Influence of stellar evolution on the evolution of planetary nebulae. I - Numerical method and hydrodynamical structures. II - Confrontation of models with observations

Details Influence of stellar evolution on the evolution of planetary nebulae. I - Numerical method and hydrodynamical structures. II - Confrontation of models with observations Influence of stellar evolution on the evolution of planetary nebulae. I - Numerical method and hydrodynamical structures. II - Confrontation of models with observations

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...174..211s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 174, no. 1-2, March 1987, p. 211-231.

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Hydrodynamic Equations, Planetary Nebulae, Stellar Evolution, Stellar Winds, Computational Fluid Dynamics, Gas Ionization, Helium, Hydrogen, Mathematical Models, Stellar Mass Accretion

Scientific paper

The evolution of planetary nebulae (PN) is studied in terms of the time dependent equations of gas flow, ionization, and energy balance. The three-wind and two-wind models which illustrate the evolution of PN are described. It is observed that the stellar time scales control the evolution of PN up to the central star's temperature maximum, and then the nebular parameters govern evolution. It is determined that the two-wind models have accretion-model properties; however, their expansion velocities and their initial nebular masses are smaller than in three-wind models. The models are compared with observational data on expansion velocities, He II/H-beta line ratios, Zanstra temperatures, and electron densities. It is noted that the evolution of PN is best represented by a model in which the central star evolves along a Schoenberner postasymptotic-giant-branch track in the mass range 0.6-0.64 solar mass; the nebula is formed in an initial expansion of 0.1 solar mass; and a progenitor star with a strong wind with a mass-loss rate of (3-30) x 10 to the -6th solar mass/yr.

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