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Polarized Line Profiles in Planetary Nebulae

Published online by Cambridge University Press:  07 August 2017

J.R. Walsh  and
R.E.S. Clegg
J.R. Walsh
Affiliation:
1Space Telescope Coordinating Facility, ESO, Karl-Schwarzchild-Strasse 2 D-8046, Garching bei München, Germany
R.E.S. Clegg
Affiliation:
2Royal Greenwich Observatory, Madingley Road, Cambridge, CB3 0HZ, United Kingdom

Extract

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There is much direct and indirect evidence for the presence of dust in Planetary Nebulae (PN): variations in extinction across the face of the nebulae; IR emission with strong 25 and 60μm fluxes; broad near-IR emission lines of Silicate, SiC and PAH grains; optically thick lines, such as [C IV]1550Å, have lower strength on account of the increased path length due to dust scattering; a centro-symmetric pattern of polarization vectors in a few PN (Leroy et al., A&A, 160, 171, 1986). An observational programme has begun to study the polarization profiles of bright emission lines in PN arising from dust scattering within the nebulae. The first results are discussed.

Type
III. Highlights on the Nebulae
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 231
Copyright
Copyright © Kluwer 1993