  A magnetic flux tube may be considered both as a separate body and as a
confined field. As a field, it is affected both by the cyclonic convection
($\alpha$-effect) and differential rotation ($\Omega$-effect). As a body, the
tube experiences not only a buoyant force, but also a dynamic pressure due to
downflows above the tube. When these two dynamic effects are incorporated into
the $\alpha\Omega$ dynamo equations, we obtain a dynamo operating in the
convection zone. We analyze and solve the extended dynamo equations in the
linear approximation by using observed solar internal rotation and assuming a
downflow suggested by numerical simulations of the solar convection zone. The
results produce: (i) the 22-year cycle period; (ii) the extended butterfly
diagram; (iii) the confinement of strong activity to low heliographic latitudes
$|\Phi|\le 35^\circ$; (iv) at low latitudes the radial field is in an
approximately $\pi$ phase lag compared to the toroidal field at the same
latitude; (v) the poleward branch is in a $\pi/2$ phase lag with respect to the
equatorward branch; (vi) most of the magnetic flux is present in a strongly
intermittent form, concentraed into strong flux tubes; (vii) the magnetic field
peaks at a depth of $r=0.96 R_{\sun}$; (viii) total solar irradiance varies in
phase with the solar cycle activity, having an amplitude of 0.1%; (ix) solar
effective temperature varies in phase with the solar cycle activity, having an
amplitude of 1.5 $^\circ C$; and (x) solar radius also varies in phase with the
solar cycle activity, having an amplitude of 20 mas. All these results are in
agreement with the corresponding observations.
