Abstract
AbstractThe long‐awaited detection of a gravitational wave from the merger of a binary neutron star in August 2017 (GW170817) marked 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 was possible to constrain several global properties of the equation of state of neutron star matter. By means of fully general‐relativistic hydrodynamic simulations, it is possible to get an insight into the hydrodynamic evolution of matter and into the structure of the space–time deformation caused by the remnant of binary neutron star merger. Neutron star mergers represent an optimal astrophysical laboratory to investigate the phase transition from confined hadronic matter to deconfined quark matter. With future gravitational wave detectors, it will most likely be possible in the near future to investigate the hadron‐quark phase transition by analyzing the spectrum of the post‐merger gravitational wave of the differentially rotating hypermassive hybrid star. In contrast to hypermassive neutron stars, these highly differentially rotating objects contain deconfined strange quark matter in their slowly rotating inner region.
Highlights
By means of fully general-relativistic hydrodynamic simulations, it is possible to get an insight into the hydrodynamic evolution of matter and into the structure of the space–time deformation caused by the remnant of binary neutron star merger
The effects of a strong hadron to quark phase transition (HQPT) have been investigated in the context of static (Hanauske & Greiner 2001; Mishustin et al 2003; Shovkovy et al 2003) and uniformly rotating hybrid stars (Banik et al 2004; Bhattacharyya et al 2005; Glendenning et al 1997) and the results show that tremendous changes in the star properties might occur including the existence of a third family of compact stars—the so-called “twin stars” (Alford & Sedrakian 2017; Glendenning & Kettner 2000; Hanauske & Greiner 2001; Mishustin et al 2003)
Astrophysical observables of the HQPT were discussed in the context of the inspiral and post-merger phase, with a main focus on the delayed phase transition (DPT) scenario
Summary
The study of astrophysical processes was limited to events visible with the eyes, and optical telescopes did not develop until the 16th century. The entire perceived image that we had of our universe was limited to astrophysical phenomena that generate electromagnetic radiation This circumstance changed in the 21st century with the detection of gravitational waves. Space-based gamma-ray telescopes (e.g., the Fermi’s gamma-ray burst monitor or the Swift gamma-ray burst mission) detect on average approximately one gamma-ray burst per day—the gamma-ray burst (LIGO Scientific Collaboration et al 2017) that had been associated with GW170817 is an outstanding event and, in addition, with the observations of the electromagnetic counterparts of the associated kilonova, provides a conclusive picture of the whole merger event This coincidence of the direct detection of a gravitational wave from a neutron star collision with the emitted short gamma-ray burst was the first observational proof that binary neutron star mergers generate short gamma-ray bursts. Constraints on cosmic strings (The LIGO Scientific Collaboration, the Virgo Collaboration, & the KAGRA Collaboration 2021a) and upper limits on continuous gravitational-wave signals from the young pulsar PSR J0537-6910 (The LIGO Scientific Collaboration, the Virgo Collaboration, & the KAGRA Collaboration 2020) and on the isotropic gravitational-wave background (The LIGO Scientific Collaboration, the Virgo Collaboration, & the KAGRA Collaboration 2021b) could be specified
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