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HFG1 is the first well observed planetary nebula (PN) which reveals acometary-like structure. Its main morphological features consist of a bowshaped shell, which surrounds the central star, accompanied by a longcollimated tail. In this study we perform two-dimensional hydrodynamicsimulations modeling the formation of HFG1 from the interaction of the localambient medium with the mass outflows of its Asymptotic Giant Branch (AGB)progenitor star. We attribute the cometary appearance of HFG1 to the systemicmotion of the PN with respect to the local ambient medium. Due to its vitalimportance, we re-estimate the distance of HFG1 by modeling the spectral energydistribution of its central star, V664 Cas, and we find a distance of $ 490 \pm50$ pc. Our simulations show that none of our models with time invariantstellar wind and ambient medium properties are able to reproduce simultaneouslythe extended bow shock and the collimated tail observed in HFG1. Given this, weincrease the complexity of our modeling considering that the stellar wind istime variable. The wind description is based on the predictions of the AGB andpost-AGB evolution models. Testing a grid of models we find that the propertiesof HFG1 are best reproduced by the mass outflows of a 3 Msun AGB star. Such ascenario is consistent with the current observed properties of V664 Cas primarystar, an O-type subdwarf, and bridges the evolutionary history of HFG1 centralstar with the observables of the PN. We discuss the implications of our studyin the understanding of the evolution of AGB/post-AGB stars towards theformation of O-type subdwarfs surrounded by PNe.

Modeling the cometary structure of the planetary nebula HFG1 based on the evolution of its binary central star V664 Cas