Where are the r-modes of isentropic stars?

TL;DR

This paper investigates the absence and nature of r-modes and g-modes in isentropic stars, revealing they are hybrid modes split by rotation, with implications for gravitational-wave emission in neutron stars.

Contribution

It demonstrates that in isentropic stars, r-modes and g-modes do not exist as pure modes but become hybrid modes due to rotation, and introduces a novel numerical method to compute these modes.

Findings

Pure r-modes are absent in isentropic stars.

Modes are hybrid, combining axial and polar parts, split by rotation.

Computed gravitational-wave instability timescales for neutron stars.

Abstract

Almost none of the r-modes ordinarily found in rotating stars exist, if the star and its perturbations obey the same one-parameter equation of state; and rotating relativistic stars with one-parameter equations of state have no pure r-modes at all, no modes whose limit, for a star with zero angular velocity, is a perturbation with axial parity. Similarly (as we show here) rotating stars of this kind have no pure g-modes, no modes whose spherical limit is a perturbation with polar parity and vanishing perturbed pressure and density. Where have these modes gone? In spherical stars of this kind, r-modes and g-modes form a degenerate zero-frequency subspace. We find that rotation splits the degeneracy to zeroth order in the star's angular velocity $\Omega$, and the resulting modes are generically hybrids, whose limit as $\Omega\to 0$ is a stationary current with axial and polar parts. Because each mode has definite parity, its axial and polar parts have alternating values of $l$. We show that each mode belongs to one of two classes, axial-led or polar-led, depending on whether the spherical harmonic with lowest value of $l$ that contributes to its velocity field is axial or polar. We numerically compute these modes for slowly rotating polytropes and for Maclaurin spheroids, using a straightforward method that appears to be novel and robust. Timescales for the gravitational-wave driven instability and for viscous damping are computed using assumptions appropriate to neutron stars.