Photoionization modeling of Magellanic Cloud planetary nebulae. I

Journal Article · Tue Jan 01 04:00:00 EST 1991 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/169607· OSTI ID:6002907

Dopita, M A; Meatheringham, S J ^[1]

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1. Mount Stromlo and Siding Spring Observatories, Canberra (Australia) NASA, Goddard Space Flight Center, Greenbelt, MD (USA)

The results of self-consistent photoionization modeling of 38 Magellanic Cloud PNe are presented and used to construct an H-R diagram for the central stars and to obtain both the nebular chemical abundances and the physical parameters of the nebulae. T(eff)s derived from nebular excitation analysis are in agreement with temperatures derived by the classical Zanstra method. There is a linear correlation between log T(eff) and the excitation class. The majority of the central stars in the sample with optically thick nebulae have masses between 0.55 and 0.7 solar mass and are observed during their hydrogen-burning excursion toward high temperatures. Optically thin objects are found scattered throughout the H-R diagram, but tend to have a somewhat smaller mean mass. Type I PN are found to have high core masses and to lie on the descending branch of the evolutionary tracks. The nebular mass of the optically thick objects is closely related to the nebular radius, and PN with nebular masses over one solar are observed. 62 refs.

• OSTI ID: 6002907
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 367; ISSN ASJOA; ISSN 0004-637X
• 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
CHEMICAL COMPOSITION
CORRELATIONS
DIAGRAMS
GALAXIES
HERTZSPRUNG-RUSSELL DIAGRAM
IONIZATION
MAGELLANIC CLOUDS
MASS
MATHEMATICAL MODELS
NEBULAE
OPACITY
OPTICAL PROPERTIES
PHOTOIONIZATION
PHYSICAL PROPERTIES
PLANETARY NEBULAE
STARS