The optical spectra of Nova Herculis 1991 (V838 Her) clearly show it to be a member of the class of novae that occur on ONeMg white dwarfs. In addition, Nova Her 1991 exhibits anomalous abundances in certain intermediate-mass elements. Photoionization modeling reveals sulfur to be greatly enhanced relative to solar abundances and nitrogen to be enhanced relative to oxygen. Comparison with published hydrodynamic models of Starrfield and collaborators implies that the progenitor was an ONeMg white dwarf with a mass of 1.30.-1.35 M ○. . The detailed velocity structure of the emission lines reveals the presence of five main components, probably corresponding to clumps in the ejecta
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