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Modelling the Planetary Nebula

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Abstract

Deep narrow-band imaging and spectroscopy of the Planetary Nebula (PN)surrounding V4334 Sagittarii have been obtained since the onset of thethermal pulse in the star. Although of low surface brightness,narrow-band imaging suggests a ring structure maybepresent. Abundances, expansion rates and physical parameters for thenebula, derived from spectroscopy, show the plasma to be essentiallytypical of old evolved PN (within the errors of observation). The mostrecent data show little evidence of recombination indicating a verylow plasma electron density.Assuming no recombination has occurred, models of the PN spectrum wereconstructed using both simplistic ideas as well as sophisticatedphoto-ionisation codes. These show good agreement, and suggest that thepre-outburst UV radiation field would need to be powered by aprecursor with a surface temperature of T ⋆ > 105K. The luminosity ofthis star is less well constrained by the models, and cannot be usedsolely to accurately determine its distance. However, by excludingunrealistic models we expect 250 > L/Lodot > 1000 or so. When plotted ona HR diagram for evolved stars this shows good agreement with thatexpected for a pre-last thermal pulse object.

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Authors and Affiliations

  1. APS Division, Queen's University Belfast, Belfast, BT7 1NN, UK

    Don Pollacco

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  1. Don Pollacco
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Pollacco, D. Modelling the Planetary Nebula. Astrophysics and Space Science 279, 129–137 (2002). https://doi.org/10.1023/A:1014620711722

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  • DOI: https://doi.org/10.1023/A:1014620711722

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