Electrohydrodynamics

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A simulation of the 3D magnetohydrodynamics at play in the outer third of a star. Each “hair” represents a magnetic field line embedded in the stellar plasma flow. Near the equator, the convective flows tend to align with the axis of rotation; in higher latitudes the convection is more cyclonic. Image produced using VAPOR
Copyright 2007 International Science Grid This Week

iSGTW Image of the week - Solar magnetic fields

September 5, 2007
A simulation of the 3D magnetohydrodynamics at play in the outer third of a star. Each “hair” represents a magnetic field line embedded in the stellar plasma flow. Near the equator, the convective flows tend to align with the axis of rotation; in higher latitudes the convection is more cyclonic.

Image produced using VAPOR

Complicated by wild convection occurring in the outer third of a star’s plasma, and by rotation that twists a star’s magnetic field into a spiral, stellar magnetohydrodynamics really is as complex as it sounds.
Magnetohydrodynamics is the study of motion and magnetism in conducting fluids such as plasmas, liquid metals and seawater.
The “hydro” bit refers to fluids, the “dynamics” bit means movement, and the “magneto” part comes into play because magnetic fields induce currents in moving conductive fluids, and are themselves amplified by the fluids’ motions.

Retrieved by DonEMitchell (talk) 15:25, 22 October 2013 (MDT) from http://www.isgtw.org/visualization/isgtw-image-week-solar-magnetic-fields