Sources of gravity waves
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The discovery of many possible sources of gravitational radiation, such as neutron stars, compact x-ray sources, rapidly rotating binary novae and the violent events occurring in quasars and galactic nuclei, has opened a new era of general-relativity physics. In the 1960's nearly all workers in the field considered the detection of gravitational radiation “exceedingly unlikely.” From this pessimistic estimate the balance of opinion has shifted to the optimistic view that gravitational radiation, a crucial prediction of Einstein's general theory of relativity, is now within reach of current experimental techniques.Keywords:
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It is well known that Einstein's General Relativity (GR) achieved a great success and overcame lots of experimental tests. On the other hand, GR also showed some shortcomings and flaws which today advise theorists to ask if it is the definitive theory of gravity. In this review we show that, if advanced projects on the detection of Gravitational Waves (GWs) will improve their sensitivity, allowing to perform a GWs astronomy, understanding if Einstein's GR is the correct and definitive theory of gravity will be possible. For this goal, accurate angular and frequency dependent response functions of interferometers for GWs arising from various Theories of Gravity, i.e. GR and Extended Theories of Gravity will have to be used. This review is founded on the Essay which won an Honorable Mention at the the 2009 Gravity Research Foundation Awards.
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The existence of gravitational radiation is a prediction of Einstein's general theory of relativity. Gravitational waves are perturbations in the curvature of spacetime caused by accelerated masses. Since the 1960s gravitational wave detectors have been built and constantly improved. The present-day generation of resonant mass antennas and laser interferometers has reached the necessary sensitivity to detect gravitational waves from sources in the Milky Way. Within a few years, the next generation of detectors will open the field of gravitational wave astronomy.
Einstein Telescope
Speed of gravity
Gravity Probe A
Gravitational time dilation
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The discovery of many possible sources of gravitational radiation, such as neutron stars, compact x‐ray sources, rapidly rotating binary novae and the violent events occurring in quasars and galactic nuclei, has opened a new era of general‐relativity physics. In the 1960's nearly all workers in the field considered the detection of gravitational radiation “exceedingly unlikely.” From this pessimistic estimate the balance of opinion has shifted to the optimistic view that gravitational radiation, a crucial prediction of Einstein's general theory of relativity, is now within reach of current experimental techniques.
Speed of gravity
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This talk reviews the constraints imposed by binary-pulsar data on gravity theories, and notably on "scalar-tensor" theories which are the most natural alternatives to general relativity. Because neutron stars have a strong gravitational binding energy, binary-pulsar tests are qualitatively different from solar-system experiments: They have the capability of probing models which are indistinguishable from general relativity in weak gravitational field conditions. Besides the two most precise binary-pulsar experiments, in the systems B1913+16 and B1534+12, we also present the results of the various "null" tests of general relativity provided by several neutron star-white dwarf binaries, notably those of gravitational radiation damping. [The main interest of this very short paper is its figure, which also takes into account the "strong equivalence principle" tests.]
Equivalence principle (geometric)
Speed of gravity
Gravity Probe A
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In this paper, we review the theoretical foundations of gravitational waves in the framework of Albert Einstein’s theory of general relativity. Following Einstein’s early efforts, we first derive the linearized Einstein field equations and work out the corresponding gravitational wave equation. Moreover, we present the gravitational potentials in the far away wave zone field point approximation obtained from the relaxed Einstein field equations. We close this review by taking a closer look on the radiative losses of gravitating [Formula: see text]-body systems and present some aspects of the current interferometric gravitational waves detectors. Each section has a separate appendix contribution where further computational details are displayed. To conclude, we summarize the main results and present a brief outlook in terms of current ongoing efforts to build a spaced-based gravitational wave observatory.
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Linearized gravity
Speed of gravity
Einstein field equations
Gravity Probe A
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We present a Bayesian data analysis pipeline for testing GR using gravitational wave signals from coalescing compact binaries, and in particular binary neutron stars. In this study, we investigate its performance when sources with spins are taken into account.
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Introduction Prologue: Tides in Newton's gravity/Relativity 1. A brief review of General Relativity 2. Gravitational waves 3. Beyond the Newtonian limit 4. Sources of gravitational radiation 5. Gravitational wave detectors 6. Gravitational wave data analysis Epilogue: Gravitational wave astronomy and astrophysics A. Gravitational wave detector data B. Post-Newtonian Binary Inspiral Waveform
Gravitational-wave astronomy
Prologue
Speed of gravity
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On February 11, 2016, Laser Interferometer Gravitational-wave Observatory (LIGO) announced the detection of gravitational waves from two merging black holes. We at Prespacetime Journal celebrate Einstein’s General Theory of Relativity and congratulate LIGO and all the people and agencies involved for this landmark discovery predicted by Einstein 100 years ago. There is no doubt that this discovery marks the beginning of a new era in astronomy, cosmology and even quantum gravity.
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Gravitational-wave astronomy
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This review is focused on tests of Einstein's theory of General Relativity with gravitational waves that are detectable by ground-based interferometers and pulsar timing experiments. Einstein's theory has been greatly constrained in the quasi-linear, quasi-stationary regime, where gravity is weak and velocities are small. Gravitational waves will allow us to probe a complimentary, yet previously unexplored regime: the non-linear and dynamical strong-field regime. Such a regime is, for example, applicable to compact binaries coalescing, where characteristic velocities can reach fifty percent the speed of light and compactnesses can reach a half. This review begins with the theoretical basis and the predicted gravitational wave observables of modified gravity theories. The review continues with a brief description of the detectors, including both gravitational wave interferometers and pulsar timing arrays, leading to a discussion of the data analysis formalism that is applicable for such tests. The review ends with a discussion of gravitational wave tests for compact binary systems.
Speed of gravity
Einstein Telescope
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