Backflow in post-asymptotic giant branch stars |
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Authors: | Noam Soker |
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Institution: | Department of Physics, University of Haifa, Oranim, Tivon 36006, Israel |
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Abstract: | 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, M i , and the solid angle it covers Ω, is given by , where . 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. |
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Keywords: | stars: AGB and post-AGB circumstellar matter stars: mass-loss planetary nebulae: general |
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