The Equation of State of Compact Stars

A special issue of Symmetry (ISSN 2073-8994). This special issue belongs to the section "Physics".

Deadline for manuscript submissions: 31 May 2025 | Viewed by 1857

Special Issue Editor


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Guest Editor
Institute of Nuclear Physics Polish Academy of Sciences, 31-342 Krakow, Poland
Interests: compact stars; dense matter; equation of state

Special Issue Information

Dear Colleagues,

The determination of the equation of state of compact stars is a modern, active field of research. Great development has been achieved by the recent multimessenger astronomy observations as well as by modern laboratory experiments. The necessary data include, for instance, detected gravitational radiation from merging neutron stars, radio, and X-ray emissions that are complemented by measurements of nuclear quantities in heavy ion collisions, nucleon scattering, and nuclear masses.

Nevertheless, there are many topics related to the composition of compact stars that urgently require detailed examination. We expect more observational and empirical data in the near future; thus, an account of the state of the art of this field is in order. As the Guest Editor, I would like to call for article contributions addressing the physics of compact star matter and related phenomena.

Submit your paper and select the Journal “Symmetry” and the Special Issue “The Equation of State of Compact Stars” via: MDPI submission system. Our papers will be published on a rolling basis and we will be pleased to receive your submission once you have finished it.

Dr. David Edwin Alvarez Castillo
Guest Editor

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Keywords

  • matter in canonical neutron star
  • the role of quantities such as nuclear incompressibility, nuclear symmetry energy, and nuclear effective mass
  • Nature of phase transitions in hybrid compact stars: first order, crossover
  • critical end points in the QCD phase diagram
  • dense matter in heavy ion collisions
  • hybrid stars in disconnected branches of the mass–radius diagram
  • quark stars with and without strangeness
  • impact of the EoS in compact star cooling processes
  • EoS with hyperon and boson content
  • hot dense nuclear matter in proto-compact stars and in mergers
  • methods of EoS determination from observables: Bayesian analyses, neural networks, machine learning approaches, effective field theories
  • dense matter in rotating compact stars
  • probing the compact star EoS with gravitational waves
  • the equation of state under the framework of alternative theories of gravity
  • dark matter in the compact star EoS

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Published Papers (1 paper)

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Research

15 pages, 695 KiB  
Article
Fundamental Oscillation Modes in Neutron Stars with Hyperons and Delta Baryons
by O. P. Jyothilakshmi, P. E. Sravan Krishnan, V. Sreekanth, Harsh Chandrakar and Tarun Kumar Jha
Symmetry 2025, 17(2), 230; https://doi.org/10.3390/sym17020230 - 5 Feb 2025
Viewed by 756
Abstract
For a new parameterization of the modified effective chiral model, developed primarily to regulate the density content of the symmetry energy and its higher order terms, equations of state (EoSs) for hyperon-rich matter (H) and delta baryon matter (Δ) [...] Read more.
For a new parameterization of the modified effective chiral model, developed primarily to regulate the density content of the symmetry energy and its higher order terms, equations of state (EoSs) for hyperon-rich matter (H) and delta baryon matter (Δ) were obtained. The models were used to investigate the emission of gravitational waves (GWs) through f-mode oscillations in the corresponding neutron stars. We obtained the stellar structure, f-mode frequency and tidal deformability Λ for our models. We report that the Δ EoS is stiffer compared to the H EoS. We also analyzed the velocity of sound in these media. The corresponding mass–radius relationships were obtained and compared with various observations. We studied the dependence of f-mode frequencies on the stellar mass, redshift and tidal deformability. We employed the well known Cowling approximation to obtain the f-mode frequencies for l=2,3 and 4 modes of oscillation. We found that the f-mode frequencies of the H and Δ EoSs were almost the same in the lower mass region, while we observed a substantial difference between them in the high-mass region. We also obtained an empirical relation for the EoSs considered. The various attributes obtained for our models showed close agreement with various observational constraints from pulsars and GW events. Full article
(This article belongs to the Special Issue The Equation of State of Compact Stars)
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