Dynamical evolution of planetary nebulae. I - Formation of shells in an accelerating wind in protoplanetary nebulae

Details Dynamical evolution of planetary nebulae. I - Formation of shells in an accelerating wind in protoplanetary nebulae Dynamical evolution of planetary nebulae. I - Formation of shells in an accelerating wind in protoplanetary nebulae

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.242..505k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 242, Feb. 1, 1990, p. 505-511. Research supported by SE

Statistics

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54

Computational Astrophysics, Planetary Nebulae, Stellar Envelopes, Stellar Evolution, Stellar Winds, Abundance, Astronomical Models, Helium, Protoplanets, Taylor Instability

Scientific paper

Evolutionary calculations of central stars of planetary nebulae show a time-dependent increase in surface temperature. The high-speed winds, which these stars emit, expand into a previously ejected 'superwind' and are most likely driven by radiation pressure. Hence a model explaining the dynamical evolution of the surrounding planetary nebulae must take into account that the wind speed increases and the mass-loss rate decreases with time. It is shown that at an early stage a shell will form and that the flow changes from momentum to energy driven, once the wind speed is in excess of 150 km/s. Radii and velocities of these shells are generally lower in an accelerating wind model than in the simple multiple-winds model. Another important difference is the occurrence of Rayleigh-Taylor instabilities in the shell when the flow is energy driven.

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