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Stellar evolution calculations with variable abundance ratios were used togauge the effects on temperatures, luminosities, and lifetimes in variousphases. Individual elements C, N, O, Mg, Si, and Fe were included. Most of theeffect relevant to integrated light models is contained in the temperaturevariable, as opposed to the timescale or luminosity. We derive a recipe forincluding abundance-sensitive temperature effects that is applicable toexisting isochrone grids. The resultant enhanced isochrones are incorporatedinto composite stellar population models and compared with galaxy data from theSloan Digital Sky Survey. A severe oxygen-age degeneracy is apparent, 2 - 3 Gyrper 0.1 dex in [O/R], where R represents a heavy element such as Fe. Over therange of early-type galaxy velocity dispersion, the spans of all abundanceratios are reduced but the age range increases, systematically older. AllowingFe-peak elements the freedom to vary accentuates this increase of age span.Overall, these results sharpen the age-mass correlation known as downsizing butdecrease the steepness of abundance ratio gradients. Both of theseobservations, in turn, imply a more robust contribution from gas free mergersin the histories of typical elliptical galaxies.

Individual element sensitivity for stellar evolutionary isochrones