# Dissipation triggers dynamical two-stream instability

## TL;DR

This paper demonstrates that dissipation in relativistic two-fluid systems can convert energetic instabilities into dynamical ones, leading to exponential growth modes, with implications for neutron star physics.

## Contribution

It reveals that dissipation causes energetic instabilities to become dynamical in relativistic fluids, a general result applicable to astrophysical systems like neutron stars.

## Key findings

- Dissipation induces exponential growth modes in relativistic fluids.
- Energetic instability becomes dynamical due to dissipation.
- Mode analogous to neutron star r-mode can be unstable at small counterflows.

## Abstract

Two coupled, interpenetrating fluids suffer instabilities beyond certain critical counterflows. For ideal fluids, an energetic instability occurs at the point where a sound mode inverts its direction due to the counterflow, while dynamical instabilities only occur at larger relative velocities. Here we discuss two relativistic fluids, one of which is dissipative. Using linearized hydrodynamics, we show that in this case the energetic instability turns dynamical, i.e., there is an exponentially growing mode, and this exponential growth only occurs in the presence of dissipation. This result is general and does not rely on an underlying microscopic theory. It can be applied to various two-fluid systems for instance in the interior of neutron stars. We also point out that under certain circumstances the two-fluid system exhibits a mode analogous to the r-mode in neutron stars that can become unstable for arbitrarily small values of the counterflow.