Atomic diffusion and mixing in old stars II. Observations of stars in the globular cluster NGC 6397 with VLT/FLAMES-GIRAFFE

TL;DR

This study confirms atomic diffusion effects in metal-poor stars of globular cluster NGC 6397 by observing surface abundance variations consistent with stellar models including diffusion and turbulent mixing.

Contribution

It provides independent observational evidence for atomic diffusion in globular cluster stars, using homogeneous spectroscopic data and analysis methods.

Findings

Iron abundance is 0.13 dex lower in turn-off stars compared to evolved stars.

Surface abundance trends align with models including diffusion and turbulent mixing.

Magnesium shows similar abundance variation trends, calcium and titanium are more uniform.

Abstract

Evolutionary trends in the surface abundances of heavier elements have recently been identified in the globular cluster NGC 6397 ([Fe/H]=-2), indicating the operation of atomic diffusion in these stars. Such trends constitute important constraints for the extent to which diffusion modifies the internal structure and surface abundances of solar-type, metal-poor stars. We perform an independent check of the reality and size of abundance variations within this metal-poor globular cluster. Observational data covering a large stellar sample, located between the cluster turn-off point and the base of the red giant branch, are homogeneously analysed. The spectroscopic data were obtained with the medium-high resolution spectrograph FLAMES/GIRAFFE on VLT-UT2. We derive independent effective-temperature scales from profile fitting of Balmer lines and by applying colour-temperature calibrations to Str\"omgren uvby and broad-band BVI photometry. An automated spectral analysis code is used together with a grid of MARCS model atmospheres to derive stellar surface abundances of Mg, Ca, Ti, and Fe. We identify systematically higher iron abundances for more evolved stars. The turn-off point stars are found to have 0.13dex lower surface abundances of iron compared to the coolest, most evolved stars in our sample. There is a strong indication of a similar trend in magnesium, whereas calcium and titanium abundances are more homogeneous. Within reasonable error limits, the obtained abundance trends are in agreement with the predictions of stellar structure models including diffusive processes (sedimentation, levitation), if additional turbulent mixing below the outer convection zone is included.