The Dispersion Relations and Instability Thresholds of Oblique Plasma Modes in the Presence of an Ion Beam

TL;DR

This paper analyzes how oblique plasma modes become unstable in the presence of an ion beam, explaining the lower threshold speeds for instability compared to parallel modes through quasilinear theory and resonance conditions.

Contribution

It provides a theoretical framework for understanding the instability thresholds of oblique plasma waves with ion beams, extending previous numerical results with analytical derivations.

Findings

Oblique modes have lower instability thresholds than parallel modes.

Resonance conditions determine the instability thresholds.

Wave polarization influences the wave-particle interactions.

Abstract

An ion beam can destabilize Alfv\'en/ion-cyclotron waves and magnetosonic/whistler waves if the beam speed is sufficiently large. Numerical solutions of the hot-plasma dispersion relation have previously shown that the minimum beam speed required to excite such instabilities is significantly smaller for oblique modes with $\vec k \times \vec B_0\neq 0$ than for parallel-propagating modes with $\vec k \times \vec B_0 = 0$, where $\vec k$ is the wavevector and $\vec B_0$ is the background magnetic field. In this paper, we explain this difference within the framework of quasilinear theory, focusing on low-$\beta$ plasmas. We begin by deriving, in the cold-plasma approximation, the dispersion relation and polarization properties of both oblique and parallel-propagating waves in the presence of an ion beam. We then show how the instability thresholds of the different wave branches can be deduced from the wave--particle resonance condition, the conservation of particle energy in the wave frame, the sign (positive or negative) of the wave energy, and the wave polarization. We also provide a graphical description of the different conditions under which Landau resonance and cyclotron resonance destabilize Alfv\'en/ion-cyclotron waves in the presence of an ion beam. We draw upon our results to discuss the types of instabilities that may limit the differential flow of alpha particles in the solar wind.