Chromospheres and Light Element Abundances

Details Chromospheres and Light Element Abundances Chromospheres and Light Element Abundances

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1894s&link_type=abstract

IUE Proposal ID #LEGTS

Physics

Scientific paper

Observations show a decline in surface lithium content of 1 M(sun) stars during their main sequence lifetimes. This is explained by models of stellar evolution as the result of convective mixing with the interior: surface material is mixed into deeper layers, T > 2 million K, where Li is destroyed by nuclear reactions. The models predict little depletion for stars more massive than the Sun, that is, for the early- and mid-F stars. Moreover, the abundance of beryllium should remain at its primordial level for all stars hotter than K2. Some nearby F dwarfs are known to have very low abundances of Li and Be, with depletions of more than an order of magnitude. These abundance peculiarities have been attributed to the action of turbulent diffusion (rather than gravitational settling). I am proposing here to look for evidence of chromospheric effects in the UV spectra of stars with different Li and Be abundances. A correlation between variations in chromospheric (and transition region) emission and light element depletions would suggest a common origin for both, arising out of differences in internal structure, differential rotation, or turbulence spectrum from one star to the next.

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