Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.atnf.csiro.au/research/masermeeting/web_papers/504_Jones.pdf Дата изменения: Mon Mar 26 22:06:42 2007 Дата индексирования: Sun Dec 23 09:44:50 2007 Кодировка: Поисковые слова: hst

The 3D Morphology of VY Canis Majoris: Kinematics, Polarimetry, and the Line-ofSight Distribution of the Ejecta

Terry Jay Jones, Roberta M. Humphreys, and L. Andrew Helton ­ University of Minnesota Changfeng Gui and Xiang Huang ­ University of Connectitcut

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Richards et al. 1998 (Merlin)
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SiO J = 1 ­ 0 Shinnaga et al. 2003

658nm HST image
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The Data Set
High resolution imaging with HST/WFPC2 in 2 epochs High resolution spectroscopy (Keck) Polarimetry with HST/ACS/HRC

Radial Velocities + Proper Motion = Total Motion Polarimetry = Independent Placement in 3D

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Proper motions of selected clumps, arcs and features in the reflection nebulosity surrounding VY CMa

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NW Arc 500yrs

S Knots 160yrs

SW Knots 250yrs

S Arc 480yrs

Arc 1 800yrs Arc 2 ­ 460yrs

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Total Intensity

Photometric Color Fractional Polarization

Note: Most features in the intensity map are also distinctive in the fractional polarization map = distinct features

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Fractional Polarization

NW Arc

S Arc

Arc 2

Arc 1

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Conclusions
· The arcs and knots appear to be separate geometric objects. · They do not display any clear association with a simple bipolar outflow geometry. · There is good agreement between the 3D geometry derived from two independent techniques. · Some sort of magnetic phenomena near the star?

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