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.
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gr-qc 2years
2026 2verdicts
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Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and empirical expressions are given for both as functions of compactness and anisotrop
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