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We present an analytical solution of a highly magnetized jet/wind flow. Theleft side of the general force-free jet/wind equation (the "pulsar" equation)is separated into a rotating and a nonrotating term. The two equations witheither term can be solved analytically, and the two solutions match each othervery well. Therefore, we obtain a general approximate solution of amagnetically dominated jet/wind, which covers from the nonrelativistic torelativistic regimes, with the drift velocity well matching the cold plasmavelocity. The acceleration of a jet includes three stages. (1) The jet flow islocated within the Alfv\'{e}n critical surface (i.e. the light cylinder), has anonrelativistic speed, and is dominated by toroidal motion. (2) The jet isbeyond the Alfv\'{e}n critical surface where the flow is dominated by poloidalmotion and becomes relativistic. The total velocity in these two stages followsthe same law $v\Gamma=\Omega R$. (3) The evolution law is replaced by$v\Gamma\approx1/\left(\theta\sqrt{2-\nu}\right)$, where $\theta$ is thehalf-opening angle of the jet and $0\leq\nu\leq2$ is a free parameterdetermined by the magnetic field configuration. This is because the earlierefficient acceleration finally breaks the causality connection betweendifferent parts in the jet, preventing a global solution. The jet has to carrylocal charges and currents to support an electromagnetic balance. Thisapproximate solution is consistent with known theoretical results and numericalsimulations, and it is more convenient to directly compare with observations.This theory may be used to constrain the spin of black holes in astrophysicaljets.

Analytical Solution of Magnetically Dominated Astrophysical Jets and Winds: Jet Launching, Acceleration, and Collimation