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Testing General Relativity with Pulsar Timing
, 2003
"... Pulsars of very different types – isolated objects, and binaries with short and longperiod orbits, whitedwarf and neutronstar companions – provide the means to test both the predictions of general relativity and the viability of alternate theories of gravity. This article presents an overview of ..."
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Pulsars of very different types – isolated objects, and binaries with short and longperiod orbits, whitedwarf and neutronstar companions – provide the means to test both the predictions of general relativity and the viability of alternate theories of gravity. This article presents an overview of pulsars, then discusses the current status and future prospects of tests of equivalence principle violations and strongfield gravitational experiments. 1 1
Deformation of the Planetary Orbits Caused by the Time Dependent Gravitational Potential in the Universe
, 2004
"... PACS number: 98.80.Jk In the recent paper [4], assuming a linear change of a gravitational potential V in the universe, i.e. ∆V = −c 2 H∆t, are explained both the Hubble red shift and the anomalous acceleration aP from the spacecraft Pioneer 10 and 11 [1]. The change of the potential V causes an acc ..."
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PACS number: 98.80.Jk In the recent paper [4], assuming a linear change of a gravitational potential V in the universe, i.e. ∆V = −c 2 H∆t, are explained both the Hubble red shift and the anomalous acceleration aP from the spacecraft Pioneer 10 and 11 [1]. The change of the potential V causes an accelerated time which is easily seen by the Hubble red shift. But the change of the potential causes also change of the distances in the galaxy, and hence modification on the planetary orbits. In this paper it is shown that the planetary orbits are not axially symmetric and the angle from the perihelion to the aphelion is π − HΘ 3eπ, while the angle from the aphelion to the perihelion is π + HΘ, where Θ is the period of revolution, e is 3eπ the eccentricity of the elliptic trajectory and H is the Hubble constant. There is no perihelion precession caused by the time dependent gravitational potential V. The quotient of the time needed for the planet to come from the perihelion to the aphelion and the time from the aphelion to the perihelion, is equal to
P oS(MCCTSKADS)014 Pulsars
"... After nearly 40 years since the original discovery, pulsar research has great vitality, making major contributions to fields ranging from ultradense matter physics to relativistic gravity, from cosmology to stellar evolution, from globular cluster dynamics to the study of interstellar medium. This ..."
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After nearly 40 years since the original discovery, pulsar research has great vitality, making major contributions to fields ranging from ultradense matter physics to relativistic gravity, from cosmology to stellar evolution, from globular cluster dynamics to the study of interstellar medium. This lecture aims to give a brief introduction to the theoretical and observational properties of pulsars. Classification and evolution of pulsars are dealt with first. Then the basic concepts driving the pulsar search experiments and the followup timing observations are presented. Finally it is reported on some of the most interesting scientific results obtained in the last decade using the pulsars as tools for the investigation, with particular emphasis for the case of the recently discovered first Double Pulsar system.
Frontiers of Cosmic Ray Science 49 Gravitational Radiation — Observing the Dark and Dense Universe
"... Astronomical observations in the electromagnetic window – microwave, radio and optical – have revealed that most of the Universe is dark. The only reason we know that dark matter exists is because of its gravitational influence on luminous matter. It is plausible that a small fraction of that dark ..."
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Astronomical observations in the electromagnetic window – microwave, radio and optical – have revealed that most of the Universe is dark. The only reason we know that dark matter exists is because of its gravitational influence on luminous matter. It is plausible that a small fraction of that dark matter is clumped, and strongly gravitating. Such systems are potential sources of gravitational radiation that can be observed with a worldwide network of gravitational wave antennas. Electromagnetic astronomy has also revealed objects and phenomena – supernovae, neutron stars, black holes and the big bang – that are without doubt extremely strong emitters of the radiation targeted by the gravitational wave interferometric and resonant bar detectors. In this talk I will highlight why gravitational waves arise in Einstein’s theory, how they interact with matter, what the chief astronomical sources of the radiation are, and in which way by observing them we can gain a better understanding of the dark and dense Universe. 1.
The 28th International Cosmic Ray Conference 1 Gravitational Radiation – Observing the Dark and Dense Universe
, 2004
"... Astronomical observations in the electromagnetic window – microwave, radio and optical – have revealed that most of the Universe is dark. The only reason we know that dark matter exists is because of its gravitational influence on luminous matter. It is plausible that a small fraction of that dark m ..."
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Astronomical observations in the electromagnetic window – microwave, radio and optical – have revealed that most of the Universe is dark. The only reason we know that dark matter exists is because of its gravitational influence on luminous matter. It is plausible that a small fraction of that dark matter is clumped, and strongly gravitating. Such systems are potential sources of gravitational radiation that can be observed with a worldwide network of gravitational wave antennas. Electromagnetic astronomy has also revealed objects and phenomena – supernovae, neutron stars, black holes and the big bang – that are without doubt extremely strong emitters of the radiation targeted by the gravitational wave interferometric and resonant bar detectors. In this talk I will highlight why gravitational waves arise in Einstein’s theory, how they interact with matter, what the chief astronomical sources of the radiation are, and in which way by observing them we can gain a better understanding of the dark and dense Universe. 1.
unknown title
, 2006
"... Testing postNewtonian theory with gravitational wave observations ..."
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New Relativistic Equations of Motion and Their Comparison with the Equations from the General Relativity
, 2004
"... In this paper is presented the infinitesimally locally Lorentzian theory of gravitation (ILLTG), which predicts the same experimental results which confirm the GR. Motion in a neighborhood of the center of gravitation is considered. The geodesics between the ILLTG and GR are compared. ILLTG differs ..."
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In this paper is presented the infinitesimally locally Lorentzian theory of gravitation (ILLTG), which predicts the same experimental results which confirm the GR. Motion in a neighborhood of the center of gravitation is considered. The geodesics between the ILLTG and GR are compared. ILLTG differs from GR mainly in the equations of motion and for v << c the trajectories are almost the same in both theories. Two tests in the solar system are proposed, such that ILLTG and GR predict different results. The mass and energy with respect to ILLTG is considered. The periastron shift of the binary stars is calculated and a cosmological problem is considered. 1
unknown title
, 2002
"... We reanalyze a binary pulsar system and show that the orbital period change rate can be completely understood as a curvature backreaction process. Appreciating a detailed theoretical and observational study of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude ..."
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We reanalyze a binary pulsar system and show that the orbital period change rate can be completely understood as a curvature backreaction process. Appreciating a detailed theoretical and observational study of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude that general relativity and astrophysical observations rule out the existence of gravitational radiation. Thus, the force of gravity is not a local gauge force. The discovery of the binary pulsar B1913+16 by Hulse and Taylor [1] represents a milestone in astrophysics because relativistic binary pulsar systems are perfect laboratories to study general relativity. In the past decades very detailed calculations were performed in the postNewtonian approximation with all possible relativity corrections to measurables (see, for example, [2], [3], [4] and references therein). However, it seems that one important part of calculations is not included into the analysis of a relativistic binary system. Namely, the impact of the spacetime curvature on the observables of a binary bound system is not elucidated in all respects. Let us define a metric in the following form: gµν = ηµν + hµν. It is suitable for the treatment of an isolated bound system if we assume that hµν vanishes at infinity. One can now write Einstein equations in the 1 following form (see $ $ 7.6 of the book in [5]; we accept conventions of this book): R (1) µν − 1