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2007MNRAS.382.1233W - Mon. Not. R. Astron. Soc., 382, 1233-1245 (2007/December-2)
The interaction of planetary nebulae and their asymptotic giant branch progenitors with the interstellar medium.
WAREING C.J., ZIJLSTRA A.A. and O'BRIEN T.J.
Abstract (from CDS):
We find that ISM interaction strongly affects outer PN structures, with the dominant shaping occurring during the AGB phase. The simulations predict four stages of PN-ISM interaction whereby (i) the PN is initially unaffected, (ii) then limb-brightened in the direction of motion, (iii) then distorted with the star moving away from the geometric centre, and (iv) finally so distorted that the object is no longer recognizable as a PN and may not be classed as such. Parsec-size shells around PNe are predicted to be common. The structure and brightness of ancient PNe are largely determined by the ISM interaction, caused by rebrightening during the second stage; this effect may address the current discrepancies in Galactic PN abundance. The majority of PNe will have tail structures. Evidence for strong interaction is found for all known PNe in globular clusters.
Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS
Journal keyword(s): hydrodynamics - stars: AGB and post-AGB - stars: mass-loss - planetary nebulae: general - ISM: structure
Simbad objects: 32
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