Extinction, ejecta masses, and radial velocities of novae

Details Extinction, ejecta masses, and radial velocities of novae Extinction, ejecta masses, and radial velocities of novae

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426..279w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 1, p. 279-287

Astronomy and Astrophysics

Astrophysics

40

Ejecta, Emission Spectra, Interstellar Extinction, Line Spectra, Novae, Oxygen, Radial Velocity, Stellar Envelopes, White Dwarf Stars, Charge Coupled Devices, Cosmic Dust, Interstellar Gas, Ion Recombination, Optical Thickness

Scientific paper

Interstellar reddening is determined for a number of recent novae based upon emission-line ratios which are generally observable using CCDs. Large values of extinction are found for most systems, possibly indicative of an intrinsic component of reddening in postoutburst novae. The unusual characteristics of the (O I) lines in novae, which are strong and optically thick, require a large population of very dense globules which are the likely sites of dust formation. These pyroclasts must be ejected from the white dwarf. The total mass of the neutral gas in the globules in some of the objects is substantially larger than the masses normally derived for the ionized ejecta of novae. The distribution of radial velocities of Galactic novae in the Tololo sample, although uncertain, shows an asymmetry in having predominantly negative values. Either high internal absorption in the expanding ejecta skews the emission lines to bluer wavelengths, or most of the novae are moving out from the center of the Galaxy.

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