---
title: Fourth Order Gravity Overview
url: https://www.emergentmind.com/topics/fourth-order-gravity-fog
type: topic
---

# Fourth Order Gravity Overview

Fourth Order Gravity (FOG) encompasses a broad class of metric theories of gravity whose field equations, derived from an action containing quadratic curvature invariants, exhibit up to four derivatives of the metric. These extensions of General Relativity (GR) are structurally distinct in that they admit additional propagating modes and new length scales, leading to modifications of the Newtonian potential and altered short-distance and high-curvature behaviors. Their phenomenology is constrained by laboratory and astrophysical experiments probing deviations from the inverse-square law.

## 1. Fundamental Action and Field Equations

The simplest prototype of Fourth Order Gravity is defined by the action
\[
S = \int d^4x \sqrt{-g} \left[ R + a\,R^2 + b\,R_{\mu\nu}R^{\mu\nu} \right] + S_{\text{matter}},
\]
where \( R \) is the Ricci scalar, \( R_{\mu\nu} \) the Ricci tensor, \( a \) and \( b \) are couplings with dimensions of length squared, and \( S_{\text{matter}} \) is the matter action [1108.1665]. The field equations are obtained by varying the action with respect to \( g^{\mu\nu} \), yielding
\[
G_{\mu\nu} + a\, H^{(R^2)}_{\mu\nu} + b\, H^{(R_{\alpha\beta}^2)}_{\mu\nu} = \kappa T_{\mu\nu},
\]
where each \( H \) tensor contains terms with up to four derivatives of the metric:
\[
\begin{aligned}
H^{(R^2)}_{\mu\nu} &= 2R R_{\mu\nu} - \tfrac{1}{2}g_{\mu\nu} R^2 - 2\nabla_\mu\nabla_\nu R + 2g_{\mu\nu} \Box R, \\
H^{(R_{\alpha\beta}^2)}_{\mu\nu} &= 2R_{\mu\alpha}R^\alpha{}_\nu - \tfrac{1}{2}g_{\mu\nu}R_{\alpha\beta}R^{\alpha\beta} + \Box R_{\mu\nu} + \nabla_\mu\nabla_\nu R - 2\nabla_\alpha\nabla_{(\mu}R_{\nu)}{}^\alpha.
\end{aligned}
\]
This generic fourth-order structure arises from the higher-derivative terms present in the action.

## 2. Weak-Field Limit and Modified Newtonian Potential

In the static, spherically symmetric, weak-field regime (\( |a|,|b| \) small and metric perturbations \( |\Phi|,|\Psi| \ll 1 \)), the field equations linearize to a coupled system for the metric potentials and Ricci scalar [1108.1665]:
\[
\begin{aligned}
(\nabla^2 - m_1^2)\chi_1 &= \kappa T, \quad m_1^2 = \frac{1}{6a + 2b}, \\
(\nabla^2 - m_2^2)\chi_2 &= \kappa T_{00}, \quad m_2^2 = -\frac{1}{b}.
\end{aligned}
\]
The gravitational potential outside a spherical source of radius \( R \) and mass \( M \) is
\[
\Phi(r) = - \frac{G M}{r} \left[ 1 + \frac{1}{3}e^{-m_1 r} - \frac{4}{3}e^{-m_2 r} \right],
\]
where \( m_1 = 1/\sqrt{6a + 2b} \) and \( m_2 = 1/\sqrt{-b} \). The \( e^{-m_1 r} \) term is attractive, the \( e^{-m_2 r} \) term repulsive.

Absence of tachyonic or oscillatory modes requires \( 6a + 2b > 0 \) and \( b < 0 \). The eigenvalues \((m_1, m_2)\) set new characteristic length scales, producing deviations from Newton's law at short distances. When \( 0 \leq a \sim -b \ll R^2 \), the Yukawa terms decay rapidly for \( r \gg \sqrt{a}, \sqrt{-b} \).

