Cosmological higher-curvature gravities
Javier Moreno, Ángel Murcia
Abstract
Abstract We examine higher-curvature gravities whose Friedmann–Lemaître–Robertson–Walker configurations are specified by equations of motion which are of second order in derivatives, just like in Einstein gravity. We name these theories Cosmological Gravities and initiate a systematic exploration in dimensions <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:mi>D</mml:mi><mml:mtext>⩾</mml:mtext><mml:mn>3</mml:mn></mml:mrow></mml:math> . First, we derive an instance of Cosmological Gravity to all curvature orders and dimensions <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:mi>D</mml:mi><mml:mtext>⩾</mml:mtext><mml:mn>3</mml:mn></mml:mrow></mml:math> . Second, we study Cosmological Gravities admitting non-hairy generalizations of the Schwarzschild solution characterized by a single function whose equation of motion is, at most, of second order in derivatives. We present explicit instances of such theories for all curvature orders and dimensions <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:mi>D</mml:mi><mml:mtext>⩾</mml:mtext><mml:mn>4</mml:mn></mml:mrow></mml:math> . Finally, we investigate the equations of motion for cosmological perturbations in the context of generic Cosmological Gravities. Remarkably, we find that the linearized equations of motion for scalar cosmological perturbations in any Cosmological Gravity in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:mi>D</mml:mi><mml:mtext>⩾</mml:mtext><mml:mn>3</mml:mn></mml:mrow></mml:math> contain no more than two time derivatives. We explicitly corroborate this aspect by presenting the equations for the scalar perturbations in some four-dimensional Cosmological Gravities up to fifth order in the curvature.