Color Magnitude Diagrams (CMDs) are plots that compare stellar
absolute magnitudes in different colors. High non-linear correlations
among the mass, color and surface temperature of newly formed stars
induce a long narrow curved point cloud in a CMD known as the main
sequence. Aging stars form new CMD groups of red giants and white
dwarfs. The physical processes that govern this evolution are studied
with complex computer models used to predict the plotted magnitudes as
a function of parameters of scientific interest such as stellar age,
mass and metallicity. Here, we describe how we use the computer models
as complex likelihood functions in a Bayesian analysis that requires
sophisticated computing, corrects for contamination of field stars in
the data, accounts for complications caused by binary stars, and aims
to compare competing physics-based computer models of stellar
evolution.
Joint work with: Steven DeGennaro, Ted von Hippel, William Jeffery,
Nathan Stein, Elizabeth Jeffery
Meet the speaker in Room 212 Cockins Hall at 4:30
p.m. Refreshments will be served.