Kavli Affiliate: Lijing Shao
| First 5 Authors: Wen-Fan Feng, Tan Liu, Yan Wang, Lijing Shao,
| Summary:
The successful detection of continuous gravitational waves (GWs) from
spinning neutron stars (NSs) will shape our understanding of the physical
properties of dense matter under extreme conditions. Binary population
synthesis simulations show that forthcoming space-borne GW detectors may be
capable of detecting some tight Galactic double NSs (DNSs) with 10-minute
orbital periods. Successfully searching for continuous GWs from such a close
DNS demands extremely precise waveform templates considering the interaction
between the NS and its companion. Unlike the isolated formation channel, the
DNSs from the dynamical formation channel have moderate to high orbital
eccentricities. To accommodate these systems, we generalize the analytical
waveforms from triaxial nonaligned NSs under spin-orbit coupling derived by
Feng et al. [Phys. Rev. D 108, 063035 (2023)
{https://journals.aps.org/prd/abstract/10.1103/PhysRevD.108.063035}] to
incorporate the effects of the orbital eccentricity. Our findings suggest that
for DNSs formed through isolated binary evolution, the impact of eccentricity
on the continuous GWs of their NSs can be neglected. In contrast, for DNSs
formed through dynamical processes, it is necessary to consider eccentricity,
as high-eccentricity orbits can result in a fitting factor of $lesssim 0.97$
within approximately 0.5 to 2 years of a coherent search. Once the GWs from
spinning NSs in tight binaries are detected, the relative measurement accuracy
of eccentricity can reach $Delta e / e sim O(10^{-7})$ for a signal-to-noise
ratio of $O(100)$ based on the Fisher information matrix, bearing significant
implications for understanding the formation mechanisms of DNSs.
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