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The Ionization of Novae Ejecta

Published online by Cambridge University Press:  12 April 2016

R.E. Williams
R.E. Williams*
Affiliation:
Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, CHILE

Abstract

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Novae ejecta pass through four distinct phases of evolution of the emission-line spectrum, caused by different ionization characteristics of the shell. These include a neutral (I), an auroral (II), a coronal (III), and a nebular (IV) phase. Photoionization from the contracting photosphere of the hot white dwarf is the source of the ionization, including the highly ionized coronal phase. Changing emission line ratios in certain novae that develop dust are caused by condensation of grains from the gas, and can be used to determine the composition of the dust. In V1370 Aql, substantial silicate grain formation appears to have taken place, probably within the ionized gas.

Type
2. Models of Observations
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 215 - 227
Copyright
Copyright © Springer-Verlag 1990

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