  One of the key challenges in solar and heliospheric physics is to understand
the acceleration of the solar wind. As a super-sonic, super-Alfv\'enic plasma
flow, the solar wind carries mass, momentum, energy, and angular momentum from
the Sun into interplanetary space. We present a framework based on two-fluid
magnetohydrodynamics to estimate the flux of these quantities based on
spacecraft data independent of the heliocentric distance of the location of
measurement. Applying this method to the Ulysses dataset allows us to study the
dependence of these fluxes on heliolatitude and solar cycle. The use of scaling
laws provides us with the heliolatitudinal dependence and the solar-cycle
dependence of the scaled Alfv\'enic and sonic Mach numbers as well as the
Alfv\'en and sonic critical radii. Moreover, we estimate the distance at which
the local thermal pressure and the local energy density in the magnetic field
balance. These results serve as predictions for observations with Parker Solar
Probe, which currently explores the very inner heliosphere, and Solar Orbiter,
which will measure the solar wind outside the plane of the ecliptic in the
inner heliosphere during the course of the mission.
