  The solar dynamo and the solar Global internal Magnetic Structure (GMS)
appear to be a thin ($\sim$2 Mm thick) structure near ($\sim$1 Mm below) the
solar surface. Evidence for these properties are found from the amplitude of
the torsional oscillations and in their velocity contours relationship to solar
magnetogram; the power to the chromosphere; power to the corona and the solar
wind; the current in the helio-current-sheet measured at the radius of the
orbit of Earth; the calculated size ($\sim$1 Mm) of the expanding polar flux
when it enters the photosphere; and from the observation that solar magnetic
activity is generated near the surface. A thin stable minimum energy state
seems to be covering most of the solar surface just below the photosphere. The
magnetic field lines should be parallel to the solar surface and rotate with
distance from the surface for 2$\pi$ radians in $\sim$2 Mm. Resistive diffusion
helps to push the magnetic fields to the surface and the GMS seems to lose
$\pi$ radians every 11 years, causing the observed 180$^\circ$ flipping of the
solar magnetic fields including the flipping of the polar flux. Further
evidence for this GMS and its loss is that solar prominences are made of thin
sheets of magnetized plasma, which are, likely, remnants of the lost thin sheet
of the GMS. The loss process is consistent with the butterfly pattern of the
sunspots and with the differences observed between solar maximum and solar
minimum in the corona. The solar dynamo drives current parallel to the polar
flux, which, in turn, sustains the GMS using cross-field current drive. For
completeness, the formation of sunspots, CMEs and flares is discussed.
