Detecting the Hadron-Quark Phase Transition with Gravitational Waves
Abstract
The long-awaited detection of a gravitational wave from the merger of a binary neutron star in August 2017 (GW170817) marks the beginning of the new field of multi-messenger gravitational wave astronomy. By exploiting the extracted tidal deformations of the two neutron stars from the late inspiral phase of GW170817, it is now possible to constrain several global properties of the equation of state of neutron star matter. However, the most interesting part of the high density and temperature regime of the equation of state is solely imprinted in the post-merger gravitational wave emission from the remnant hypermassive/supramassive neutron star. This regime was not observed in GW170817, but will possibly be detected in forthcoming events within the current observing run of the LIGO/VIRGO collaboration. Numerous numerical-relativity simulations of merging neutron star binaries have been performed during the last decades, and the emitted gravitational wave profiles and the interior structure of the generated remnants have been analysed in detail. The consequences of a potential appearance of a hadron-quark phase transition in the interior region of the produced hypermassive neutron star and the evolution of its underlying matter in the phase diagram of quantum cromo dynamics will be in the focus of this article. It will be shown that the different density/temperature regions of the equation of state can be severely constrained by a measurement of the spectral properties of the emitted post-merger gravitational wave signal from a future binary compact star merger event.
Additional Information
© 2019 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/). This article belongs to the Special Issue Compact Stars in the QCD Phase Diagram and in the Multi-Messenger Era of Astronomy. We would like to thank Luciano Rezzolla. Without his profound knowledge and his comprehensive expertise in the field of numerical relativity and general relativistic hydrodynamics, the presented simulations and the whole article would not have been possible. Additionally, we would like to thank Glòria Montaña and Laura Tolos for valuable discussions. M.H. gratefully acknowledges support from the Frankfurt Institute for Advanced Studies (FIAS) and the Goethe University Frankfurt, V.D. acknowledges support from the National Science Foundation under grant PHY-1748621, while H.S. acknowledges the Judah M. Eisenberg laureatus Professur endowment. Author Contributions. Conceptualization, M.H., H.S.; Methodology, M.H., H.S., E.M., L.B., V.D.; Investigation, M.H., J.S., A.M., L.B., E.M., J.P., S.S., V.V., V.D.; Writing—Original Draft Preparation, M.H.; Writing—Review & Editing, M.H., V.D., H.S.; Funding Acquisition, H.S. The authors declare no conflict of interest.Attached Files
Published - universe-05-00156-v2.pdf
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Additional details
- Eprint ID
- 121247
- Resolver ID
- CaltechAUTHORS:20230502-434554000.2
- Frankfurt Institute for Advanced Studies
- Goethe University Frankfurt
- PHY-1748621
- NSF
- GSI Helmholtz Centre for Heavy Ion Research
- Created
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2023-05-04Created from EPrint's datestamp field
- Updated
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2023-05-04Created from EPrint's last_modified field