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Cosmic gamma rays spectrum from neutral pions production and decay in metagalactic cosmic ray p-p collisions, deriving models based on Einstein general relativity theory
Pulsating very dense white dwarfs models noting general relativity
Light emission from collapsing nonrotating gas in general relativity, noting restrictions on range and frequency shift
Celestial mechanics experiment for Mariner Mars 1971 to test general relativity theory and improve Martian ephemeris
DSIF operations for testing theory of general relativity by very long baseline interferometers and for study of pulsar polarization
A manual is presented which is designed to familiarize the GE 635 user with the configuration and operation of the overall system. Work submission, programming standards, restrictions, testing and debugging, and related general information is provided for GE 635 programmer.
This article studies the relativistic theory of the motion of a particle in the presence of a uniform acceleration field. The problem is introduced as a linearization of the fundamental line element of general relativity. The linearized line element is a solution of Einstein's field equations. The equations of geodesics corresponding to this line element are solved and applied to the clock paradox problem.-
Demonstration that the conventional theory of the mass-zero spin-two field with sources introduces extraneous nonspin-two field components in source regions and fails to be covariant under the full or restricted conformal group. A modified theory is given, expressed in terms of the physical components of mass-zero spin-two field rather than in terms of 'potentials,' which has no extraneous components inside or outside sources, and which is covariant under the full conformal group. For a proper choice of source term, this modified theory has the correct Newtonian limit and automatically implies that a symmetric second-rank source tensor has zero divergence. It is shown that possibly a generally covariant form of the spin-two theory derived here can be constructed to agree with general relativity in all currently accessible experimental situations.
Measurement of echo delays of radar signals transmitted from earth to Mercury, yielding an accurate value for the advance of the latter's perihelion position. Given that the sun's gravitational quadrupole moment is negligible, the result in terms of the Eddington-Robertson parameters is (2 + 2 gamma-beta)/3 approximately equal to 1.005 plus or minus 0.007, where gamma = beta = 1 in general relativity, and where 0.007 represents the statistical standard error. Inclusion of the probable contribution of systematic errors raises the uncertainty to about 0.02.
Dicke and Goldenberg (1967) on the basis of the value of the solar oblateness obtained had concluded that the excess perihelion motion of mercury is not in accord with Einstein's prediction according to general relativity. However, the observations from which the oblateness value was derived might be simply the result of an excess brightness at the equatorial solar limb. Such brightness might be due to the presence of faculae. Dicke (1970) had concluded that the effect of faculae on the oblateness determination is insignificant. In a reexamination of Dicke's argument it was found that his reasons for rejecting faculae as a source of oblateness are unjustified.
A theoretical framework for testing theories of gravitation is considered. This framework separates theories into those that are viable and those that are nonviable by sending each through a series of tests. Most of these tests compare the theory's predictions with the results of experiment, but one test judges each theory's completeness, self-consistency and agreement with Newtonian physics at lowest order. Only a few theories, including general relativity, are currently viable, that is, pass all five tests in the framework. Einstein's 1912 theory is also ruled out because it predicts only half the observed time-delay effect. Future tests proposed include improvements of old experiments and a number of new experiments.
A new relativistic theory of gravity is presented. This theory agrees with all experiments to date. It is a metric theory, it is Lagrangian-based, and it possesses a preferred frame with conformally-flat space slices. With an appropriate choice of certain adjustable functions and parameters, this theory possesses precisely the same post-Newtonian limit as general relativity.
Approaches regarding the role of gravitational wave observations in the investigation of relativistic theories of gravity are treated as providing greater potential in the prediction of wave propagation speed and the polarization properties of gravitational waves. The invariant classes of waves discussed have the same post-Newtonian limit as general relativity for a reasonable choice of cosmological models.
A theory is presented of gravity which has the same post-Newtonian (PN) as that of general relativity. The field equations, and a calculation of the PN limit of the theory are discussed along with the equations of stellar structure for static spherically symmetric stars. A special exterior spherically symmetric solution, time dependent solutions, conservations, and gravitational waves are analyzed.
The efforts and accomplishments of the CME Team are summarized. The objectives and experiment status, gravity field of Mars, test of general relativity, and the generation of normal points are discussed.
Review of historical and recent experiments which speak in favor of a post-Newtonian relativistic gravitational theory. The topics include the foundational experiments, metric theories of gravity, experiments designed to differentiate among the metric theories, and tests of Machian concepts of gravity. It is shown that the metric field for any metric theory can be specified by a series of potential terms with several parameters. It is pointed out that empirical results available up to date yield values of the parameters which are consistent with the prediction of Einstein's general relativity.
The study of cosmological models by means of equations of motion in Hamiltonian form is considered. Hamiltonian methods applied to gravity seem to go back to Rosenfeld (1930), who constructed a quantum-mechanical Hamiltonian for linearized general relativity theory. The first to notice that cosmologies provided a simple model in which to demonstrate features of Hamiltonian formulation was DeWitt (1967). Applications of the ADM formalism to homogeneous cosmologies are discussed together with applications of the Hamiltonian formulation, giving attention also to Bianchi-type universes. Problems involving the concept of superspace and techniques of quantization are investigated.
It is well known that the gyromagnetic ratio (g factor) of a classical, slowly rotating body whose charge density is proportional to its mass density must be equal to unity. However, if the body is very massive, the spacetime curvature effects of general relativity become important and the result g = 1 is no longer valid. We calculate here the gyromagnetic ratio of a slowly rotating, massive shell with uniform charge density. When the shell is large compared with the Schwarzschild radius we have g = 1, but as the shell becomes more massive the g factor increases. In the limit as the shell approaches its Schwarzschild radius we obtain g approaching 2 (the same value as for an electron).