Planetary Nebulae and Sharp-Lined Displaced Features in White Dwarfs

Details Planetary Nebulae and Sharp-Lined Displaced Features in White Dwarfs Planetary Nebulae and Sharp-Lined Displaced Features in White Dwarfs

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1774b&link_type=abstract

IUE Proposal ID #IGGFB

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Scientific paper

Sharp shortward-shifted spectral features in two (2) hot white dwarfs and three (3) 0 subdwarfs indicate mass loss. The presence of such features in white dwarfs is quite puzzling. One possible explanation for the white dwarf features is that these lines are formed in old diffuse planetary nebulae. Yet, the presence of non-resonance lines of Si III in 2111+49 suggest a dense shell rather than an old planetary nebula. Since these stars have such large gravitational binding energies, other possible models might require "exotic" interpretations. Thus, the planetary nebula interpretation must be thoroughly explored before we consider such models. We identify five (5) early-type stars which would lie behind putative old planetary nebulae around the two white dwarfs exhibiting the shortward-displaced features. Observations of circumstellar material in the UV spectra of these stars could prove or disprove the old planetary nebula model. This question can be resolved with a small investment of IUE time, namely, one (1) US2 shift.

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