The evolutionary sequence of planetary nebulae

Journal Article · Sun Jul 01 04:00:00 EDT 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/168900· OSTI ID:6577953

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)

A first-order solution to the problem of nebular evolution is presented and used to construct photoionization models with the correct ionized gas geometry with respect to the central star. The models are used to investigate the evolution of the central star in terms of a transformed H-R diagram in which H-beta luminosity replaces stellar luminosity and the nebular excitation class takes the place of stellar effective temperature. It is shown that the optically thick PN in the Magellanic Clouds behave as ram-pressure confined H II regions trapped between the shocked remnants of AGB wind and the high-velocity stellar wind of the PN nuclei. 72 refs.

• OSTI ID: 6577953
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 357; 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
BALMER LINES
DIAGRAMS
FLUIDS
GALAXIES
GASES
HERTZSPRUNG-RUSSELL DIAGRAM
IONIZED GASES
MAGELLANIC CLOUDS
MATHEMATICAL MODELS
NEBULAE
PLANETARY NEBULAE
RADIATION PRESSURE
STAR EVOLUTION
STAR MODELS
STELLAR ACTIVITY
STELLAR WINDS