UV Spectroscopy of Wolf-Rayet-Type Central Stars in the Magellanic Clouds

Details UV Spectroscopy of Wolf-Rayet-Type Central Stars in the Magellanic Clouds UV Spectroscopy of Wolf-Rayet-Type Central Stars in the Magellanic Clouds

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7303h&link_type=abstract

HST Proposal ID #7303

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Hst Proposal Id #7303 Hot Stars And Stellar Corpses

Scientific paper

We propose to take low-resolution UV spectra of two WC-type {subtypes WC5-6 and WC7} Central Stars of Planetary Nebulae {CSPN} in the LMC. Three spectral ranges shall be observed with STIS for each star {grisms G140L, G230L, 430L}, with exposure times ranging from 26min to 62min per frame for a S/N ratio of 20-30 in the stellar continuum. Special advantage is taken from the high spatial resolution of HST which allows suppression of the nebular emission through a small slit. Together with ground-based optical spectra which we have already secured we will be able to perform quantitative spectral analyses of the central stars together with consistent nebular analyses. The decisive advantage of studying CSPN in the LMC is the knowledge of the distance. By this we will obtain definite values of the stellar parameters {especially the luminosity}. This will reveal, e.g., whether WC-type CSPN are really more luminous than other CSPN, as has been suggested. A related question is why only CSPN with carbon-rich surface composition develop strong, WR-type winds. The results from the spectroscopic analyses will be used to construct post-AGB evolutionary tracks which, thanks to new physical ingredients {mixing treatment in overshoot layers}, are capable now for the first time to produce WC-type abundance patterns. Metallicity effects on the evolution {LMC vs. Galaxy} will be studied. Consistent modelling of the nebulae will add further information about the evolutionary past of the central stars.

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