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Modified Gravity and Cosmology
, 2012
"... In this review we present a thoroughly comprehensive survey of recent work on modified theories of gravity and their cosmological consequences. Amongst other things, we cover General Relativity, ScalarTensor, EinsteinAether, and Bimetric theories, as well as TeVeS, f(R), general higherorder theo ..."
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In this review we present a thoroughly comprehensive survey of recent work on modified theories of gravity and their cosmological consequences. Amongst other things, we cover General Relativity, ScalarTensor, EinsteinAether, and Bimetric theories, as well as TeVeS, f(R), general higherorder theories, HořavaLifschitz gravity, Galileons, Ghost Condensates, and models of extra dimensions including KaluzaKlein, RandallSundrum, DGP, and higher codimension braneworlds. We also review attempts to construct a Parameterised PostFriedmannian formalism, that can be used to constrain deviations from General Relativity in cosmology, and that is suitable for comparison with data on the largest scales. These subjects have been intensively studied over the past decade, largely motivated by rapid progress in the field of observational cosmology that now allows, for the first time, precision tests of fundamental physics on the scale of the observable Universe. The purpose of this review is to provide a reference tool for researchers and students in cosmology and gravitational physics, as well as a selfcontained, comprehensive and uptodate introduction to the subject as a whole.
Testing Relativistic Gravity with Radio Pulsars”, ArXiv eprints
, 2014
"... Before the 1970s, precision tests for gravity theories were constrained to the weak gravitational fields of the Solar system. Hence, only the weakfield slowmotion aspects of relativistic celestial mechanics could be investigated. Testing gravity beyond the first postNewtonian contributions was fo ..."
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Before the 1970s, precision tests for gravity theories were constrained to the weak gravitational fields of the Solar system. Hence, only the weakfield slowmotion aspects of relativistic celestial mechanics could be investigated. Testing gravity beyond the first postNewtonian contributions was for a long time out of reach. The discovery of the first binary pulsar by Russell Hulse and Joseph Taylor in the summer of 1974 initiated a completely new field for testing the relativistic dynamics of gravitationally interacting bodies. For the first time the back reaction of gravitational wave emission on the binary motion could be studied. Furthermore, the HulseTaylor pulsar provided the first test bed for the orbital dynamics of strongly selfgravitating bodies. To date there are a number of pulsars known, which can be utilized for precision test of gravity. Depending on their orbital properties and their companion, these pulsars provide tests for various different aspects of relativistic dynamics. Besides tests of specific gravity theories, like general relativity or scalartensor gravity, there are pulsars that allow for generic constraints on potential deviations of gravity from general relativity in the quasistationary strongfield and the radiative regime. This article presents a brief overview of this modern field of relativistic celestial mechanics, reviews some of the highlights of gravity tests with radio pulsars, and discusses their implications for gravitational physics and astronomy, including the upcoming gravitational wave astronomy. 1 ar
THE USE OF XRAY PULSARS FOR AIDING GPS SATELLITE ORBIT DETERMINATION
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INSPIRALMERGERRINGDOWN MODELS FOR SPINNING BLACKHOLE BINARIES AT THE INTERFACE BETWEEN ANALYTICAL AND NUMERICAL RELATIVITY
"... The longsought direct detection of gravitational waves may only be a few years away, as a new generation of interferometric experiments of unprecedented sensitivity will start operating in 2015. These experiments will look for gravitational waves with frequencies from 10 to about 1000 Hz, thus tar ..."
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The longsought direct detection of gravitational waves may only be a few years away, as a new generation of interferometric experiments of unprecedented sensitivity will start operating in 2015. These experiments will look for gravitational waves with frequencies from 10 to about 1000 Hz, thus targeting astrophysical sources such as coalescing binaries of compact objects, core collapse supernovae, and spinning neutron stars, among others. The search strategy for gravitational waves emitted by compactobject binaries consists in filtering the output of the detectors with template waveforms that describe plausible signals, as predicted by general relativity, in order to increase the signaltonoise ratio. In this work, we modeled these systems through the effectiveonebody approach to the generalrelativistic 2body problem. This formalism rests on the idea that binary coalescence is universal across different mass ratios, from the testparticle limit to the equalmass regime. It bridges the gap between postNewtonian theory (valid in the slowmotion, weakfield limit) and blackhole perturbation theory (valid in the small massratio limit, but not limited to slow motion). The
Article Orbital Motions and the ConservationLaw/PreferredFrame α3 Parameter
, 2014
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Confronting General Relativity to binary pulsars.
, 2004
"... The aim of this work is to discuss how binary pulsar data can be used for experimental tests of the strongfield regime of relativistic gravity, in the frame of the parametrized PostKeplerian formalism. In 1915, Einstein’s field equations gave the correct prediction for the perihelion shift of Merc ..."
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The aim of this work is to discuss how binary pulsar data can be used for experimental tests of the strongfield regime of relativistic gravity, in the frame of the parametrized PostKeplerian formalism. In 1915, Einstein’s field equations gave the correct prediction for the perihelion shift of Mercury: General Relativity was born. The first prediction put to test was the apparent bending of light as it passes near a massive body. This effect was conclusively observed by Eddington during the solar eclipse of 1919. However, tests of General Relativity within the Solar System are limited. Indeed, if we compare the gravitational energy of a test particle of mass m, GMmR with its rest mass, mc 2, we get: GMc2R