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  1. Home
  3. Constraining The P-mode-g-mode Tidal Instability With Gw170817.
  1. Home
  3. Constraining The P-mode-g-mode Tidal Instability With Gw170817.

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Constraining the p-Mode-g-Mode Tidal Instability with GW170817.

B P Abbott1, R Abbott1, T D Abbott2

  • 1LIGO, California Institute of Technology, Pasadena, California 91125, USA.

Physical Review Letters
|March 2, 2019

View abstract on PubMed

Summary
This summary is machine-generated.

We investigated tidal instability effects on neutron star inspirals using GW170817 data. Our analysis found no significant evidence for these p-g mode effects, constraining their impact on gravitational wave signals.

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Area of Science:

  • Astrophysics
  • Gravitational Wave Astronomy
  • Neutron Star Physics

Background:

  • Neutron stars possess complex internal structures with various oscillation modes.
  • Tidal interactions in binary neutron star systems can excite these internal modes, potentially affecting their inspiral.

Purpose of the Study:

  • To analyze the impact of a proposed tidal instability coupling p-modes and g-modes in neutron stars on the gravitational wave signal of GW170817.
  • To quantify the influence of this p-g mode instability on the gravitational wave phasing and energy dissipation during binary neutron star inspiral.

Main Methods:

  • Modeling the effect of p-g mode instability on gravitational wave signals using three parameters per star: amplitude, saturation frequency, and spectral index.
  • Computing Bayes factors to compare models with and without p-g effects.
  • Performing signal injections to assess the probability of observing similar results when the instability is absent.

    • Main Results:

    • The observed GW170817 signal is consistent with models neglecting p-g effects, with a Bayes factor lnB_{!pg}^{pg}=0.03_{-0.58}^{+0.70}.
    • There is approximately a 50% chance of obtaining similar Bayes factors even without p-g effects.
    • Constraints on the p-g amplitude for 1.4 solar mass neutron stars are less than a few tenths of the theoretical maximum, with a saturation frequency around 70 Hz.

    Conclusions:

    • The study rules out extreme values for the p-g instability parameters.
    • The energy dissipated by this instability is less than a few percent of the total gravitational wave energy radiated.
    • Further observations and refined models are needed to definitively probe the role of p-g mode instabilities in neutron star mergers.