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How Planetary Nebulae Shells Interact with their Local Environement

Published online by Cambridge University Press:  15 December 2006

Eva Villaver ,
Arturo Manchado ,
Guillermo García-Segura  and
Letizia Stanghellini
Eva Villaver
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA; Affiliated to the Hubble Space Telescope Department of ESA
Arturo Manchado
Affiliation:
Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna, E-38200 Tenerife, Spain; Affiliated to CSIC
Guillermo García-Segura
Affiliation:
Instituto de Astronomía-UNAM, Apartado postal 877, Ensenada, 22800 Baja California, México
Letizia Stanghellini
Affiliation:
National Optical Astronomy Observatory, 950 N Cherry Avenue, Tucson AZ 85719, USA
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Abstract

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Planetary Nebula (PN) shells and AGB circumstellar envelopes evolve under a wide range of external conditions, from the high ISM densities found in the Galactic plane, to the rarefied and hot intracluster medium where the systemic velocity of the star can be as high as 2000 km $s^{-1}$. We explore the effects that the external pressure and/or stellar systemic velocity have on the observable properties of PNe. We investigate how the mass and size of the PN halos are reduced when the star is moving with respect to the external medium. We have studied as well how the mass of the circumstellar envelope is fed by ISM material when high ISM densities characteristic of the Galactic plane are considered. By studying the evolution of PNe in the intracluster medium in Virgo, we infer shorter PN lifetimes than what is usually adopted. This has important implications, since the assumed PN lifetime strongly affects the fraction of intracluster light derived from PN studies.

Keywords

hydrodynamicsstars: AGB and post-AGBplanetary nebulae: generalintergalactic medium
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 333 - 336
Copyright
© 2006 International Astronomical Union