Volume 584, December 2015
|Number of page(s)||5|
|Published online||02 December 2015|
1 ITAP, Universität zu Kiel, Leibnizstr. 15, 24118 Kiel, Germany
2 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany
3 European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago, Chile
4 Astronomy and Astrophysics Research Group, Dep. of Physics and Astrophysics, V.U. Brussel, Pleinlaan 2, 1050 Brussels, Belgium
5 Sobolev Astronomical Institute, St. Petersburg University, Universitetskii prosp., 28, St. Petersburg 198504, Russia
Received: 15 October 2015
Accepted: 9 November 2015
Massive stars live short lives, losing large amounts of mass through their stellar wind. Their mass is a key factor determining how and when they explode as supernovae, enriching the interstellar medium with heavy elements and dust. During the red supergiant phase, mass-loss rates increase prodigiously, but the driving mechanism has proven elusive. Here we present high-contrast optical polarimetric-imaging observations of the extreme red supergiant VY Canis Majoris and its clumpy, dusty, mass-loss envelope, using the new extreme-adaptive-optics instrument SPHERE at the VLT. These observations allow us to make the first direct and unambiguous detection of submicron dust grains in the ejecta; we derive an average grain radius ~0.5 μm, 50 times larger than in the diffuse ISM, large enough to receive significant radiation pressure by photon scattering. We find evidence for varying grain sizes throughout the ejecta, highlighting the dynamical nature of the envelope. Grains with 0.5 μm sizes are likely to reach a safe distance from the eventual explosion of VY Canis Majoris; hence it may inject upwards of 10-2 M⊙ of dust into the ISM.
Key words: stars: winds, outflows / supergiants / circumstellar matter / stars: individual: VY Canis Majoris / stars: mass-loss / polarization
Based on observations made with European Southern Observatory (ESO) telescopes at the La Silla Paranal Observatory under program 60.A-9368(A).
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2015
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