Physics
Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8304k&link_type=abstract
HST Proposal ID #8304
Physics
Hst Proposal Id #8304 Hot Stars
Scientific paper
Stellar winds from central stars of planetary nebulae {CSPN} are responsible for driving the dynamical expansion as well as shaping the morphology of planetary nebulae {PN}. The stellar winds also remove material from the thin hydrogen atmosphere of the central star, determining whether a PN will stay hydrogen burning throughout its lifetime or will go through an episode of thermal pulse and revert back to the asymptotic giant branch. Wind signatures have been seen in the IUE spectra of a number of evolved PN with high temperature central stars but very little is known about the properties of the stellar winds in young PN when the nebular morphology is being shaped. We request HST time to carry out sensitive UV spectroscopic observations of a number of CSPN. With good S/N spectra, we will be able to fit the line profiles of resonance lines to deduce the mass loss rates and terminal velocities of the stellar winds. We propose to observe 4 young PN selected for their small angular sizes, low temperature sta rs, and high nebular densities. We have chosen a mixture of carbon-rich and oxygen-rich nebulae to see if the wind properties are dependent on atmospheric chemistry. In addition, by fitting the line profiles of some of the atmospheric lines, we can derive the surface gravity and therefore obtain a better determination of the mass and luminosities of the central stars.
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