Spectroscopy of Main Sequence Stars in Globular Clusters

Simple item page
dc.creatorCannon, Russell
dc.creatorDa Costa, Gary
dc.creatorNorris, John
dc.creatorStanford, Laura
dc.creatorCroke, Barry
dc.date2002-10-15
dc.date.accessioned2026-07-07T02:05:43Z
dc.date.available2026-07-07T02:05:43Z
dc.descriptionAlthough globular clusters are generally chemically homogeneous, substantial abundance variations are sometimes seen even among unevolved main sequence stars, especially for the CNO group of elements. Multi-object intermediate-dispersion spectroscopic systems are now being used to determine the patterns of abundance variations for large samples of stars, while high dispersion spectrographs on 8m-class telescopes are providing good spectra of individual faint stars. In some circumstances the spectra of many similar stars can be combined to yield extremely high S/N spectra. The sample of clusters which has been studied remains small, but it seems that many of the more metal-rich clusters must have experienced some sort of self-enrichment, either in a proto-cluster stage, or through successive episodes of star formation or some other processes early in their lives. The metal-poor clusters provide equally clear evidence for internal mixing and dredge-up of processed material within evolving red giant stars.
dc.description9 pages, 3 eps figures, to appear in `New Horizons in Globular Cluster Astronomy', Padova, June 2002, ASP conf. series
dc.identifierhttps://arxiv.org/abs/astro-ph/0210324
dc.identifierhttp://arxiv.org/abs/astro-ph/0210324
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5184
dc.subjectAstrophysics
dc.titleSpectroscopy of Main Sequence Stars in Globular Clusters
dc.typetext

Files

Collections

arXiv