Eur. Phys. J. Plus (2026) 141: 21
https://doi.org/10.1140/epjp/s13360-025-07084-4

Regular Article

Gravitational wave strain and orbital dynamics of binary pulsars from LIGO/Virgo to LISA

Physics Department, Al-Balqa Applied University, 19117, As-Salt, Jordan

^a ali.taani@bau.edu.jo

Received: 20 June 2025
Accepted: 17 November 2025
Published online: 7 January 2026

Abstract

We present comprehensive calculations of gravitational wave strain amplitudes for known binary pulsar systems, using data from current ground based detectors (LIGO-Virgo-KAGRA) and the upcoming space-based missions (LISA). We present detailed calculations of the characteristic gravitational wave strain values, ranging from 3.0 to 73 $\times {10}^{-22}$, across frequencies between 0.66 and 5.87 $\times {10}^{-4}$ Hz. Our post-Newtonian approximation analysis yields predicted periastron advance rates from 1.6 to 80.5 deg/yr and orbital period decay rates between −5 and −176 $\mathrm{\mu }$s/yr for the binary pulsar population. We derive common envelope efficiency parameters (${\alpha }_{\mathrm{CE}}$) for representative progenitor scenarios within our sample, finding values between 0.63 and 1.16, with notable sensitivity to the binding energy parameter $\lambda$. Binary neutron star merger rates are estimated at $22.{77}_{-6.83}^{+6.83}$${\text{Myr}}^{-1}$ for the Milky Way, corresponding to a volumetric rate of $227.{71}_{-68.31}^{+68.31}$${\text{Gpc}}^{-3}$${\text{yr}}^{-1}$, consistent with the latest LIGO-Virgo-KAGRA observational constraints. Our results illustrate how multi-band gravitational wave observations, from LIGO/Virgo to LISA, can contribute to precise measurements of binary pulsar strain and orbital evolution histories, improving merger time predictions and constraining neutron star physics and common envelope processes.