Computer Science
Scientific paper
Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11699r&link_type=abstract
HST Proposal ID #11699. Cycle 17
Computer Science
Scientific paper
We propose UV spectroscopy of the four unique post-AGB stars of spectral type O{He} in order to understand the origin of their peculiar surface abundances. These stars are the only known amongst the hottest post-AGB stars {effective temperatures > 100,000 K} whose atmospheres are composed of almost pure helium. This chemistry markedly differs from that of the hydrogen-deficient post-AGB evolutionary sequence with objects which have carbon dominated atmospheres {PG1159 stars and Wolf-Rayet central stars}. While PG1159 and Wolf-Rayet stars are the result of a late helium-shell flash, this scenario cannot explain the O{He} stars. Instead, they are possibly double-degenerate mergers. We speculate that the four O{He} stars represent evolved RCrB stars, which also have helium-dominated atmospheres. We aim to determine the C, N, O, and Si abundances precisely, in order to proof this evolutionary link.;
No associations
LandOfFree
On the evolutionary status of extremely hot helium stars - are the O{He} stars successors of the R CrB stars? does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with On the evolutionary status of extremely hot helium stars - are the O{He} stars successors of the R CrB stars?, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On the evolutionary status of extremely hot helium stars - are the O{He} stars successors of the R CrB stars? will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1320466