The Physical Basis of Luminosity Classification in the Late A, F and early G--type Stars

Details The Physical Basis of Luminosity Classification in the Late A, F and early G--type Stars The Physical Basis of Luminosity Classification in the Late A, F and early G--type Stars

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.4414g&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #44.14; Bulletin of the American Astronomical Society, Vol. 32, p.1474

Astronomy and Astrophysics

Astronomy

Scientific paper

Classification--resolution CCD spectra (1.8Å/2 pixels) of high quality (S/N> 300) have been obtained for nearly 400 A5 -- G5 stars of all luminosity classes (V -- Ib) on the 0.8 meter telescope of Appalachian State University's Dark Sky Observatory. These spectra have been classified carefully on the MK Spectral Classification system. The basic parameters for these stars, T{eff}, log g, [M/H] and ξ t, the microturbulent velocity, have been determined using a multidimensional simplex routine which finds the best fit to the observed spectrum and fluxes (from Strömgren uvby photometry) from a four--dimensional grid of synthetic spectra and fluxes calculated from Kurucz models. Internal errors are approximately +/- 80K in T{eff}, +/- 0.10 in log g, +/- 0.10 in [M/H] and +/- 0.5km/s in ξ t, the microturbulent velocity. The results have been examined for correlations between log g, ξ t and the luminosity class. Using partial correlation analysis, it is found that for most spectral types the microturbulent velocity is as good or better a predictor of the luminosity type as the gravity. The implications of this result for the interpretation of luminosity classification on the MK Spectral Classification system will be discussed.

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