Hydrodynamical models of aspherical planetary nebulae

Details Hydrodynamical models of aspherical planetary nebulae Hydrodynamical models of aspherical planetary nebulae

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..718m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 718-732. Research supported by NWO.

Astronomy and Astrophysics

Astrophysics

74

Asphericity, Astronomical Models, Hydrodynamic Equations, Interstellar Matter, Planetary Nebulae, Stellar Mass, Stellar Winds, Asymptotic Giant Branch Stars, Boundary Conditions, Computerized Simulation, Density Distribution, Morphology, Stellar Evolution

Scientific paper

The emergence of these nebulae is accomplished with the 'Roe-solver' characteristic-based modeling technique extended by Eulderink (1990). The technique treats the Riemann problem with a numerical approximation that linearizes the problem. The correct velocity is thereby found if the initial discontinuity is a pure contact discontinuity or a pure shock. The aspherical planetary nebulae can be modeled in terms of aspherical bubbles by utilizing a density contrast in the remnants of the AGB wind. The analytical results of Icke (1988) are generally confirmed including the division of the shocks into spherical and 'protruding' parts. A cusp is described that forms the transition between these two parts and relates to a high degree of collimation in the high-density flow. A wide range of morphologies can be formed in the nebulae if it is assumed that intermediate-mass stars lose mass in two successive hydrodynamical stages.

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