HST/COS Observations of O(He) Stars

Details HST/COS Observations of O(He) Stars HST/COS Observations of O(He) Stars

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1273..203r&link_type=abstract

17TH EUROPEAN WHITE DWARF WORKSHOP. AIP Conference Proceedings, Volume 1273, pp. 203-208 (2010).

Computer Science

Stellar Evolution, White Dwarfs, Spectroscopy, Photometry, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Spectroscopy And Spectrophotometry, Photography And Photometry

Scientific paper

The four known O(He) stars are the only amongst the hottest post-AGB stars (Teff>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 that have carbon-dominated atmospheres (namely PG 1159 stars and Wolf-Rayet type central stars). While PG 1159 and Wolf-Rayet stars are the result of a (very) late helium-shell flash, this scenario cannot explain the O(He) stars. Instead, they are possibly double-degeneratemergers. We speculate that the four O(He) stars represent evolved RCrB stars, which also have helium-dominated atmospheres.
We present UV spectroscopy of the O(He) stars based on recently performed HST/COS observations.

Affiliated with

Also associated with

No associations

Rating

HST/COS Observations of O(He) 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 HST/COS Observations of O(He) Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and HST/COS Observations of O(He) Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1158147