Abstract
As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a crossover transition to quark matter. We discuss how the late time gravitational wave emission from binary neutron star mergers may possibly reveal the existence of a crossover transition to quark matter.
| Original language | English |
|---|---|
| DOIs | |
| State | Published - 2022 |
| Externally published | Yes |
| Event | 15th Conference on Quark Confinement and the Hadron Spectrum, Confinement 2022 - Stavanger, Norway Duration: Aug 1 2022 → Aug 6 2022 |
Conference
| Conference | 15th Conference on Quark Confinement and the Hadron Spectrum, Confinement 2022 |
|---|---|
| Country/Territory | Norway |
| City | Stavanger |
| Period | 08/1/22 → 08/6/22 |
Funding
Kim for continuous support. The work of H.I.K. was supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education through the Center for Quantum Spacetime (CQUeST) of Sogang University (Grant No. NRF-2020R1A6A1A03047877). This research used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC05-00OR22725. Work at the Center for Astrophysics of the University of Notre Dame is supported by the U.S. Department of Energy under Nuclear Theory Grant No. DE-FG02-95-ER40934. This research was supported in part by the Notre Dame Center for Research Computing through the high performance computing resources. H.I.K. graciously thanks Jinho Kim and Chunglee Figure 3: Power spectral density (2h˜(f)f1/2) as a function of frequency for various simulations as labelled and shown on Figure 2. The upper green curve shows the LIGO sensitivity while the lower blue and orange curves show anticipated sensitivity of the Einstein Telescope and Cosmic Explorer, respectively. The first peak at around 1 kHz for all of the simulations corresponds to the initial contact of the merging binaries. The second peak near 2 kHz corresponds to the maximum chirp strain, fmax, while the third peak, at around 3 kHz corresponds to the long postmerger phase, fpeak.
| Funders | Funder number |
|---|---|
| CQUeST | |
| Center for Quantum Spacetime | |
| Notre Dame Center for Research Computing | |
| U.S. Department of Energy | DE-FG02-95-ER40934 |
| Office of Science | DE-AC05-00OR22725 |
| Sogang University | NRF-2020R1A6A1A03047877 |
| Ministry of Education | |
| National Research Foundation of Korea |