Flash Mixing on the White Dwarf Cooling Curve: Spectroscopic Confirmation in NGC 2808

TL;DR

This study uses HST FUV spectroscopy to confirm that blue-hook stars in NGC 2808 are the result of late He-core flash induced flash mixing, revealing their unique surface compositions and evolutionary origins.

Contribution

It provides spectroscopic evidence supporting the flash mixing scenario for blue-hook stars, linking their properties to late He-core flashes on the white dwarf cooling curve.

Findings

Blue-hook stars are hotter and enriched in He and C compared to normal HB stars.

Spectroscopy confirms flash mixing as the origin of blue-hook stars.

Atmospheric diffusion affects surface abundances of C, Si, and Fe-peak elements.

Abstract

[Abridged] We present new HST FUV spectroscopy of 24 hot evolved stars in NGC2808, a massive globular cluster with a large population of "blue-hook" (BHk) stars. The BHk stars are found in UV color-magnitude diagrams of the most massive globular clusters, where they fall at luminosities immediately below the hot end of the horizontal branch (HB), in a region of the HR diagram unexplained by canonical stellar evolution theory. Using new evolutionary and atmospheric models, we have shown that these subluminous HB stars are very likely the progeny of stars that undergo extensive internal mixing during a late He-core flash on the white dwarf cooling curve. This flash mixing leads to hotter temperatures and an enormous enhancement of the surface He and C; these hotter temperatures, together with the decrease in H opacity shortward of the Lyman limit, make the BHk stars brighter in the EUV while appearing subluminous in the UV and optical. Our FUV spectroscopy demonstrates that, relative to normal HB stars at the same color, the BHk stars of NGC2808 are hotter and greatly enhanced in He and C, thus providing unambiguous evidence of flash mixing. Although the C abundance in the BHk stars is orders of magnitude larger than that in the normal HB stars, the C abundance in both the BHk and normal HB stars appears to be affected by gravitational settling. The variations seen in Si and the Fe-peak elements also indicate that atmospheric diffusion is at play in our sample, with all of our hot subdwarfs at 25,000 to 50,000 K exhibiting large enhancements of the Fe-peak elements. The hottest subdwarfs in our BHk sample may be pulsators, given that they fall in the temperature range of newly-discovered pulsating subdwarfs in omega Cen. In addition to the normal hot HB and BHk stars, we obtain spectra of 5 blue HB stars, a post-HB star, and 3 unclassified stars with unusually blue UV colors.