Ionization structure of planetary nebulae. Part 4: NGC 7662

Technical Report · Tue Jan 01 04:00:00 EST 1985

OSTI ID:6077517

Barker, T

Spectrophotometric observations of emission-line intensities over the spectral range 1400 to 7200 A were made in five positions in the planetary nebula NGC 7662. Standard equations used to correct for the existence of elements in other than the optically observable ionization stages show a consistent and approximate agreement with abundances calculated using ultraviolet lines. The abundances of C and N indicate that some mixing of CNO-processed material into the nebular shell may have occurred in NGC 7662; the low He abundance, however, indicates that little or no He enrichment occurred. The Ar, Ne, and O and S abundances appear to be low. It is suggested that the progenitor to NGC 7662 may have formed out of somewhat metal-poor material.

• Research Organization: California Univ., San Diego, La Jolla (USA)
• OSTI ID: 6077517
• Report Number(s): N-85-35844; NASA-CR-176151
• Country of Publication: United States
• Language: English

Related Subjects

640107* -- Astrophysics & Cosmology-- Planetary Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ARGON
CARBON
ELEMENTS
EMISSION SPECTRA
FLUIDS
GASES
HELIUM
IONIZATION
NEBULAE
NEON
NITROGEN
NONMETALS
PLANETARY EVOLUTION
PLANETARY NEBULAE
RARE GASES
SOLAR SYSTEM EVOLUTION
SPECTRA
ULTRAVIOLET SPECTRA