Yes, internal energy can be used as an additional "pool of energy" to feed a flow's acceleration, but even that can be related back to pressure as I showed previously. You just factor in the ratio of specific heats. If you would like more, allow me to show you exactly how to arrive at the isentropic pressure relationship for any compressible flow. Again, start with the energy equation in terms of enthalpy, which is ##h = e + p/\rho##.
d\left( h + \dfrac{V^2}{2}\right) = 0
Let's treat this as being a statement about the relationship between two states: one at rest and one at any arbitrary velocity, ##V##:
h_0 = h +\dfrac{V^2}{2}
We can assume the gas is calorically perfect (we aren't talking about super hot or cold things here so it's a good assumption), so ##h = c_p T##:
c_p T_0 = c_p T + \dfrac{V^2}{2}
From the ideal gas law, we know that ##p = \rho R T##, so
\dfrac{c_p p_0}{\rho_0 R} = \dfrac{c_p p}{\rho R} + \dfrac{V^2}{2}.
I already showed that ##c_p/R## can be cast in terms of ##\gamma## for the gas, so
\left( \dfrac{\gamma}{\gamma -1} \right)\dfrac{p_0}{\rho_0} = \left( \dfrac{\gamma}{\gamma -1} \right)\dfrac{p}{\rho} + \dfrac{V^2}{2}
or
\dfrac{p_0}{\rho_0} = \dfrac{p}{\rho} + \left( \dfrac{\gamma - 1}{\gamma} \right)\dfrac{V^2}{2}
If you divide through by ##RT##, you end up with a term that is ##a^2 = \gamma R T##, which, when combined with ##V^2## gives the square of the Mach number:
\dfrac{p_0}{\rho_0 RT} = \dfrac{p}{\rho RT} + \left( \dfrac{\gamma - 1}{2} \right)M^2
Also note that ##p/(\rho R T) = 1## from the ideal gas law, so
\dfrac{p_0}{\rho_0 RT} = 1 + \left( \dfrac{\gamma - 1}{2} \right)M^2
So far that is getting more useful than what we had before, but ideally, we'd like to keep this in terms of only pressure and Mach number, which means it would be nice to cast the ##\rho_0## term in terms of ##\rho## (so that it can be converted into a pressure term due to the ideal gas assumption and the ##RT## term) and pressures. Luckily, isentropic gas relations give us this. We know that
\dfrac{\rho}{\rho_0} = \left( \dfrac{p}{p_0} \right)^{1/\gamma}
so if you solve that for ##\rho_0##, the resulting ##\rho RT## term becomes a ##p## and, and after some algebra the final relationship is
\boxed{ \dfrac{p}{p_0} = \left[ 1 + \left( \dfrac{\gamma-1}{2} \right)M^2 \right]^{-\frac{\gamma}{\gamma-1}} }
This is a very classical result, and hopefully the derivation has proven to you that it already takes into account the change in ##e## associated with acceleration of the gas to a higher speed. This is isentropic, so it also applies to slowing a flow back down. It's an energy conservation statement. It also has a maximum at ##M=0## (see plot below that includes the equivalent relations for ##T## and ##\rho##) so no matter what process you use to speed it up and no matter what it then impacts, the maximum stagnation pressure it can recover is still the same stagnation pressure that occurred upstream when it was at rest. That's true whether you are talking about bringing it up to sonic velocity at a throat or supersonic velocity downstream. Of course, if it is supersonic, that means that slowing it down likely incurs a shock, which is not an isentropic process and dissipates some of the available energy, meaning you recover less total pressure even when slowing to zero. The bottom line is that you will never increase total pressure without adding energy to the system. This is dictated by the second law of thermodynamics.
I'll even do you one further. Using a similar analysis to that which I did above, you can get similar relations for ##rho## and ##T##, which are plotted above. You can also pick a Mach number you'd like to use and use its relationship with velocity, namely ##V = Ma## to derive a relationship for a dimensionless momentum flux (##\rho u^2## in a one-dimensional flow) as a function of the ##M## and ##\gamma##.
So, the end result is that if you assume you have expanded your flow to be moving one dimensionally, then the plot of momentum flux versus Mach number looks like the following:
So, there actually
is a peak in momentum flux that occurs as ##M\approx 1.41##. Momentum flux is probably the closest related quantity to force on an object it eventually hits. If you imagine an object redirecting all of that momentum flux, then it requires a force in order to do that. However, this has nothing (directly) to do with pressure (or "effective pressure", whatever that may be), and you can never recover more pressure than exists in the form of total or stagnation pressure.
In case you were curious, I also included similar plots for mass flux, ##\rho u## (the maximum is unsurprisingly at ##M=1##) and the kinetic energy flux, ##\rho u^3##, which has a maximum at ##M\approx 1.73##.