Asymmetry and inhomogeneity in proto- and young planetary nebulae

@article{Soker2000AsymmetryAI,
  title={Asymmetry and inhomogeneity in proto- and young planetary nebulae},
  author={Noam Soker},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2000},
  volume={318},
  pages={1017-1022}
}
  • N. Soker
  • Published 1 December 1999
  • Physics
  • Monthly Notices of the Royal Astronomical Society
I study some effects of aspherical mass loss during the last stages of the asymptotic giant branch (AGB) on the appearance of proto-planetary nebulae (proto-PNs) and young PNs. The aspherical mass loss can be small-scale inhomogeneities, and/or axially symmetric mass-loss geometry. I first examine the role of the dust opacity in the optical band on the appearance of proto-PNs. I conclude that large optical depths will be found in proto-PNs that are post-AGB stars having high equatorial mass… Expand
Axisymmetry in protoplanetary nebulae - II. A near-infrared imaging polarimetric survey
In an imaging polarimetry survey of candidate post-AGB stars, scattering envelopes are detected around 20 objects. These envelopes represent the final mass-loss phases at the end of the AGB. In allExpand
The Very Slow Wind from the Pulsating Semiregular Red Giant, L2 Puppis
We have obtained 1 1.7 and 17.9 micron images at the Keck I telescope of the circumstellar dust emission from L(sub 2) Pup, which is one of the nearest ( D = 61 pc) mass-losing, pulsating red giantsExpand
Proto-Planetary Nebulae as Explosions: Bullets versus Jets and Nebular Shaping
Many proto-planetary nebulae (PPNs) appear as narrow collimated structures sometimes showing multiple, roughly aligned lobes. In addition, many PPN flows have been shown to have short accelerationExpand
Backflow in post‐asymptotic giant branch stars
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 beExpand
A model for the strings of $\mathsf{\eta}$ Carinae
We propose a model based on ionization shadows to explain the formation of the long and narrow strings of Eta Carinae. Five strings are known, all located along the symmetry axis outside theExpand

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