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Inferring the dense nuclear matter equation of state with neutron star tides

Published online by Cambridge University Press:  27 February 2023

Pantelis Pnigouras Open the ORCID record for Pantelis Pnigouras [Opens in a new window]  and
Nils Andersson
Pantelis Pnigouras
Affiliation:
Dipartimento di Fisica, “Sapienza” Università di Roma & Sezione INFN Roma1, Piazzale Aldo Moro 2, 00185 Roma, Italy email: pantelis.pnigouras@uniroma1.it Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
Nils Andersson
Affiliation:
School of Mathematics and STAG Research Centre, University of Southampton, SO17 1BJ Southampton, UK
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Abstract

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During the late stages of a neutron star binary inspiral finite-size effects come into play, with the tidal deformability of the supranuclear density matter leaving an imprint on the gravitational-wave signal. As demonstrated in the case of GW170817—the first direct detection of gravitational waves from a neutron star binary—this can lead to strong constraints on the neutron star equation of state. As detectors become more sensitive, effects which may have a smaller influence on the neutron star tidal deformability need to be taken into consideration. Dynamical effects, such as oscillation mode resonances triggered by the orbital motion, have been shown to contribute to the tidal deformability, especially close to the neutron star coalesence. We calculate the contribution of the various stellar oscillation modes to the tidal deformability and demonstrate the (anticipated) dominance of the fundamental mode, showing what the impact of the matter composition is on the tidal deformability.

Keywords

dense matterequation of stategravitational wavesrelativitymethods: analytical(stars:) binaries: generalstars: neutronstars: oscillations (including pulsations)
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 191 - 194
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Abbott, B. P. et al. 2017, Phys. Rev. Lett., 119, 161101 CrossRefGoogle ScholarPubMed
Andersson, N. & Pnigouras, P. 2020, Phys. Rev. D, 101, 083001 CrossRefGoogle Scholar
Passamonti, A., Andersson, N., & Pnigouras, P. 2021, Mon. Not. R. Astron. Soc., 504, 1273 CrossRefGoogle Scholar
Schmidt, P. & Hinderer, T. 2019, Phys. Rev. D, 100, 021501 CrossRefGoogle Scholar
Andersson, N. & Pnigouras, P. 2021, Mon. Not. R. Astron. Soc., 503, 533 CrossRefGoogle Scholar
Flanagan, É. É. & Hinderer, T. 2008, Phys. Rev. D, 77, 021502 CrossRefGoogle Scholar
Abbott, B. P. et al. 2020, Astrophys. J., 892, L3 CrossRefGoogle Scholar
Pratten, G., Schmidt, P., & Williams, N. 2021, ArXiv e-prints, 2109.07566Google Scholar