Statistics – Computation
Scientific paper
May 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...340..927s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 340, May 15, 1989, p. 927-931.
Statistics
Computation
16
Binary Stars, Hydrodynamics, Planetary Nebulae, Computational Astrophysics, Stellar Evolution, Stellar Mass Ejection, Stellar Winds
Scientific paper
It is suggested that the shape of a young asymmetrical planetary nebulae may be influenced by a close binary-star located at its center. This binary is a relic of the common envelope phase, presumably through which the asymmetrical planetary nebula evolved. It is assumed that, for a short period of time, shortly after the cessation of the slow wind and long before the fast wind becomes effective, the binary ejects a small amount of mass, mainly in the equatorial plane. By using two-dimensional hydrodynamics it is found that, at late times, the high-density region has a 'horsehoe' shape, as viewed in the symmetry plane. There is an instability in the maximum density region, which shows up as a high-density knot. The exact scale of the knot is determined by the numerics. The applications of the results to observations are discussed.
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