Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...434..262d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 1, p. 262-267
Astronomy and Astrophysics
Astrophysics
24
Differential Equations, Hydrodynamics, Magnetohydrodynamic Waves, Mass Ratios, Radiation Spectra, Shock Wave Attenuation, Two Dimensional Boundary Layer, Boundary Layers, Interstellar Matter, Morphology, Planetary Nebulae, Stability
Scientific paper
We investigate the radiative shock overstability for finite-sized objects. We follow the analysis of Chevalier & Imamura (1982), but we take into account the transverse flow of material out of the potshock region. The mass loss from the postshock region stabilizes the flow. As a rough estimate, the shock radiative instability takes place when the shock wave position with no radiative cooling (only mass loss present) is larger than the shock position with no mass loss (only radiative cooling present). For typical conditions of planetary nebulae we find that in order for the shock radiative overstability to occur, the nebular radius should be R approximately less than 1019 na-1 cm, where nalpha is the total number density of the interstellar medium (in units of cm-3. We give several examples of interacting planetary nebulae in light of this condition.
Dgani Ruth
Soker Noam
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