Parametric derivation of the observable relativistic periastron advance for binary pulsars

Abstract

We compute the dimensionless relativistic periastron advance parameter $k$, which is measurable from the timing of relativistic binary pulsars. We employ for the computation the recently derived Keplerian-type parametric solution to the post-Newtonian (PN) accurate conservative dynamics of spinning compact binaries moving in eccentric orbits. The parametric solution and hence the parameter $k$ are applicable for the cases of \emph{simple precession}, namely, case (i), the binary consists of equal mass compact objects, having two arbitrary spins, and case (ii), the binary consists of compact objects of arbitrary mass, where only one of them is spinning with an arbitrary spin. Our expression, for the cases considered, is in agreement with a more general formula for the 2PN accurate $k$, relevant for the relativistic double pulsar PSR J0737--3039, derived by Damour and Schäfer many years ago, using a different procedure.

12 pages including 1 figure; submitted to PRD

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Cited by in corpus (6)

• Phasing of gravitational waves from inspiralling eccentric binaries at the third-and-a-half post-Newtonian order
• Gravity experiments with radio pulsars
• The Kepler equation for inspiralling compact binaries
• Spinning compact binary dynamics and chameleon orbits
• The second post-Newtonian motion in Reissner-Nordström spacetime
• Spin dynamics of moving bodies in rotating black hole spacetimes