  We present the first 3D radiation-hydrodynamic simulations on the formation
and evolution of born-again planetary nebulae (PNe), with particular emphasis
to the case of HuBi1, the inside-out PN. We use the extensively-tested GUACHO
code to simulate the formation of HuBi1 adopting mass-loss and stellar wind
terminal velocity estimates obtained from observations presented by our group.
We found that, if the inner shell of HuBi1 was formed by an explosive very late
thermal pulse (VLTP) ejecting material with velocities of $\sim$300 km
s$^{-1}$, the age of this structure is consistent with that of $\simeq$200 yr
derived from multi-epoch narrow-band imaging. Our simulations predict that, as
a consequence of the dramatic reduction of the stellar wind velocity and photon
ionizing flux during the VLTP, the velocity and pressure structure of the outer
H-rich nebula are affected creating turbulent ionized structures surrounding
the inner shell. These are indeed detected in Gran Telescopio Canarias MEGARA
optical observations. Furthermore, we demonstrate that the current relatively
low ionizing photon flux from the central star of HuBi1 is not able to
completely ionize the inner shell, which favors previous suggestions that its
excitation is dominated by shocks. Our simulations suggest that the kinetic
energy of the H-poor ejecta of HuBi1 is at least 30 times that of the clumps
and filaments in the evolved born-again PNe A30 and A78, making it a truly
unique VLTP event.
