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

TL;DR

This study reveals an unexpected equatorial dust lane on the AGB star IRC+10216 through scattered light imaging, challenging previous assumptions and suggesting new models for circumstellar dust structures.

Contribution

It introduces the first detection of an equatorial dust lane on an AGB star and compares two models explaining this feature, advancing understanding of stellar envelope morphology.

Findings

Detection of a narrow equatorial dust lane in IRC+10216

Both density enhancement and dust ring models can explain the observed structure

The dark lane is caused by dense dust, not bipolar outflow

Abstract

Understanding the formation of planetary nebulae remains elusive because in the preceding asymtotic giant branch (AGB) phase these stars are heavily enshrouded in an optically thick dusty envelope. To further understand the morphology of the circumstellar environments of AGB stars we observe the closest carbon-rich AGB star IRC+10216 in scattered light. When imaged in scattered light at optical wavelengths, IRC+10216 surprisingly shows a narrow equatorial density enhancement, in contrast to the large-scale spherical rings that have been imaged much further out. We use radiative transfer models to interpret this structure in terms of two models: firstly, an equatorial density enhancement, commonly observed in the more evolved post-AGB stars, and secondly, in terms of a dust rings model, where a local enhancement of mass-loss creates a spiral ring as the star rotates. We conclude that both models can be used to reproduce the dark lane in the scattered light images, which is caused by an equatorially density enhancement formed by dense dust rather than a bipolar outflow as previously thought. We are unable to place constraints on the formation of the equatorial density enhancement by a binary system.