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Abstract: Individual Super-massive Black Hole
Binaries in non-circular orbits are possible nanohertz gravitational
wave (GW) sources for pulsar timing arrays. We develop an accurate and
efficient approach to compute pulsar timing residuals due to GWs from
inspiralling massive black hole binaries in relativistic eccentric
orbits. Our approach employs a Keplerian-type parametric solution to
model third post-Newtonian accurate precessing eccentric orbits while
a novel semi-analytic prescription is provided to model the effects of
quadrupolar order GW emission. These inputs lead to a semi-analytic
prescription to model timing residuals from relativistic massive BH
binaries inspiralling along arbitrary eccentric orbits. Additionally,
we provide a fully analytic approach to model timing residuals from BH
binaries inspiralling along moderately eccentric orbits, influenced by
Boetzel et al. 2017. Relevant Codes are being incorporated into
Enterprise and TEMPO2 for searching the presence of such binaries in
the PTA data-sets.
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