On the dynamical evolution of planetary nebulae

Details On the dynamical evolution of planetary nebulae On the dynamical evolution of planetary nebulae

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...248..590m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 248, no. 2, Aug. 1991, p. 590-598.

Physics

76

Asymptotic Giant Branch Stars, Hydrodynamic Equations, Planetary Nebulae, Stellar Evolution, Stellar Winds, Boundary Conditions, Stellar Mass Ejection, Stellar Physics

Scientific paper

Hydrodynamical calculations on the evolution of planetary nebulae over a time span of 25,000 yr are presented. The nebulae are treated as spherically symmetric gaseous shells, expanding in the gravitation and radiation field of an evolving star with 0.6 solar mass. For the origin of the nebulae, the possibility of a superwind with a mass loss rate of 0.0001 solar mass/yr for a time interval of 1000 yr is taken into consideration. The pressure exerted upon the inner rim of the nebular material varies significantly during the course of the central star's evolution, leading to concomitant variations of the shell thickness. The present nebular models yield relative shell thicknesses between 0.2 and 0.5, in good agreement with observations. The full hydrodynamic calculations presented do not support the often used concept of 'thin' nebular shells.

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