Physics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6454w&link_type=abstract
HST Proposal ID #6454
Physics
Hst Proposal Id #6454 Hot Stars
Scientific paper
HS2115+1148 belongs to a small group of peculiar white dwarfsdetected within the framework of follow--up spectroscopy offaint blue stars selected from the Hamburg Schmidt survey. Thespectra of these stars exhibit shallow metal absorption (lines from ultrahighly excited ionization stages (CV,CVI / NVI, NVII / OVII, OVIII / NeIX,NeX) with ionization energies ranging from 392eV to 1362eV,far too high for a photospheric origin even for the hotteststars known. Due to the blue shift and asymmetric shape ofthese lines we proposed that they are formed in a stellarwind. The underlying photospheric spectra resemble that of hothelium rich (DO) white dwarfs in five cases. Recently wedetected this phenomenon also in a single hydrogen rich whitedwarf with traces of helium (HS2115+1148), making this star uniqueamong the peculiar white dwarfs. The number ratio of thesestars to ordinary hot white dwarfs suggests that thisphenomenon might be common at the beginning of the white dwarfcooling sequence. Depending on the duration and the mass--lossrate, cooling time scales and luminosity functions of whitedwarfs could be affected with serious consequences for ourunderstanding of the late stages of low--mass star evolution.The proposed HST observation is needed to verify the nature ofthis star by detailed spectrum synthesis in order to preciselydetermine stellar and wind parameters.
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