2003/11/10 by S. Moehler, A. V. Sweigart, W. B. Landsman +3 · 2 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Blue straggler #Carbon star #Globular cluster #Horizontal branch #Physics #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20034505
published as Astron.Astrophys. 415 (2004) 313-323 · 11 pages, 9 figures, LaTeX, uses aa.cls (included), accepted for publication in Astronomy and Astrophysics
arxiv created 2003/11/10 · openalex publication_date 2004/02/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Recent UV observations of the globular cluster NGC 2808 (Brown et al. [CITE]) show a significant population of hot stars fainter than the zero-age horizontal branch (“blue hook” stars), which cannot be explained by canonical stellar evolution. Their results suggest that stars which experience unusually large mass loss on the red giant branch and which subsequently undergo the helium core flash while descending the white dwarf cooling curve could populate this region. Theory predicts that these “late hot flashers” should show higher temperatures than the hottest canonical horizontal branch stars and should have helium- and carbon-rich atmospheres. As a test of this late hot flasher scenario, we have obtained and analysed medium resolution spectra of a sample of blue hook stars in NGC 2808 to derive their atmospheric parameters. Using the same procedures, we have also re-analyzed our earlier spectra of the blue hook stars in ω Cen (Moehler et al. [CITE]) for comparison with the present results for NGC 2808. The blue hook stars in these two clusters are both hotter ( K) and more helium-rich than canonical extreme horizontal branch stars in agreement with the late hot flasher scenario. Moreover, we find indications for carbon enhancement in the three most helium-enriched stars in NGC 2808. However, the blue hook stars still show some hydrogen in their atmospheres, perhaps indicating that some residual hydrogen survives a late hot flash and then later diffuses to the surface during the horizontal branch phase. We note that the presence of blue hook stars apparently depends mostly on the total mass of the globular cluster and not so much on its horizontal branch morphology.