Hot Gas and Thermal Conduction in Planetary Nebulae

Details Hot Gas and Thermal Conduction in Planetary Nebulae Hot Gas and Thermal Conduction in Planetary Nebulae

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006cxo..prop.2110g&link_type=abstract

Chandra Proposal ID #08200733

Physics

Chandra Proposal Id #08200733

Scientific paper

Planetary nebulae (PNe) consist of the material ejected by stars with masses less than 8-10 Msun near the end of their evolution. Shock-heated gas fills the central cavity of PNe and should be detectable in X-rays. The few existing detections of diffuse X-ray emission from PNe appear to suggest that the X-ray luminosity and plasma temperature decrease as a PN evolves. We have used FUSE detections of nebular OVI emission or absorption to identify 3x10E5 K gas from the interface between a hot PN interior and its nebular shell to identify PNe most likely to possess X-ray-emitting gas. We request Chandra observations of two such PNe. These PNe have intermediate ages and can be used to study the role of thermal conduction in PNe as well as better establish how the hot gas evolves with time.

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