Ionization and temperature structure in nova shells

Details Ionization and temperature structure in nova shells Ionization and temperature structure in nova shells

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...238..283b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 238, no. 1-2, Nov. 1990, p. 283-295.

Astronomy and Astrophysics

Astrophysics

5

Astronomical Models, Chemical Reactions, Ionization, Novae, Reaction Kinetics, Stellar Evolution, Temperature Distribution, Carbon, Cosmic Dust, Emission Spectra, Helium, Hydrogen, Iron, Line Spectra, Magnesium, Nitrogen, Oxygen, Silicon, Sodium, Sulfur

Scientific paper

The time-dependent ionization structure of an expanding nova shell is determined by solving the corresponding rate equations for the elements H, He, C, N, O, Na, Fe, Si, Mg, S simultaneously with the energy balance equation for calculating the temperature in the gas. This paper considers photoionization as heating and gas expansion, collisionally excited forbidden line emission from CI, OI, OII, NII, SiII, SII, recombination and free-free radiation of hydrogen as cooling mechanisms. The calculation is restricted to the transient phase where a zone of ionized hydrogen in the inner part of the shell coexists with a zone of neutral hydrogen ahead of it. Two models are calculated: one for a typical nondust-forming nova and one for a nova with copious dust formation. The results show that, for the dust forming case, the temperature in the neutral region rapidly drops below 1000 K and, thus, conditions for molecule and dust formation are favorable.

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