The interpretation of internal motions in planetary nebulae

Details The interpretation of internal motions in planetary nebulae The interpretation of internal motions in planetary nebulae

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...136..181s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 136, no. 2, July 1984, p. 181-192. Research supported by the Consiglio Naziona

Astronomy and Astrophysics

Astrophysics

52

Planetary Nebulae, Stellar Evolution, Stellar Motions, Astronomical Models, Asymptotic Giant Branch Stars, Gas Dynamics, Gas Ionization, Stellar Luminosity, Stellar Mass Ejection

Scientific paper

The observational data on the expansion velocity in planetary nebulae are discussed. The velocities are proportional to the nebular radius Rn up to about 0.15 pc and decrease slowly for larger radii. Two models are proposed to interpret the observational trend: (1) the planetary nabula is the region of interaction of a fast wind emitted by the nucleus with a slow wind emitted by the progenitor, accelerated by the transfer of momentum from the radiation field to the nebular material; (2) the planetary nebula is a Stromgren sphere evolving in an expanding nebula which results from a sudden ejection by an AGB star. Only model (2) agrees satisfactorily with all the observational data. The masses of the nebulae are in the range 0.1 to 0.5 solar mass and their initial velocities range from zero up to 30-70 km/s; the mass of the central star is close to 0.60 solar mass; the mass loss rate from the progenitor is of the order of 10 to the -6th solar mass/yr and the wind velocities are 5 to 10 km/s.

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