2001MNRAS.328.1081S -
Mon. Not. R. Astron. Soc., 328, 1081-1084 (2001/December-3)
Backflow in post-asymptotic giant branch stars.
SOKER N.
Abstract (from CDS):
We derive the conditions for a backflow toward the central star(s) of circumstellar material to occur during the post-asymptotic giant branch (post-AGB) phase. The backflowing material may be accreted by the post-AGB star and/or its companion, if such exists. Such a backflow may play a significant role in shaping the descendant planetary nebula, by, among other things, slowing down the post-AGB evolution, and by forming an accretion disc which may blow two jets. We consider three forces acting on a slowly moving mass element: the gravity of the central system, radiation pressure, and fast wind ram pressure. We find that for a significant backflow to occur, a slow dense flow should exist, such that the relation between the total mass in the slow flow, Mi, and the solid angle it covers Ω, is given by (M_i/β)\gtrsim 0.1 M_☉, where {formmu2} β ≡ Ω/4π. The requirement for both a high mass-loss rate per unit solid angle and a very slow wind, such that it can be decelerated and flow back, probably requires close binary interaction, hence this process is rare.
Abstract Copyright:
The Royal Astronomical Society
Journal keyword(s):
stars: AGB and post-AGB - circumstellar matter - stars: mass-loss - planetary nebulae: general
Simbad objects:
3
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