Origin of the coronal line emission from novae

Details Origin of the coronal line emission from novae Origin of the coronal line emission from novae

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...225..950s&link_type=abstract

Astrophysical Journal, Part 1, vol. 225, Nov. 1, 1978, p. 950-953.

Other

12

Emission Spectra, Line Spectra, Novae, Stellar Coronas, Ejecta, Gas Ionization, H Alpha Line, Photoionization, Shock Waves

Scientific paper

It is proposed that the coronal line emission from V1500 Cyg and other fast novae originates in gas shocked to about 10 to the 6th power K as a result of supersonic random motions within the principal ejecta. This model simultaneously explains the similar widths of the coronal and nebular lines, the temperature and luminosity of the coronal line region, the gradual decrease in ionization, the variability of the coronal line profiles, and the progressive sharpening of velocity structure in the nebular line profiles. The ejecta are characterized by approximately 10 to the 3rd power clouds with a relative velocity dispersion of about 10 to the 2.2 power km/s, compared with an expansion velocity about 10 to the 3.2 power km/s. Alternative models for the coronal lines involving photoionization or interaction of the principal shell with circumstellar gas or with a fast wind from the central object are considered and rejected.

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