Backflow in Post-Asymptotic Giant Branch Stars

Details Backflow in Post-Asymptotic Giant Branch Stars Backflow in Post-Asymptotic Giant Branch Stars

2001-03-07

arxiv.org/abs/astro-ph/0103105v1

Mon.Not.Roy.Astron.Soc. 328 (2001) 1081

Astronomy and Astrophysics

Astrophysics

Submitted to MNRAS

Scientific paper

10.1046/j.1365-8711.2001.04975.x

We derive the conditions for a backflow toward the central star(s) of circumstellar material to occur during the post-asymptotic giant branch (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 disk 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 exsist, such that the relation between the total mass in the slow flow, M, and the solid angle it covers, Omega, is given by (4*pi*M/Omega)>0.1Mo. The requirement for both 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.

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