Physics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6761t&link_type=abstract
HST Proposal ID #6761
Physics
Hst Proposal Id #6761 Interstellar Medium
Scientific paper
While evolved planetary nebulae {PNe} have been well studied, the transition from the AGB to the PN phase of evolution is still poorly understood. In particular, the characteristics of the mass loss occurring during this transition period are not well known. We propose to probe this phase of evolution by obtaining Planetary Camera images of three bipolar proto- planetary nebulae {PPNe}. Shock emission dominates the optical line spectra of the lobes of these objects and shocks probably play a significant role in their dynamic evolution. This shock emission is an excellent tracer of the ongoing mass outflow in these objects and affords a powerful probe into the geometry of the mass loss between the AGB and PN phases of evolution. Is the shock emission the result of a uniform flow impacting over the entire face of the nebula or is this emission formed in fast moving bullets of material? One model for the mass loss during this phase of evolution suggests that this outflow might be collimated. Do we see evidence for a collimated outflow in these objects? We will address these questions by obtaining narrow-band images of three PPNe through filters centered on emission lines known to be produced via shock heating. These PPNe are too small to be resolved in detail from the ground, but can be resolved using the high spatial resolution capabilities of HST.
No associations
LandOfFree
The Origin of Shock Emission in Proto- Planetary Nebulae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Origin of Shock Emission in Proto- Planetary Nebulae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Origin of Shock Emission in Proto- Planetary Nebulae will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1118379