Identifying QCD Phase Transitions via the Gravitational Wave Frequency from a Supernova Explosion - INSPIRE

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Identifying QCD Phase Transitions via the Gravitational Wave Frequency from a Supernova Explosion

Zhan Bai
(
- Peking U. and
- Peking U., SKLNPT
)
,
Wei-jie Fu
(
- Dalian U. Tech.
)
,
Yu-xin Liu
(
- Peking U. and
- Peking U., SKLNPT and
- CICQM, Beijing and
- Peking U., CHEP
)

Sep 26, 2021

18 pages

Published in:

Astrophys.J. 922 (2021) 2, 266

Published: Dec 6, 2021

e-Print:

2109.12614 [nucl-th]

DOI:

10.3847/1538-4357/ac2a31

View in:

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Abstract: (IOP)

We investigate the nonradial oscillations of newly born neutron stars (NSs) and strange quark stars (SQSs). This is done with the relativistic nuclear field theory with hyperon degrees of freedom employed to describe the equation of state (EoS) for the stellar matter in NSs, and with both the MIT bag model and the Nambu–Jona-Lasinio model adopted to construct the configurations of the SQSs. We find that the gravitational-mode (g-mode) eigenfrequencies of newly born SQSs are significantly lower than those of NSs, which is independent of models implemented to describe the EoS for the strange quark matter. Meanwhile, the eigenfrequencies of the other modes of nonradial oscillations, e.g., fundamental (f)- and pressure (p)-modes, are much larger than those of the g-mode, and are related to the stiffness of the EoSs. In light of the first direct observation of gravitational waves (GWs), it is promising to employ GWs to identify the QCD phase transition in high-density strong-interaction matter.

Note:

22 pages, 10 figures, Extension of arXiv:1701.00418. Version to appear in AstroPhys. J

quantum chromodynamics: critical phenomena
quark: matter
quark: star
gravitational radiation: frequency
matter: strangeness
matter: strong interaction
density: high
equation of state
oscillation
supernova

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