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March 2009 Statistical analysis of stellar evolution
David A. van Dyk, Steven DeGennaro, Nathan Stein, William H. Jefferys, Ted von Hippel
Ann. Appl. Stat. 3(1): 117-143 (March 2009). DOI: 10.1214/08-AOAS219

Abstract

Color-Magnitude Diagrams (CMDs) are plots that compare the magnitudes (luminosities) of stars in different wavelengths of light (colors). High nonlinear 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 can be described with mathematical models and explored using complex computer models. These calculations are designed 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 a component of a complex likelihood function in a Bayesian analysis that requires sophisticated computing, corrects for contamination of the data by field stars, accounts for complications caused by unresolved binary-star systems, and aims to compare competing physics-based computer models of stellar evolution.

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David A. van Dyk. Steven DeGennaro. Nathan Stein. William H. Jefferys. Ted von Hippel. "Statistical analysis of stellar evolution." Ann. Appl. Stat. 3 (1) 117 - 143, March 2009. https://doi.org/10.1214/08-AOAS219

Information

Published: March 2009
First available in Project Euclid: 16 April 2009

zbMATH: 1160.62098
MathSciNet: MR2668702
Digital Object Identifier: 10.1214/08-AOAS219

Keywords: Astronomy , Color-Magnitude Diagram , contaminated data , dynamic MCMC , informative prior distributions , Markov chain Monte Carlo , Mixture models

Rights: Copyright © 2009 Institute of Mathematical Statistics

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Vol.3 • No. 1 • March 2009
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