Abstract. The ¯rst eclipsing binary pulsar, PSR B1957+20, was discovered in 1987. Since then, 13 other eclipsing low-mass binary pulsars have been found; 12 of these are in globular clusters. In this paper we list the known eclipsing bi-nary pulsars and their properties, with special attention

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Accepted. Received; in original form

or non-detection of these elements, and their relative abundances if detected, would provide a diagnostic of the high energy output of the primary, and possibly the shock acceleration of particles at the companion’s bow shock in a pulsar wind.

Abstract. In this paper we calculate the emission of gravity waves by the binary pulsar in the framework of five dimensional spacetime. We consider only spacetimes with one compact extra-dimension. We show that the presence of additional degrees of freedom, especially the ’gravi-scalar ’ leads to a

In the present work, an exact solution of Einstein’s field equations representing the field of a binary system, is obtained. It is shown that this solution is a time-dependent one. This solution is a modified version of that obtained by Curzon, since it reduces to the later one in the static case

We present a simple novel method for determining the orbital parameters of binary pulsars. This method works with any sort of orbital sampling, no matter how sparse, provided that information on the period derivatives is available with each measurement of the rotational period of the pulsar

of gravitational relativity theory now available. One of these is the 3 millimeter decrease per revolution in the orbit of the Hulse Taylor binary pulsar. It is no longer valid to attempt to explain this with EH theory and a straightforward qualitative explanation is given in terms of ECE theory without using

The aim of this work is to discuss how binary pulsar data can be used for experimental tests of the strong-field regime of relativistic gravity, in the frame of the parametrized Post-Keplerian formalism. In 1915, Einstein’s field equations gave the correct prediction for the perihelion shift

Abstract. We describe the results of a relativistic analysis of our observations of binary pulsar B1913+16, up to the latest measurements in 2001 August. 1.