Radio Photosphere and Mass-Loss Envelope of VY CMa

Abstract

We have used the VLA to detect emission from the supergiant VY CMa at radio wavelengths and have constructed 3000-4500 K isothermal outer atmospheres constrained by the data. These models produce a radio photosphere at 1.5-2 R_ast. An extrapolation of the model can account for the observed total mass-loss rate of the star. We also present mid-infrared imaging of the supergiant that suggests warm dust is extended in the same direction as the near-infrared reflection nebula around VY CMa. The origin of the asymmetries in the outflow remains an unsolved problem.

arXiv commentAccepted for publication in June 10, 2005, ApJ. 20 pages, 5 figures

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• ALMA sub-mm maser and dust distribution of VY Canis Majoris
• The molecular envelope around the red supergiant VY CMa
• On massive dust clumps in the envelope of the red supergiant VY Canis Majoris
• Simultaneous VLBA polarimetric observations of the v=$\{$1,2$\}$ J=1-0 and v=1, J=2-1 SiO maser emission toward VY CMa II: component-level polarization analysis
• 658 GHz Vibrationally-Excited Water Masers with the Submillimeter Array