  A high sensitivity, 7mm Very Long Baseline Array image of M\,87 was
previously analyzed in order to estimate the bulk flow jet velocity between 0.4
and 0.65 mas from the point of origin using the asymmetry between the
well-characterized double-ridged counter-jet (unique to this image) and the
double ridged jet. We use this same image to estimate the cross-sectional area
of this tubular stream. The velocity, acceleration, cross-sectional area and
flux density along this stream determines a unique, perfect magnetohydrodynamic
jet solution that satisfies, conservation of energy, angular momentum and mass
(a monotonic conversion of Poynting flux to kinetic energy flux along the jet).
The solution is protonic and magnetically dominated. The bilateral jet
transports $\approx 1.2\times10^{-4} M_{\odot}/\rm{yr}$ and $\approx
1.1\times10^{42}$ erg/sec, placing strong constraints on the central engine. A
Keplerian disk source that also produces the Event Horizon Telescope (EHT)
annulus of emission can supply the energy and mass if the vertical magnetic
field at the equator is $\sim 1-3.5$ G (depending on location). A Parker spiral
magnetic field, characteristic of a wind or jet, is consistent with the
observed EHT polarization pattern. Even though there is no image of the jet
connecting with the annulus, it is argued that these circumstances are not
coincidental and the polarized portion of the EHT emission is mainly jet
emission in the top layers of the disk that is diluted by emission from an
underlying turbulent disk. This is a contributing factor to the relatively low
polarization levels that were detected.
