 102(22):221101. · 7.37 Impact Factor
arXiv:1107.5183v1 [gr-qc] 26 Jul 2011
An overview of f(R) theories
Santiago Esteban Perez Bergliaffa
Departamento de Física Teórica, Instituto de Física, Universidade do Estado do Rio de Janeiro,
Abstract. A brief introduction to theories of the gravitational field with a Lagrangian that is a
function of the scalar curvature is given. The emphasis will be placed in formal developments,
while comparison to observation will be discussed in the chapter by S. Jorás in this volume.
Keywords: modified theories of gravity, cosmology, dark energy
The predictions of General Relativity (GR) are confirmed to an impressive degree by
observations in number of situations . In spite of this fact, theories that differ from
GR either in the limit of low or high curvature have been intensively studied lately,
and have a long tradition, starting with a paper by Weyl in 1918 . Although Weyl’s
motivationwas related to the unification of GR and Electrodynamics, the current revival
of these theories is twofold. In the case of low curvature, the aim is to describe the
accelerated expansion of the universe that follows from several observations  (when
interpreted in the standard cosmological model )1. Regarding the high-curvature
regime, it is important to note that there is no observational evidence of the behaviour
of the gravitational field for very large values of the curvature. This makes objects such
as black holes and neutron stars the ideal places to look for deviations from General
Relativity in the strong regime. In fact, the Kerr solution is not unique in f(R) theories
. Consequently, any deviation from Kerr’s spacetimee in compact objects will be
unequivocally signaling the need of changes in our description of strong gravity. The
task of understanding what kind of deviations can be expected, and their relation to
observable quantities is of relevance in view of several developments that offer the
prospect of observing properties of black holes in the vicinity of the horizon .
In this short review we will be concerned with gravitational theories described by the
where g is the determinant of the metric gµνand f is an arbitrary function of the the
curvature scalar R2. The function f must satisfy certain constraints, some of which
1The possibility of describing the current accelerated expansion of the universe using f(R) theories was
first discussed in .
2This choice if favoured by a theorem by Ostrogradski  over Lagrangians built with invariants
obtained from the the Ricci and Riemann tensors.
are necessary for the theory to be well-defined ab initio, and others to account for
observational facts. Those in the first class will be discussed in this review, while those
in the second class are presented in the chapter by S. Jorás in this volume3. We shall
begin by reviewing in the next section some general features of this type of theories.
THE THREE VERSIONS OF f(R) THEORIES
We shall see in this section that f(R) theories can be classified in three different types,
according to the role attibuted to the connection. In all of the versions, the equation for
the energy-momentum conservation is valid, since the total (gravitational plus matter)
action is diffeomorphism-invariant and gravity and matter are minimaly coupled by
hypothesis (see for instance , ).
In the metric version of f(R) theories, the action
is varied with respect to gµν. Here, SMis the matter action, which is independent of the
connection. The resultant equations of motion are of fourth order in the derivatives of
the metric tensor:
where Tµνis the energy-momentum of he matter fields, defined by
and the covariant derivative is defined using the usual Levi-Civita connection. Taking
the trace, we obtain
which is to be compared to R = −κT, the result in GR.
3There are several reviews that deal with different aspects of f(R) theories, see ,,, and also the
recent book .
Equivalence with Brans-Dicke theory
As shown for instance in , the gravitational part of the action given in Eqn.(2) is
equivalent to the following action:
U(φ) =φχ(φ)− f(χ(φ))
φ = f,χ(χ), and χ = R, corresponding to a Brans-Dicke theory with ω = 0 . Note
that the absence of a kinetic term for the scalar field does not mean that it is non-
dynamical: its evolution, due to the non-minimal coupling with the gravitational field, is
given by the variation of the action wrt φ:
Through a conformal transformation of the metric and a redefinition of the scalar field,
the action given in Eqn.(4) can be taken to that of a scalar field minimally coupled
with gravity, and with nonzero kinetic term and potential. These representations of f(R)
theories show that there is a massive scalar degree of freedom, which manifests as a
longitudinal mode in gravitational radiation (see for instance  for the cosmological
We close this section by stating that the equivalent representations are convenient
because sometimes the potential in Eqn.(5) is typically multivalued (see for instance
). It may be better to work directly in the original representation, as for instance
in Ref. in the case of compact stars.
In this second type of f(R) theories, the metric and the connection are taken as
independent fields, and the matter action SMis independent of the connection. So the
starting point is the action
where R = gµνRµν, and the corresponding Riemann tensor is constructed with a
connection Γ a priori independent of the metric.
From the variation of the action wrt the metric and Γ we get4(see for instance )
¯∇λ(√−g f′(R)gµν) = 0,
where the prime denotes derivative wrt R, and the barred covariant derivative is built
with the connection Γ. GR is recovered by setting f(R) = R in these equations. Taking
the trace of Eqn.(8) we obtain
f′(R)R−2f(R) = κT,
which shows that in this case the relation between R and T is algebraic, hence no scalar
mode is present.
From Eqn.(9), it follows that 
Since this expression relates Γ to R and the metric, and R and T are in principle
interchangeable through Eqn.(10), the connection can be in principle expressed in terms
of the matter fields and the metric. In other words, it is an auxiliary field. In fact, Eqn.(8)
can be rewritten as
where the Einstein tensor and the covariant derivatives are built with the Levi-Civita
connection, and R is expressed in terms of T using Eqn.(10). It follows that this version
of f(R) theories can be interpreted as GR with a modified source. Perhaps the most
important modification is that third order derivatives of the matter fields appear on the
rhs of Eqn.(13). As reported in , this feature may cause serious problems in static
spherically symmetric solutions with a polytropic fluid with index 3/2 < γ < 2 as a
source. Note however that this result result was challenged in the review 5.
4In the case of GR, this method furnishes the same result as the metric case, but this is not the case in
more general theories as discussed for example in .
5It has also been claimed that the Cauchy problem is not well-posed for the Palatin version of f(R)
theories . For an updated discussion see .
In thiscase, the matteraction depends of theconnection, which is a prioriindependent
of the metric. The action is given by
Depending on the matter fields, the theory may display non-propagating torsion and
non-metricity (see  and  for details).
Metric f(R) theories havebeen generalized by allowinga nonminimalcoupling between
the curvature and the matter Lagrangian, with action given by
where f1and f2are arbitrary functions of R, and λ is a constant. A particular case of
this action was considered in  in the context of the accelerated expansion of the
universe. Later, it was shown in  that this type of theory leads to a modification of
the conservation law of the matter energy-momentum tensor, namely
The presence of a nonzero rhs leads to non-geodesic motion, and it was suggested in
 that this may be related to MOND.
A more general type of theories was propposed in , with action given by
where f is an arbitrary function of R and of the matter Lagrangian. As in the previous
case, an extra force, perpendicular to the 4-velocity, accelerates the particles.
f(R)theories havebeen used to describe different aspects ofrelativisticastrophysicsand
cosmology. Since the low curvature limit, which has been studied primarily to explain
the accelerated expansion of the universe, is discussed in the chapter by S. Joras in
this volume, only one example will be given here in this regime. Afterwards, some
applications in the strong-curvature regime will be discussed.