## 3. Experimental Bounds and Astrophysical Implications

Laboratory searches for non-Newtonian gravity (e.g., torsion-balance experiments) constrain any Yukawa interaction of strength \( |\alpha| \sim \mathcal{O}(1) \) to have a range smaller than a few tenths of a millimeter. This translates to [1108.1665]
\[
\sqrt{a}, \sqrt{-b} \lesssim 10^{-3}~\mathrm{m},
\]
implying
\[
a, |b| \lesssim 10^{-6}~\mathrm{m}^2.
\]
Consequently, for all astrophysical and cosmological objects, with radii \( R \gg \sqrt{a}, \sqrt{-b} \) (e.g., \( R_\odot \sim 10^9~\mathrm{m} \)), the Yukawa corrections are negligibly small. Thus, at the level constrained by experiment, FOG has no observable effect on stellar structure, galaxy rotation curves, or the large-scale expansion.

## 4. Regimes of the Gravitational Field and Potential Structure

The behavior of the solution qualitatively depends on the interplay between the characteristic lengths and the source size:

- For \( 0 \leq a \sim -b \ll R^2 \), the Newtonian potential is modified outside the body by both an attractive and a repulsive Yukawa interaction.
- For \( a \sim -b \gg R^2 \), the gravitational field is screened near the body (effectively zero), but becomes Newtonian at distances \( r \gtrsim \sqrt{a} \sim \sqrt{-b} \).

This suggests that the higher-order terms could, in principle, produce strong screening over short distances or new intermediate regimes, but laboratory constraints render these behaviors unobservable at macroscopic/astrophysical scales.

## 5. Theoretical Extensions and Key Features

The prototype FOG action sits within a broader landscape of higher-derivative gravity models. In four dimensions, only two independent quadratic invariants produce physically nontrivial effects at the linearized level—typically chosen as \( R^2 \) and \( R_{\mu\nu}R^{\mu\nu} \), since variation of the Riemann-squared term is reducible via Gauss–Bonnet in \( D=4 \) [1007.1917]. The fourth-order field equations generically propagate extra massive modes beyond the massless graviton, with masses set by \( a \) and \( b \).

No relevant astrophysical or cosmological deviation from GR arises within experimental bounds. For larger values of \( a \), \( b \), the theory can yield strong modifications, but these are empirically excluded. Nevertheless, the fourth-order structure provides a well-defined playground for theoretical studies of higher-derivative corrections, possible screening effects, and attempts at ultraviolet completion.

## 6. Summary Table: FOG Properties and Constraints

| Property                         | FOG Prediction                                             | Experimental Constraint / Implication   |
|-----------------------------------|-----------------------------------------------------------|-----------------------------------------|
| Potential form                   | Newtonian + \( +\frac{1}{3} \) attractive Yukawa \(-\frac{4}{3}\) repulsive Yukawa | Both terms must have sub-mm range       |
| Yukawa ranges                    | \( \sqrt{6a + 2b} \), \( \sqrt{-b} \)                     | \( <10^{-3}~\mathrm{m} \)               |
| Astrophysical/Cosmological effect| Negligible                                                | None for stars, galaxies, cosmology     |
| Admissible parameters             | \( 6a+2b > 0,~ b < 0 \), \( a,|b| \ll R^2 \) (body size) | Lab: \( a,|b| \lesssim 10^{-6}~\mathrm{m}^2 \) |
| Field equation order              | Fourth                                                   | --                                      |
| Additional propagating modes      | Two Yukawa (massive) modes in linearized limit            | Not observed                            |

The structure and experimental constraints collectively imply that, in its simplest form, Fourth Order Gravity is mathematically consistent and phenomenologically viable only in a regime where its corrections to GR are unmeasurably small on all scales above millimeters [1108.1665].

Source: https://www.emergentmind.com/topics/fourth-order-gravity-fog