B Stars and the abundance gradient of the galactic disk

Details B Stars and the abundance gradient of the galactic disk B Stars and the abundance gradient of the galactic disk

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998egdg.conf..125g&link_type=abstract

"Dynamics of Galaxies and Galactic Nuclei, An International Workshop of the SFB 328 "Evolution of Galaxies" held at the ITA Nove

Physics

Scientific paper

Recent determinations of metallicity gradients in normal and barred spiral galaxies are reviewed and confronted with abundance measurements in the disk of our Milky Way. Discordant results are reported for the youngest stellar populations, H II regions and B stars. The relevance of the central bar structure of the Galaxy for the chemodynamical evolution of the Galactic disk is stressed. A novel study of B stars between 5 and 13 kpc galactocentric distance using non-LTE techniques reveals a steep abundance gradient of about -0.07 dex/kpc for CNO elements, in accordance to normal spiral galaxies of similar Hubble type. It is argued that the central bar structure of the Milky Way is still too young (about 800 Myr) to exert a notable flattening effect on the chemical abundance gradient of the Galactic disk.

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