A Turbulent Heliosheath Driven by the Rayleigh–Taylor Instability

Abstract The heliosphere is the bubble formed by solar wind as it interacts with interstellar medium (ISM). collimation of heliosheath (HS) flows magnetic field in heliotail into distinct north and south columns (jets) seen recent global simulations heliosphere. However, there disagreement between models about how far downtail two-lobe feature persists whether ambient ISM penetrates region two lobes. Magnetohydrodynamic show that these heliospheric jets become unstable they move down drive large-scale turbulence. mechanism produces this turbulence had not been identified. Here we driver Rayleigh–Taylor (RT) instability produced interaction neutral H atoms streaming from ionized matter HS. drag acts an effective gravity, which causes RT to develop along axis HS field. A density gradient exists perpendicular due confinement characteristic timescale depends on for typical values growth rate ?3 years. destroys coherence reconnection ensues, allowing material penetrate tail. Signatures should be observable Energetic Neutral Atom maps future missions such Interstellar Mapping Acceleration Probe (IMAP). driven macroscopic potentially has important implications particle acceleration.