On the linear structure of the interlaced Alfvén vortices in the tail of Uranus at solstice

Abstract

Incompressible vortex flow are observed in a large variety of astrophysical plasmas such as the convection zone and the atmosphere of stars, in astrophysical jets in stellar winds and in planetary magnetospheres. More specifically, magnetohydrodynamic (MHD) simulations have shown that two large scale interlaced Alfvénic vortices structure the magnetic tail of Uranus at solstice time. Assuming identical vortices, we compute the general linear structure of the flow near their centers within the frame of ideal MHD. We then use the analytic results to interpret and qualify the vortices observed in a 3D MHD simulation of a fast rotating Uranus-type planet.

References in corpus (12)

• Stability of Relativistic Jets from Rotating, Accreting Black Holes via Fully Three-Dimensional Magnetohydrodynamic Simulations
• Poynting Flux Dominated Jets in Decreasing Density Atmospheres. I. The Non-relativistic Current-driven Kink Instability and the Formation of "Wiggled" Structures
• Vortices in simulations of solar surface convection
• Stability of rotating magnetized jets in the solar atmosphere. I. Kelvin-Helmholtz instability
• On the plasma flow inside magnetic tornadoes on the Sun
• The Alfvénic nature of chromospheric swirls
• Kelvin-Helmholtz instability of twisted magnetic flux tubes in the solar wind
• Persistent magnetic vortex flow at a supergranular vertex
• Magnetic Tornado Properties: A Substantial Contribution to the Solar Coronal Heating via Efficient Energy Transfer
• Tornado-Like Evolution of A Kink-Unstable Solar Prominence
• Strong swirl approximation and intensive vortices in the atmosphere
• A physical model for the magnetosphere of Uranus at solstice time