Uv Spectroscopy of Two Ultra-Hot White Dwarf Candidates

Details Uv Spectroscopy of Two Ultra-Hot White Dwarf Candidates Uv Spectroscopy of Two Ultra-Hot White Dwarf Candidates

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6090w&link_type=abstract

HST Proposal ID #6090

Computer Science

Hst Proposal Id #6090 Hot Stars

Scientific paper

We propose GHRS UV spectroscopy of two outstanding stars which define a completely new spectroscopic class. The optical spectra are dominated by ultra-high ionization absorption ( lines of carbon and oxygen (CVI, OVII, OVIII). In comparison, the very hot (T(eff)>100 000 K) PG 1159 stars exhibit lines from CIV and OVI. First exploratory non- LTE model calculations indicate that the effective temperature of these objects must exceed half a million degrees temperatures by far exceed those of the hottest stars known. The surface gravities are high (log g>8), hence these object are probably compact post-AGB stars which are just about to enter the white dwarf cooling sequence. Comparison with evolutionary tracks suggests masses just below the Chandrasekhar limit. The proposed HST observations are needed to verify the nature of these stars by detailed spectrum synthesis in order to precisely determine the stellar parameters.

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