Analysis of radial and quasiradial oscillations in quark stars for different equations of state
Abstract
We investigate quark stars (QSs) described by three quark matter (QM)equations of state (EoSs) and analyse their radial and quasiradial oscillation modes within the slowly rotating relativistic approximation. The considered EoSs describe massless quarks, massive quarks, and massive quarks with a temperature-dependent gluon mass. Our analysis of radial modes shows that the mode separation depends on the stellar mass and radius for a given compactness, as well as on the stellar temperature. The considered QS models satisfy the slowly rotating relativistic condition of Hartle, Thorne and Chitre formalism, allowing rotation to be treated as a small perturbation of the non-rotating configuration. We find that, although more massive and larger stars can exhibit greater surface eccentricity and quadrupole deformation, their stronger self-gravity results in a lower tendency to deform than less massive and smaller stars. For all models, the variation in mass distribution increases towards the stellar surface, while the variations in pressure, energy density, and number density remain small near the center and become more pronounced towards the surface. More compact stars exhibit stronger twisting of the local inertial frame but weaker frame dragging for a given angular velocity. Rotation shifts the oscillation modes from their non-rotating values and leads to different vibrational decay times at different angular velocities. The fundamental modes considered here exhibit frequencies below $2$ kHz and show non-continuous behaviour across the investigated rotational configurations.
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BibTeX
@misc{rajbongshi2026analysis,
title = {{Analysis of radial and quasiradial oscillations in quark stars for different equations of state}},
author = {Nivamani Rajbongshi and Umananda Dev Goswami},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.27529},
eprint = {2609.27529},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.27529},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Analysis of radial and quasiradial oscillations in quark stars for different equations of state
AU - Nivamani Rajbongshi
AU - Umananda Dev Goswami
PY - 2026
DA - 2026/09/23
PB - arXiv
DO - 10.48550/arxiv.2609.27529
UR - https://arxiv.org/abs/2609.27529
AB - We investigate quark stars (QSs) described by three quark matter (QM)equations of state (EoSs) and analyse their radial and quasiradial oscillation modes within the slowly rotating relativistic approximation. The considered EoSs describe massless quarks, massive quarks, and massive quarks with a temperature-dependent gluon mass. Our analysis of radial modes shows that the mode separation depends on the stellar mass and radius for a given compactness, as well as on the stellar temperature. The considered QS models satisfy the slowly rotating relativistic condition of Hartle, Thorne and Chitre formalism, allowing rotation to be treated as a small perturbation of the non-rotating configuration. We find that, although more massive and larger stars can exhibit greater surface eccentricity and quadrupole deformation, their stronger self-gravity results in a lower tendency to deform than less massive and smaller stars. For all models, the variation in mass distribution increases towards the stellar surface, while the variations in pressure, energy density, and number density remain small near the center and become more pronounced towards the surface. More compact stars exhibit stronger twisting of the local inertial frame but weaker frame dragging for a given angular velocity. Rotation shifts the oscillation modes from their non-rotating values and leads to different vibrational decay times at different angular velocities. The fundamental modes considered here exhibit frequencies below $2$ kHz and show non-continuous behaviour across the investigated rotational configurations.
ER -