Axial modes of anisotropic neutron stars are integrated numerically for realistic EOS; frequency falls with mass, damping time rises, and scaled quantities follow a near-universal quadratic in compactness that is largely EOS-insensitive but mildly model-dependent.
Anisotropic Quark Stars with an Interacting Quark Equation of State,
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
citation-role summary
background 1
citation-polarity summary
fields
gr-qc 2years
2026 2verdicts
UNVERDICTED 2roles
background 1polarities
background 1representative citing papers
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.
citing papers explorer
-
Nonradial oscillations of realistic anisotropic neutron stars: Axial modes
Axial modes of anisotropic neutron stars are integrated numerically for realistic EOS; frequency falls with mass, damping time rises, and scaled quantities follow a near-universal quadratic in compactness that is largely EOS-insensitive but mildly model-dependent.
-
Radial oscillations of quark stars in light of current astrophysical constraints: A comparative study
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.