  The problem of Astrophysical Jet formation from relativistic accretion disks
through the establishment of relativistic disk-powerful jet equilibrium
structure is studied applying the Beltrami-Bernoulli equilibrium approach of
Shatashvili & Yoshida 2011; Arshilava et al. 2019. Accretion disk is weakly
magnetized consisting of fully ionized relativistic electron-ion plasma and
photon gas strongly coupled to electrons due to Thompson Scattering. %hence,
making the behavior of photon gas similar to that of "a charged fluid".
Analysis is based on the generalized Shakura-Sunyaev $\alpha $-turbulent
dissipation model for local viscosity (being the main source of accretion), in
which the contributions from both the photon and ion gases are taken into
account. Ignoring the self-gravitation in the disk we constructed the
analytical self-similar solutions for the equilibrium relativistic disk-jet
structure characteristic parameters in the field of gravitating central compact
object for the force-free condition. It is shown, that the magnetic field
energy in the Jet is several orders greater compared to that of accretion disk,
while jet-outflow is locally Super-Alfv\'enic with local {\it Plasma-beta} $<
1$ near the jet-axis. The derived solutions can be used to analyze the
astrophysical jets observed in binary systems during the star formation process
linking the jet properties with the parameters of relativistic accretion disks
of electron-ion-photon gas.
