A Helium-Carbon Correlation on the Extreme Horizontal Branch in Centauri
arXiv:1409.4042 · doi:10.1088/0004-637X/795/2/106
Abstract
Taking advantage of a recent FORS2/VLT spectroscopic sample of Extreme Horizontal Branch (EHB) stars in Cen, we isolate 38 spectra well suited for detailed atmospheric studies and determine their fundamental parameters (, log , and log (He)/(H)) using NLTE, metal line-blanketed models. We find that our targets can be divided into three groups: 6 stars are hot ($\buildrel>\over\sim\ $ 45,000 K) H-rich subdwarf O stars, 7 stars are typical H-rich sdB stars ($ \buildrel<\over\sim\ $35,000 K), and the remaining 25 targets at intermediate effective temperatures are He-rich (log (He)/(H)$ \buildrel>\over\sim\ $ 1.0) subdwarfs. Surprisingly and quite interestingly, these He-rich hot subdwarfs in Cen cluster in a narrow temperature range (35,000 K to 40,000 K). We additionally measure the atmospheric carbon abundance and find a most interesting positive correlation between the carbon and helium atmospheric abundances. This correlation certainly bears the signature of diffusion processes - most likely gravitational settling impeded by stellar winds or internal turbulence - but also constrains possible formation scenarios proposed for EHB stars in Cen. For the He-rich objects in particular, the clear link between helium and carbon enhancement points towards a late hot flasher evolutionary history.
arXiv commentAccepted for publication in ApJ (12-09-2014), 17 pages
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