Central Stars of Planetary Nebulae: a Test of the Radiatively Driven Wind Theory: CYCLE4 Medium

Details Central Stars of Planetary Nebulae: a Test of the Radiatively Driven Wind Theory: CYCLE4 Medium Central Stars of Planetary Nebulae: a Test of the Radiatively Driven Wind Theory: CYCLE4 Medium

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5339m&link_type=abstract

HST Proposal ID #5339

Computer Science

Hst Proposal Id #5339 Hot Stars Subdwarfs

Scientific paper

We propose to test the radiatively driven wind theory for central stars of planetary nebulae (CSPN). The test is interesting because CSPN differ substantially from the luminous and massive Pop.I stars. There is a clear discrepancy between spectroscopic+wind masses versus evolutionary masses of Pop.I OB stars. The result of the CSPN test would help to decide which masses need correction, with obvious impact on stellar atmosphere and stellar evolution theory. A well-tested and confirmed wind theory would become a powerful tool for stellar spectroscopic mass, radius, distance and luminosity determinations throughout the Local Group. In order to make this test with maximum efficiency we have selected a sample of CSPN with temperatures similar to those of Pop.I OB stars and showing a variety of wind strengths. We wish to obtain high S/N ultraviolet spectrograms with HST+FOS. Our list of CSPN necessarily includes faint and reddened objects which can only be observed with HST. FOS spectra in the range from 1150 to 2300 Angstroms, combined with existing high resolution optical data, will provide reliable values of Teff, log g, photospheric abundances and mass loss rates, using sophisticated NLTE "unified" models and NLTE metal line formation calculations including wind effects. This input will be used to predict, from wind models, the P Cygni profiles of UV resonance lines, to be compared with the observed ones.

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