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Proposal for Determining the Total Masses of Eccentric Binaries Using Signature of Periastron Advance in Gravitational Waves

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arxiv astro-ph/0111107 v2 pith:5RROLPGT submitted 2001-11-06 astro-ph gr-qc

Naoki Seto This is my paper · ORCID
classification astro-phgr-qc
keywords binariesfrequencymassestotaladvancedeterminingeccentricgravitational
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abstract

We propose a new method for determining total masses of low frequency eccentric binaries (such as, neutron star binaries with orbital frequency $f\gsim 10^{-3}$Hz) from their gravitational waves. In this method we use the frequency shift caused by periastron advance, and it works even at low frequency band where chirp signal due to radiation reaction is difficult to be measured. It is shown that the total masses of several Galactic neutron star binaries might be measured accurately (within a few percent error) by LISA with operation period of $\sim 10$ years.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Data-driven extraction, phenomenology and modeling of eccentric harmonics in binary black hole merger waveforms

    gr-qc 2025-04 conditional novelty 6.0 of 10

    Eccentric merger waveforms decompose into four smooth harmonics whose phases follow j times a common orbital phase plus an eccentricity-only correction, and whose mean-anomaly dependence can be fitted with simple functions.

  2. gwharmone: first data-driven surrogate for eccentric harmonics in binary black hole merger waveforms

    astro-ph.HE 2025-04 conditional novelty 6.0 of 10

    gwharmone is a data-driven surrogate that reproduces the eccentric harmonics of the dominant quadrupole mode in non-spinning eccentric binary black hole waveforms with average frequency-domain mismatches near 0.004.

  3. Probing vector gravitational atoms with eccentric intermediate mass-ratio inspirals

    gr-qc 2024-11 conditional novelty 5.0 of 10

    Eccentric intermediate-mass-ratio inspirals around vector gravitational atoms acquire faster decay, stronger circularization, and negative periastron precession, making the cloud visible to LISA-like detectors.

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