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We present the first 3D radiation-hydrodynamic simulations on the formationand evolution of born-again planetary nebulae (PNe), with particular emphasisto the case of HuBi1, the inside-out PN. We use the extensively-tested GUACHOcode to simulate the formation of HuBi1 adopting mass-loss and stellar windterminal velocity estimates obtained from observations presented by our group.We found that, if the inner shell of HuBi1 was formed by an explosive very latethermal pulse (VLTP) ejecting material with velocities of $\sim$300 kms$^{-1}$, the age of this structure is consistent with that of $\simeq$200 yrderived from multi-epoch narrow-band imaging. Our simulations predict that, asa consequence of the dramatic reduction of the stellar wind velocity and photonionizing flux during the VLTP, the velocity and pressure structure of the outerH-rich nebula are affected creating turbulent ionized structures surroundingthe inner shell. These are indeed detected in Gran Telescopio Canarias MEGARAoptical observations. Furthermore, we demonstrate that the current relativelylow ionizing photon flux from the central star of HuBi1 is not able tocompletely ionize the inner shell, which favors previous suggestions that itsexcitation is dominated by shocks. Our simulations suggest that the kineticenergy of the H-poor ejecta of HuBi1 is at least 30 times that of the clumpsand filaments in the evolved born-again PNe A30 and A78, making it a trulyunique VLTP event.

Formation and fate of the born-again planetary nebula HuBi 1