The 3D Morphology of the Extreme Red Supergiant VY CMa

Details The 3D Morphology of the Extreme Red Supergiant VY CMa The 3D Morphology of the Extreme Red Supergiant VY CMa

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004hst..prop10262h&link_type=abstract

HST Proposal ID #10262

Physics

Hst Proposal Id #10262 Cool Stars

Scientific paper

The extreme RSG and powerful OH/IR source VY CMa is surrounded by an asymmetric reflection nebula dominated by a prominent nebulous arc, bright filamentary arcs, and several clumps of dusty knots that are evidence for multiple and asymmetric mass loss events. Our groundbased velocities show that these structures are kinematically distinct from the gneral flow of the diffuse gas and may be directional. We have speculated that these arcs and knots may be caused by localized activity on the star involving convection and possibly magnetic fields analogous to lower mass stars. If correct this would have important implications for the causes of high mass loss events in evolved massive stars. Fortunately, VY CMa provides us with an opportunity to learn more about its possible mass loss mechanisms and history from the morphology of its ejecta. We propose to use polarimetry and second epoch images combined with our radial velocities to map the morphology of the nebula and the discrete structures embedded in it.

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