Classical and general relativistic post-Keplerian effects in binary pulsars hosting fast rotating main sequence stars

Abstract

We consider a binary system composed of a pulsar and a massive, fast rotating, highly distorted main sequence star as a potential scenario to dynamically put to the test certain post-Keplerian effects of both Newtonian and post-Newtonian nature. We numerically produce time series of the perturbations $\Delta \left(\delta \tau \right)$ of the Rømer-like, orbital component of the pulsar's time delay $\delta \tau$ induced over 10 years by the pN gravitoelectric mass monopole, quadrupole, gravitomagnetic spin dipole and octupole accelerations along with the Newtonian quadrupolar one. We do not deal with the various propagation time delays due to the travelling electromagnetic waves. It turns out that, for a Be-type star with $M=15{\text{M}}_{\odot }$, $R_{\text{e}}=5.96{\text{R}}_{\odot }$, $\nu =0.203$, $S=3.41\times 10^{45}\text{J}\text{s}$, $J_2=1.92\times 10^{-3}$ orbited by a pulsar with an orbital period $P_{\text{b}}\simeq 40-70\text{d}$, the classical oblateness-driven effects are at the $\lesssim 4-150\text{s}$ level, while the pN shifts are of the order of $\lesssim 1.5-20\text{s}\left(GM{c}^{-2}\right)$, $\lesssim 10-40\text{ms}\left(GM{R}_{\text{e}}^2{J}_2{c}^{-2}\right)$, $\lesssim 0.5-6\text{ms}\left(GS{c}^{-2}\right)$, $\lesssim 5-20\mu \text{s}\left(GS{R}_{\text{e}}^2{\epsilon }^2{c}^{-2}\right)$, depending on their orbital configuration. The root-mean-square (rms) timing residuals ${\sigma }_{\tau }$ of almost all the existing non-recycled, non-millisecond pulsars orbiting massive, fast rotating main sequence stars are $\lesssim \text{ms}$. Thus, such kind of binaries have the potential to become interesting laboratories to measure, or, at least, constrain, some Newtonian and post-Newtonian key features of the distorted gravitational fields of the fast rotating stars hosted by them [Abridged].

arXiv commentLatex2e, 24 pages, 5 figures, 3 tables. One affiliation corrected

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