g-mode oscillations in hybrid stars: A tale of two sounds
Abstract
We study the principal core g-mode oscillation in hybrid stars containing quark matter and find that they have an unusually large frequency range ( ≈ 200 - 600 Hz) compared to ordinary neutron stars or self-bound quark stars of the same mass. Theoretical arguments and numerical calculations that trace this effect to the difference in the behaviour of the equilibrium and adiabatic sound speeds in the mixed phase of quarks and nucleons are provided. We propose that the sensitivity of core g-mode oscillations to non-nucleonic matter in neutron stars could be due to the presence of a mixed quark-nucleon phase. Based on our analysis, we conclude that for binary mergers where one or both components may be a hybrid star, the fraction of tidal energy pumped into resonant g-modes in hybrid stars can exceed that of a normal neutron star by a factor of 2-3, although resonance occurs during the last stages of inspiral. A self-bound star, on the other hand, has a much weaker tidal overlap with the g-mode. The cumulative tidal phase error in hybrid stars, ΔΦ = 0.5 rad, is comparable to that from tides in ordinary neutron stars, presenting a challenge in distinguishing between the twomore »
- Authors:
-
[1];
[2];
[2];
[3]
- California State Univ. (CalState), Long Beach, CA (United States)
- Ohio Univ., Athens, OH (United States)
- Trento Institute of Fundamental Physics and Applications, Povo (Italy). INFN-TIFPA; European Centre for Theoretical Studies in Nuclear Physics and Related Areas, Villazzano, Trento (Italy)
- Publication Date:
- Research Org.:
- Ohio Univ., Athens, OH (United States)
- Sponsoring Org.:
- USDOE Office of Nuclear Energy (NE), Nuclear Infrastructure Programs; USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF); Marie Skłodowska-Curie
- OSTI Identifier:
- 1831784
- Alternate Identifier(s):
- OSTI ID: 1798636; OSTI ID: 1831785
- Grant/Contract Number:
- FG02-93ER40756; PHY-1608959; PHY-1913693; 754496
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review. D.
- Additional Journal Information:
- Journal Volume: 103; Journal ID: ISSN 2470-0010
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; 79 ASTRONOMY AND ASTROPHYSICS; Gravitational wave sources; Nuclear matter in neutron stars; Neutron stars & pulsars
Citation Formats
Jaikumar, Prashanth, Semposki, Alexandra, Prakash, Madappa, and Constantinou, Constantinos. g-mode oscillations in hybrid stars: A tale of two sounds. United States: N. p., 2021.
Web. doi:10.1103/PhysRevD.103.123009.
Jaikumar, Prashanth, Semposki, Alexandra, Prakash, Madappa, & Constantinou, Constantinos. g-mode oscillations in hybrid stars: A tale of two sounds. United States. https://doi.org/10.1103/PhysRevD.103.123009
Jaikumar, Prashanth, Semposki, Alexandra, Prakash, Madappa, and Constantinou, Constantinos. Mon .
"g-mode oscillations in hybrid stars: A tale of two sounds". United States. https://doi.org/10.1103/PhysRevD.103.123009. https://www.osti.gov/servlets/purl/1831784.
@article{osti_1831784,
title = {g-mode oscillations in hybrid stars: A tale of two sounds},
author = {Jaikumar, Prashanth and Semposki, Alexandra and Prakash, Madappa and Constantinou, Constantinos},
abstractNote = {We study the principal core g-mode oscillation in hybrid stars containing quark matter and find that they have an unusually large frequency range ( ≈ 200 - 600 Hz) compared to ordinary neutron stars or self-bound quark stars of the same mass. Theoretical arguments and numerical calculations that trace this effect to the difference in the behaviour of the equilibrium and adiabatic sound speeds in the mixed phase of quarks and nucleons are provided. We propose that the sensitivity of core g-mode oscillations to non-nucleonic matter in neutron stars could be due to the presence of a mixed quark-nucleon phase. Based on our analysis, we conclude that for binary mergers where one or both components may be a hybrid star, the fraction of tidal energy pumped into resonant g-modes in hybrid stars can exceed that of a normal neutron star by a factor of 2-3, although resonance occurs during the last stages of inspiral. A self-bound star, on the other hand, has a much weaker tidal overlap with the g-mode. The cumulative tidal phase error in hybrid stars, ΔΦ = 0.5 rad, is comparable to that from tides in ordinary neutron stars, presenting a challenge in distinguishing between the two cases. Furthermore, should the principal g-mode be excited to sufficient amplitude for detection in a postmerger remnant with quark matter in its interior, its frequency would be a possible indication for the existence of non-nucleonic matter in neutron stars.},
doi = {10.1103/PhysRevD.103.123009},
journal = {Physical Review. D.},
number = ,
volume = 103,
place = {United States},
year = {Mon Jun 07 00:00:00 EDT 2021},
month = {Mon Jun 07 00:00:00 EDT 2021}
}
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