Photoionization modelling of metal-enriched nova shells

Details Photoionization modelling of metal-enriched nova shells Photoionization modelling of metal-enriched nova shells

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.248..217s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 248, Jan. 15, 1991, p. 217-228.

Astronomy and Astrophysics

Astronomy

4

Astronomical Models, Metallicity, Novae, Photoionization, Stellar Envelopes, Abundance, Ionized Gases, Stellar Evolution, Stellar Temperature

Scientific paper

A photoionization model has been developed to investigate the physical conditions in old nova shells with large metal abundances. Atomic rates at low temperatures are included in the model so that the evolution of shells can be traced from their hot, early stages to their later cool phases. X-ray processes are also included. A situation in which a region of lowest temperature but highest ionization can exist at the inner edge of a nebula is demonstrated. A nonuniform density distribution is compared with a uniform density and the observational consequences discussed. The shell of the old nova, CP Pup, is analyzed in detail and its evolution during its constant-luminosity phase traced. The CNO abundances, nitrogen in particular, must be enhanced with respect to solar values to explain the observations. The strongest emission from the shell during most of its constant-luminosity phase was from N III 57 microns and was also responsible for most of the cooling in the gas. Conflicting reports on the distance to nova CP Pup are examined, from which a distance of 800 pc is determined.

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