In Christ ... a future with hope

Historical series, 18. Sermon preached at the opening service of the Saskatchewan Synod Convention, Swift Current, Saskatchewan, 4 Jl 2002. Jer 29:11-14; Rom 8:18-27; Jn 17:1-6, 17-26

We would see Jesus

Historical series, 10. Jn 12:20-33. Preached during Lent, 1997, Hodgeville Lutheran parish

Nitrogen abundances in giant stars of the globular cluster NGC 6752

We present N abundances for 21 bright giants in the globular cluster NGC 6752 based on high-resolution UVES spectra of the 3360A NH lines. We confirm that the Stromgren c1 index traces the N abundance and find that the star-to-star N abundance variation is 1.95 dex, at the sample's luminosity. We find statistically significant correlations, but small amplitude variations, between the abundances of N and alpha-, Fe-peak, and s-process elements. Analyses using model atmospheres with appropriate N, O, Na, and Al abundances would strengthen, rather than mute, these correlations. If the small variations of heavy elements are real, then the synthesis of the N anomalies must take place in stars which also synthesize alpha-, Fe-peak, and s-process elements. These correlations offer support for contributions from both AGB and massive stars to the globular cluster abundance anomalies.Comment: Accepted for publication in Ap

Observational signatures of lithium depletion in the metal-poor globular cluster NGC6397

The "stellar" solution to the cosmological lithium problem proposes that surface depletion of lithium in low-mass, metal-poor stars can reconcile the lower abundances found for Galactic halo stars with the primordial prediction. Globular clusters are ideal environments for studies of the surface evolution of lithium, with large number statistics possible to obtain for main sequence stars as well as giants. We discuss the Li abundances measured for >450 stars in the globular cluster NGC6397, focusing on the evidence for lithium depletion and especially highlighting how the inferred abundances and interpretations are affected by early cluster self-enrichment and systematic uncertainties in the effective temperature determination.Comment: 6 pages, 2 figures, conference proceedings for IAU symposium 26