Lithium abundances of halo dwarfs

However, after the success of the Wilkinson Microwave Anisotropy Probe (WMAP) in determining the baryon density, {Omega}_B_h^2^, there was a discrepancy between observationally determined and theoretically determined abundances in the case of ^7^Li. One of the most important uncertain factors in the calculation of the stellar ^7^Li abundance is the effective temperature, Teff.

We use sixteen metal-poor halo dwarfs to calculate new Teff values using the excitation energy method. With this temperature scale we then calculate new Li abundances for this group of stars in an attempt to resolve the ^7^Li discrepancy.