Pumping of Magnetic Fields by PTCC

This research explores the transport of magnetic fields on the Solar surface by
Penetrative Turbulent Compressible Convection (PTCC).This research attempts to
better understand the process of solar magnetic field generation by
investigating the origin of strong magnetic fields that emerge at the solar
surface. This field is believed to be derived from a strong toroidal magnetic
field generated in a layer just below the base of the solar convection zone,
called the tachocline. The tachocline is a thin region of stability located
below the unstably stratified convection zone.

A thin horizontal magnetic field is arbitrarily introduced into the upper layer
of a simulated solar convection zone. To maintain constant pressure, the
density of the fluid inside the magnetic field is reduced. Hence the magnetic
field is buoyant relative to its surroundings. In the absence of convective
motion the magnetic field would rise. However, the highly turbulent convection
zone drags components of the magnetic field down into the stably stratified
layer by the advection of downward flowing plumes. As these plumes penetrate
the stable layer in an area called the "overshoot" region, they decelerate
rapidly. This rapid deceleration causes the plumes to "splash" and produce
numerous small vortices. These highly turbulent vortices stretch the magnetic
field and amplify its strength through local dynamo action. The net effect is a
redistribution of magnetic energy as the magnetic field is both pumped into the
tachocline region and then amplified.