Origin of the coronal line emission from novae

Journal Article · Wed Nov 01 04:00:00 EST 1978 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/156561· OSTI ID:6467970

Shields, G A; Ferland, G J

We propose that the coronal line emission from V1500 Cyg and other fast novae originates in gas shocked to approx.10/sup 6/ 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 approx.10/sup 3/ clouds with a relative velocity dispersion approx.10/sup 2.2/ km s/sup -1/, compared with an expansion velocity approx.10/sup 3.2/ km s/sup -1/.We consider and reject 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.

• Research Organization: McDonald Observatory and Department of Astronomy, University of Texas at Austin
• OSTI ID: 6467970
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 225:3; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
LINE WIDTHS
MATHEMATICAL MODELS
NOVAE
PLASMA
SHOCK WAVES
SPECTRA
STAR MODELS
STARS
STELLAR ATMOSPHERES
TURBULENCE
VARIABLE STARS