Molecular Photodissociation in the Neutral Envelopesof Planetary Nebulae

Details Molecular Photodissociation in the Neutral Envelopesof Planetary Nebulae Molecular Photodissociation in the Neutral Envelopesof Planetary Nebulae

1994-11-22

arxiv.org/abs/astro-ph/9411094v1

Astronomy and Astrophysics

Astrophysics

36 pages, postscript file includes 8 figures, accepted for publication in MNRAS, file also available as ftp://pandora.phys.u

Scientific paper

The dissociation and subsequent ionisation of molecular material in a detached, spherically symmetric stellar wind is modelled as a star evolves from the post-asymptotic giant branch phase to a planetary nebula (i.e. from a stellar effective temperature of Teff=6000K to Teff=33000K). The model is compared to the observed mass and distribution of ionised and atomic hydrogen in the planetary nebula IC418. It is found that the mass of circumnebular atomic hydrogen observed in IC418 can easily be produced by the dissociation of originally molecular material by the ultraviolet radiation of the central star. However, the observed spatial distribution of the gas is not accurately recreated by the current model.

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