ALMA data suggest the presence of spiral structure in the inner wind of CW Leonis

@article{Decin2015ALMADS,
  title={ALMA data suggest the presence of spiral structure in the inner wind of CW Leonis},
  author={Leen Decin and Anita M. S. Richards and David A. Neufeld and Wolfgang Steffen and Gary J. Melnick and Robin Lombaert},
  journal={Astronomy and Astrophysics},
  year={2015},
  volume={574},
  pages={26}
}
Context. Evolved low-mass stars lose a significant fraction of their mass through stellar winds. While the overall morphology of the stellar wind structure during the asymptotic giant branch (AGB) phase is thought to be roughly spherically symmetric, the morphology changes dramatically during the post-AGB and planetary nebula phase, during which bipolar and multi-polar structures are often observed. Aims. We aim to study the inner wind structure of the closest well-known AGB star CW Leo… 

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References

SHOWING 1-10 OF 70 REFERENCES

Surprising detection of an equatorial dust lane on the AGB star IRC+10216

Aims. Understanding the formation of planetary nebulae remains elusive because in the preceding asymptotic giant branch (AGB) phase these stars are heavily enshrouded in an optically thick dusty

The carbon star IRC+10216: linking the complex inner region with its spherical large‐scale structures

IRC+10216 is located at the tip of the asymptotic giant branch of the Hertzsprung-Russell diagram in a transition phase toward the post-asymptotic giant branch stage. Its study contributes to our

PROBING SUBSTELLAR COMPANIONS OF ASYMPTOTIC GIANT BRANCH STARS THROUGH SPIRALS AND ARCS

Recent observations of strikingly well-defined spirals in the circumstellar envelopes of asymptotic giant branch (AGB) stars point to the existence of binary companions in these objects. In the case

Modeling the physical and excitation conditions of the molecular envelope of NGC 7027

Context. The link between the shaping of bipolar planetary nebulae and the mass ejection activity of their central stars is still poorly understood. Appropriately characterizing the evolution of

Winds of M-type AGB stars driven by micron-sized grains

Context. In view of the recent problem regarding the dynamical modelling of winds of M-type AGB stars (insufficient radiation pressure on silicate grains), some of the basic assumptions of these

Unexpectedly large mass loss during the thermal pulse cycle of the red giant star R Sculptoris

It is concluded that R Sculptoris is a binary system that underwent a thermal pulse about 1,800 years ago, lasting approximately 200  years, and about three times more mass was returned to the interstellar medium during and immediately after the pulse than previously thought.

Three-dimensional simulations of the atmosphere of an AGB star

Context. Winds of asymptotic giant branch stars are assumed to be driven by radiation pressure on dust. Previously, this process has been modeled with detailed time-dependent simulations of

Bipolar Pre-Planetary Nebulae: Hydrodynamics of Dusty Winds in Binary Systems. II. Morphology of the Circumstellar Envelopes

We have constructed three-dimensional smoothed particle hydrodynamics models to examine the influence of a detached binary companion on the dusty winds from red giants and asymptotic giant branch

Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: derivation of mass-loss rate formulae

Context. The evolution of intermediate and low-mass stars on the asymptotic giant branch is dominated by their strong dust-driven winds. More massive stars evolve into red supergiants with a similar

The birth of a planetary nebula around the carbon star IRC+10216

Our current understanding of the evolution of solar-type stars suggests that after a period as a red giant star, during which mass loss occurs continuously in the form of a stellar wind, a period of
...