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Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai's Star)*
After becoming ionized, low-density astrophysical plasmas will begin a process of slow recombination. Models for this still have significant uncertainties. Recombination cannot normally be observed in isolation, because the ionization follows the evolutionary timescale of the ionizing source. Laboratory experiments are unable to reach the appropriate conditions because of the very long required timescales. The extended nebula around the very late helium pulse (VLTP) star V4334 Sgr provides adoi:10.3847/1538-4357/ac90c4 fatcat:b5xi4r4pxzf6vcfdzfs7sfynvq