Coupling of neutrino beam-driven MHD waves and resonant instabilities in rotating magnetoplasmas with neutrino two-flavor oscillations

TL;DR

This paper analyzes how neutrino-driven MHD waves and instabilities in rotating magnetoplasmas are coupled by the Coriolis force, revealing new wave modes and instabilities relevant to supernovae dynamics.

Contribution

It demonstrates for the first time the coupling of shear Alfvén and magnetosonic waves by the Coriolis force in neutrino-influenced plasmas, including effects of neutrino oscillations.

Findings

Neutrino effects influence shear Alfvén waves.

Magnetosonic waves exhibit higher instability growth rates than Alfvén waves.

Instability timescales align with supernova explosion timescales.

Abstract

We present an analysis of neutrino-driven magnetohydrodynamic (MHD) waves and instabilities in a rotating magnetoplasma with weak neutrino interactions. We show, for the first time, that neutrino-driven shear Alfv{\'e}n and oblique magnetosonic waves can be coupled by the Coriolis force, forming new wave modes affected by this force, as well as neutrino beam and two neutrino flavor oscillations. Our work extends previous theories by demonstrating that shear Alfv{\'e}n waves are influenced by neutrino effects and by identifying instabilities resulting from resonant interactions with both a streaming neutrino beam and flavor oscillations. We find that the Coriolis force, as well as plasma density and magnetic field strength, significantly affect the profiles of the instability growth rates. Such a growth rate for magnetosonic waves appears much higher than the Alfv{\'e}n wave, implying that magnetosonic waves provide a superior mechanism for energy extraction from the neutrino beam. For typical parameters relevant to the protoneutron star surface, the instability time for magnetosonic waves may vary in the range 0.09-0.14 s, which is within the predicted time of the neutrino-driven explosion (0.3 s after bounce) reported in the recent three-dimensional MHD simulations of core-collapse supernovae. Our findings may shed new light on the physical mechanisms underlying core-collapse supernovae.